101 Ways to Leave a Gameshow, Format
The show's production company, Endemol, describes the show as "the play-along fun of a glitzy, Saturday night quiz with the full-on adrenaline rush of an extreme stunt show." Each episode features eight contestants, with a mix of sexes, ages and backgrounds, competing to be the winner of the £10,000 prize in the UK version ($50,000 in the US version). Contestants are reduced one by one in the first four rounds, attempting to guess the correct answers to a selection of multiple-choice questions.


101 Ways to Leave a Gameshow, Format
The contestant who chooses the wrong answer will leave the show in spectacular fashion, in one of the 101 Ways To Leave A Gameshow. At any time during the first four rounds, a buzzer could sound, which announces the start of the Emergency Exit round. In this round, contestants are asked a series of questions at random, with the first contestant to give a wrong answer being eliminated. The Emergency Exit round is not used in the US and Italian versions. In the final round, only three contestants remain (four contestants in the US version), who have to answer one last question in an attempt to win the jackpot prize.


101 Ways to Leave a Gameshow, Production
The show was created jointly by Endemol USA and Endemol UK. It was first produced by the UK division of Endemol for the BBC. Like its Saturday night stablemate, Total Wipeout, the show is filmed entirely at Endemol's filming facility in Benavídez, approximately 40 km Northwest of Buenos Aires, Argentina. Generally, most of the programme is recorded outside, however, studio segments are recorded in a monolithic purpose-built 100 feet (30 m) tall tower, located above the 'exits'. Studio segments are generally filmed on three different levels, with the '101 Ways To Leave' segments recorded on the Tower's exterior. Some exits from the show are recorded on a disused airfield runway located adjacent to the tower. Most of the exits culminate in the contestant ending up in a large pool of water directly in front of the tower.


101 Ways to Leave a Gameshow, Production
The United States version was filmed at Agua Dulce, California, which is a popular filming location in Northern Los Angeles County. The site has an active general aviation airfield that was closed down during filming.


101 Ways to Leave a Gameshow, Gameplay
In each of the first four rounds, Nemone reveals the exit method that will be used to dismiss the losing contestant, numbered between 1 and 101. Jones then asks a question and reads as many answers as there are contestants still in the game; all but one of them are correct. After each contestant secretly chooses one answer, all reveal their selections. If any answer is chosen by multiple contestants, a toss-up question on the buzzer is used to determine which one of them gets to keep it.


101 Ways to Leave a Gameshow, Gameplay
After all ties have been resolved, the remaining contestants select again from the unchosen answers. Further toss-ups are played as needed until all contestants have chosen different answers, at which point they are prepared for the exit. Jones reveals one correct answer at a time until only two contestants are left in jeopardy, then announces the wrong answer. The contestant who chose it is immediately eliminated from the game.


101 Ways to Leave a Gameshow, Gameplay
Once per episode, a buzzer sounds off between rounds to indicate that an "Emergency Exit" round must be played. Jones asks a question to one contestant at a time in random order, and the first to miss a question is eliminated.


101 Ways to Leave a Gameshow, Gameplay
Once three contestants remain, the fifth and final round begins, following the same format as the previous four except that the question has only one right answer. The contestant who chooses it wins £10,000, while the other two are dismissed by exit #101, "The Trap Door" - being dropped through trapdoors on which they are standing to fall into the water below.


101 Ways to Leave a Gameshow, Exits used on the show
A total of 34 different exits were used over the course of the series, including #101 and the Emergency Exit that were common to all episodes.


101 Weddings
101 Weddings is a 2012 Indian Malayalam-language romantic comedy film directed by Shafi and starring Kunchacko Boban, Jayasurya, Biju Menon, Samvrutha Sunil, and Bhama in the lead roles. The film is written by Kalavoor Ravikumar based on a story by the director. The film is produced by Shafi's brother Rafi Mecartin, Hasainar, and Shaleer, with audiography by M. R. Rajakrishnan under the banner of Film Folks and features music composed by Deepak Dev.


101 Weddings, Plot
The movie opens up in the childhood pranks of  Krishnankutty (Kunchacko Boban), the son of famous Gandhian Munshi Shankara Pillai (Vijayaraghavan) who is repeatedly beaten up by Antappan (Biju Menon), his big schoolmate. Antappan is taking vengeance for the Gandhian deeds of Munshi who has closed down the toddy shop owned by Antappan's father. And when a chance comes up, Krishankutty retaliates by placing the costly golden church arrow in the bag of Antappan, which makes him a thief and lands him in a juvenile home for young criminals.


101 Weddings, Plot
As they grow up, Krishnankutty becomes a TV producer in the name Krish but is ready to play fowl games and make money by little frauds. But his father Munshi who has now become a much proclaimed Gandhian finds an able girl in Abhirami (Samvrutha Sunil), the only daughter of Abkari contractor Bhasi, to reform his son.


101 Weddings, Plot
Abhirami and Co who is running the Kasturba Society are on the plans to hold a mass wedding of 101 couples in which she will also find a suitable groom and marry. The mass wedding is arranged in such a way that the interested persons are needed to stay in the picturesque resort-like village for two weeks to get familiar with their probable future partners.


101 Weddings, Plot
Krish is but reluctant to marry another girl with Gandhian principles and brings in Jyothish Kumar a.k.a. Jyothi (Jayasurya), a dance teacher with all female mannerisms, gets him registered as Krishanankutty to make Abhirami move away from this alliance. Antappan and his gang who has now grown up as famous quotation gangs also register for the marriage in the plans to grab the money and 5 gold coins that are given to each couple. And as the day to the marriage comes up, more and more persons enroll into the mass wedding with their own interesting plans.


101 Weddings, Production
Shooting started on 15 July 2012 at Kochi, the other locations are Thodupuzha, Ottappalam and Hyderabad.


101 Weddings, Soundtrack
The soundtrack was composed by Deepak Dev, with lyrics penned by Rafeeq Ahmed. The album consists of four songs. The audio rights of the film were acquired by Manorama Music. The album was launched on 28 October 2012 at Kochi.


101 Zen Stories
101 Zen Stories is a 1919 compilation of Zen koans including 19th and early 20th century anecdotes compiled by Nyogen Senzaki, and a translation of Shasekishū, written in the 13th century by Japanese Zen master Mujū (無住) (literally, "non-dweller"). The book was reprinted by Paul Reps as part of Zen Flesh, Zen Bones. Well-known koans in the collection include A Cup of Tea (1), The Sound of One Hand (21), No Water, No Moon (29), and Everything is Best (31).


101 series
The 101 series (101系, 101-kei) was a DC electric multiple unit (EMU) commuter train type introduced in 1957 by Japanese National Railways (JNR), and formerly operated by East Japan Railway Company (JR East) and West Japan Railway Company (JR-West). The last remaining trains were withdrawn in November 2003.


101 series, History
The prototype 101 series set was delivered in June 1957, as a 10-car (4+6-car) set classified as 90 series with all cars motored. Cab cars were numbered MoHa 90500 to 90503, and the intermediate cars were numbered MoHa 90000 to 90005. Production sets were delivered from March 1958, differing visually from the prototype in having exposed rain gutters along the top of each car. The 90 series was reclassified as 101 series from 1959, with the prototype set cars numbered in the 900 subseries. The prototype set was modified in 1962 to bring it up to production set standards.


101 series, Lines used, Osaka Area
JNR 101 series EMU approaching Kinshicho Station at Chuo-Sobu Line, August 1978


101 series, Lines used, Osaka Area
A JNR 101 series EMU leaving Katamachi Station on the Katamachi Line, 1985


101 series, Lines used, Osaka Area
JR East 3-car Tsurumi Line set at Musashi-Shiraishi Station, circa December 1990


101 series, Lines used, Osaka Area
A JR East 2-car Nambu Branchline set at Shitte Station in July 2002


101 series, Lines used, Osaka Area
Last standing 101 series with "Sayonara" head mark on its last run on Nambu Branch Line Services on December 2003


101 series, Private operators
A number of former 101 series trains were sold to the private railway operator Chichibu Railway in Saitama Prefecture in 1986, where they operated as 3-car 1000 series sets until March 2014.


101 series, Private operators
Chichibu Railway 1000 series sets in "revival" JNR liveries in December 2007


101 series, Preserved examples
KuMoHa 101-902 at Tokyo General Rolling Stock Center, August 2005


101 series, Preserved examples
Mock-up of a 101 series at the Kyoto Railway Museum, April 2017


101-in-1 Explosive Megamix
101-in-1 Explosive Megamix is a video game developed by Nordcurrent and published by Atlus for the Nintendo DS. It was first released in Europe on November 28, 2008 and features 10 hours' worth of minigames. A version for the WiiWare service was released on September 22, 2011 in Europe and on October 13, 2011 in North America.


101-in-1 Explosive Megamix
The Nintendo DS version received mostly mixed reviews. By contrast, the WiiWare version received overwhelmingly negative reviews, with most criticism directed towards the repetitive minigames and the controls.


101-in-1 Explosive Megamix, Gameplay
Players can use the stylus and touch screen to test their reflexes in action minigames like racing and skydiving, take on sporting events such as basketball, curling, and archery, strategize with tank and space combat games, or play match three, Sudoku, and jigsaw puzzles. Gamers who set high scores earn gold coins that can be used to unlock other activities, and those looking for multiplayer action take on friends in multi-card wireless play.


101-in-1 Explosive Megamix, Development
On February 9, 2009, Atlus U.S.A., Inc. announced that it had secured the North American publishing rights from Nordcurrent for 101-in-1 Explosive Megamix for Nintendo DS. Players could challenge a friend to multiplayer competition through local wireless play. It was scheduled for release on April 21, 2009 for a price of US$19.99.


101-in-1 Explosive Megamix, Reception
The Nintendo DS version of 101-in-1 Explosive Megamix received mixed reviews. Nintendo World Report commented "101-in-1 Explosive Megamix is the definitive bad budget title. Some of the mini-games are remotely fun, but others feel like a chore. With so many poor and forgettable games on the compilation, it's hard to recommend this one". Eurogamer stated "There is so little replay potential here, so little urge to top high scores or perfect shoddy make-do attempts, that completing each task feels more of a relief than an achievement". Game Revolution commented "You're better off putting on a blindfold, walking into a rack of DS titles, and picking the game that your face lands on".


101-in-1 Explosive Megamix, Reception
The WiiWare version, however, received extremely negative reviews. IGN commented "[...] keep your cash held back from this 'value' option. It's a waste of money no matter how the math works out". IGN also criticized the game being a direct port from the DS and the iPhone. Official Nintendo Magazine UK noted "You'll find it tough to unlock all 101 games. Not that you'd want to bother because they're so abysmal, not even of the standard of your average Flash game". Review aggregator Metacritic gave the game 16/100 based on 5 reviews, and is the lowest-rated Wii game on the website. Game Revolution gave the game a "D-". GamesRadar+ gave the game a 4/10.


101-in-1 Sports Party Megamix
101-in-1 Sports Party Megamix is a video game developed by Nordcurrent and published by Atlus for the Wii. It was first released in Europe on November 19, 2010 and in North America on January 13, 2011.


101-in-1 Sports Party Megamix, Gameplay
Players move the Wii Remote in games such as bowling, motorcross, and racing. Two to four players can compete against each other in a sack race, tennis, and skateboarding. Gamers who set high scores can unlock other games to play.


101-in-1 Sports Party Megamix, Reception
Upon release, Sports Party Megamix earned mostly negative reviews. Metacritic gave the game a 41/100 based on 7 reviews. The game was also criticized for sloppy graphics, and unresponsive controls.


101.1 FM
The following radio stations broadcast on FM frequency 101.1 MHz:


101.3 FM
The following radio stations broadcast on FM frequency 101.3 MHz:


101.4 FM
The following radio stations broadcast on FM frequency 101.4 MHz:


101.5 FM
The following radio stations broadcast on FM frequency 101.5 MHz:


101.6 FM
This is a list of radio stations that broadcast on FM frequency 101.6 MHz:


101.7 FM
The following radio stations broadcast on FM frequency 101.7 MHz:


101.7 WSFM
101.7 WSFM (call sign: 2UUS) is a radio station broadcasting in Sydney, Australia. Its main content is commercial music, in particular classic hits from 1960 to about 2003, but with a stronger focus from 1970 to 1999. The station is part of the Pure Gold Network (which itself is a part of ARN).


101.7 WSFM
WS FM's main frequency is 101.7 MHz on the FM band, with two repeaters in the outer suburbs of Sydney: 88.3 MHz in the Macarthur region, and 99.1 MHz centred in the Richmond/Hawkesbury region. It previously transmitted on 1224 kHz on the AM band; this frequency is now used by print-handicapped radio station 2RPH.


101.7 WSFM, Music
WS FM's former catchlines were Sydney's Classic Hits.... Good Times and Great Classic Hits.....Real music, real variety & Better Music and More of It. WSFM generally plays Pure gold classic hits from the last four decades, as well as current hits.


101.7 WSFM, History
Liverpool Broadcasting and Transmitting Co Pty Ltd was granted an AM radio license in the late 1970s, specifically to serve the Western Suburbs of Sydney. 2WS began broadcasting at 12:24AM on 23 November 1978, the same day all Australian AM radio stations switched from 10 kHz to 9 kHz frequencies from temporary studios in a relocated cottage at 2 Leabons Lane, Seven Hills with a 5 kW transmitter located at nearby Prospect.


101.7 WSFM, History
The studios subsequently moved, in October 1979, into a purpose built complex behind the old cottage in Leabons Lane. The original building was demolished, with the material donated to charity.


101.7 WSFM, History
In the early 1990s the station was granted an FM licence covering the full Sydney metropolitan area. Its new transmitter site was located at Artarmon, in northern Sydney. The official callsign was changed to 2UUS (using a literal 'double-U' to compensate for the extra letter required), although the station still identified as 2WS until 2001, when they changed their on-air name to WSFM.


101.7 WSFM, History
2WS, 1224 on the A.M. band converted to the FM band and began broadcasting as 2WS-FM on 101.7 MHz in 1 June 1993 at 8a.m..


101.7 WSFM, History
WSFM now broadcasts from studios at North Ryde. The building also houses facilities for KIIS 106.5 and The Edge 96.1, both also owned by  ARN.


101.7 WSFM, History
The previous studios in Seven Hills are now serviced by Christian/Adult Contemporary radio station, Hope 103.2.


101.9 FM
The following radio stations broadcast on FM frequency 101.9 MHz:


101.9 Jay FM Jos
JayFM Jos is a Nigerian privately owned commercial radio station located at No. 14 Akila Machunga Road, Jos. Plateau State. The station features a mix of diverse music genres and talk shows with special focus on local and global news, current affairs, and sports. The radio station airs and streams for 24 hours.


101.9 Jay FM Jos
The Jos-based radio station started broadcasting in September 2016. The JayFM team is led by the Managing Director and Chief Executive Officer, Clinton Garuba.


101.9 Jay FM Jos
.On the 1st of March 2019, the radio station was shut from operation by the Nigeria Broadcasting Commission (NBC). The station was said to have broadcast hate speech. That led to the station taking NBC to court and an out of court settlement was ensued by the two parties which led to the reopening of the station on 15 May 2019.


101.9 Jay FM Jos, Listenership Projections
Their terrestrial listenership projections and evaluation so far reaches up to 2.0 million people daily in Plateau state and the immediate broadcast environs; FCT Abuja, Bauchi, Gombe, Kaduna, and Nassarawa states with 5000 listeners joining via the live stream daily


1010
Year 1010 (MX) was a common year starting on Sunday (link will display the full calendar) of the Julian calendar.


1010 AM
The following radio stations broadcast on AM frequency 1010 kHz: 1010 AM is a Canadian clear-channel frequency. CFRB Toronto and CBR Calgary are both Class A, 50,000 watt stations.


1010 Brickell
1010 Brickell is a residential high-rise in the Brickell neighborhood of Miami, Florida. It is located behind an office building at 1000 Brickell Avenue, adjacent to the Tenth Street Metromover station. Construction began in 2014 and required the demolition of an existing parking garage. The building is expected to rise about 548 feet (167 m) with 50 floors and nearly 400 units, with ceiling heights of 9.28 feet (2.83 m). The 5,600 cubic yards (4,300 m3) mat pour was completed on April 4, 2015.


1010 Brickell
1010 Brickell construction in May 2016 from the east on 10th Street


1010 Common
1010 Common (formerly the Bank of New Orleans Building), located at 1010 Common Street in the Central Business District of New Orleans, Louisiana, is a 31-story skyscraper. The building, designed by Skidmore, Owings & Merrill and completed in 1970, is an example of the international style typical of the time. It is located adjacent to the 14-story Latter Center Garage & Annex.


1010 Common
It was listed on the National Register of Historic Places in 2016.


1010 Marlene
1010 Marlene (prov. designation: A923 VH or 1923 PF) is a carbonaceous background asteroid from the outer regions of the asteroid belt, approximately 47 kilometers in diameter. It was discovered on 12 November 1923, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after German actress and singer Marlene Dietrich.


1010 Marlene, Classification and orbit
Marlene is not a member of any known asteroid family. It orbits the Sun in the outer main-belt at a distance of 2.6–3.2 AU once every 5.02 years (1,832 days). Its orbit has an eccentricity of 0.10 and an inclination of 4° with respect to the ecliptic.


1010 Marlene, Classification and orbit
The asteroid was first identified as A903 UD at the discovering observatory in October 1903. The body's observation arc begins at Heidelberg in January 1924, more than two months after its official discovery observation.


1010 Marlene, Naming
This minor planet was named after German-born Marlene Dietrich (1901–1992), actor, singer and high-profile entertainer during World War II. The name was proposed by astronomer Gustav Stracke. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 97).


1010 Marlene, Physical characteristics, Rotation period
Photometric measurements of Marlene – made by American astronomer Brian Warner at the Palmer Divide Observatory (716), Colorado, in February 2005 – showed a lightcurve with a longer-than average rotation period of 31.06±0.02 hours and a brightness variation of 0.32±0.02 in magnitude (U=2+). Most asteroids have periods shorter than 20 hours.


1010 Marlene, Physical characteristics, Rotation period
Another lightcurve, obtained by French amateur astronomer René Roy, gave a period of 29.0 hours and an amplitude of 0.17 magnitude (U=2).


1010 Marlene, Physical characteristics, Spin axis
In 2013 and 2016, an international study modeled a lightcurve with a concurring period of 31.0651 and 31.066 hours, respectively. The study also determined two spin axis of (299.0°, 42.0°) and (106.0°, 47.0°) in ecliptic coordinates (λ, β) (U=n.a. ).


1010 Marlene, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Marlene measures between 43.47 and 51.085 kilometers in diameter and its surface has an albedo between 0.03 and 0.0647.


1010 Marlene, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives an albedo of 0.054 and a diameter of 43.38 kilometers based on an absolute magnitude of 10.6.


1010 Mass
1010 Mass is a high-rise building in Washington, D.C. The building rises 15 floors and 157 feet (48 m) in height. The building was designed by architectural firm Esocoff & Associates and was completed in 2007, making it one of the most recently constructed high-rises in the city. As of July 2008, the structure stands as the 24th-tallest building in the city, tied in rank with 1620 L Street, 1333 H Street, 1000 Connecticut Avenue, the Republic Building, 1111 19th Street, the Army and Navy Club Building and the Watergate Hotel and Office Building. 1010 Mass is an example of postmodern architecture, with a facade composed of brick and cast stone. The structure is composed almost entirely of residential units, with a total of 163 condominiums; the lowest floor is used for retail. The entire structure also rises above a 169-unit underground parking garage.


1010 Midtown
1010 Midtown is a 35-story, 124 m (407 ft) skyscraper in Atlanta, Georgia with 425 condominiums atop 38,000 sq ft (3,500 m2) of retail and dining space. The structure is part of the 12th & Midtown development, situated on approximately 2 acres (0.81 ha) on the block between 11th and 12th streets in Midtown Atlanta, the front of which follows the curve of Peachtree Street. The 1010 Midtown building also features a park-in-the-sky, which will be one of the largest environmentally green rooftops in the city.


1010 Midtown
Daniel Corporation, Selig Enterprises, the Canyon-Johnson Urban Fund (CJUF), and MetLife combined forces to make 1010 Midtown, a key piece in the Midtown Mile, a reality. The building was designed by the architecture firm Rule Joy Trammell + Rubio and built by Brasfield & Gorrie. Construction of this first phase of the 12th & Midtown development began in August 2006 and was completed in early 2009.


1010 Midtown
At the base of 1010 Midtown sit several new restaurants and bars, including Ra Sushi, Ribalta, and Ri Ra Irish Pub. It also houses a Bank of America branch and additional retail space fronting Peachtree Street.


1010 Midtown, Incident
On March 9, 2012, a man jumped to his death from the 35th floor of the building.


1010 Midtown, Midtown Mile
The Midtown Mile, a block that is expected to cover some 3,000,000 sq ft (280,000 m2) when completed, will run along Peachtree Street and will be the newest location for high-end retail and dining activities in Atlanta. It will host a variety of flagship storefronts, restaurants, hotels and high-rises, of which, 1010 Midtown will be the first to be fully completed.


1010s
The 1010s was a decade of the Julian Calendar which began on January 1, 1010, and ended on December 31, 1019.


1010s BC
The 1010s BC is a decade which lasted from 1019 BC to 1010 BC.


1010s BC, Significant people
This BC year article is a stub. You can help Wikipedia by .


1010s in England, Incumbents
Monarch – Æthelred the Unready (to December 1013), Sweyn Forkbeard (to 3 February 1014), Æthelred the Unready (to 23 April 1016), Edmund Ironside (to 30 November 1016), Canute


1010s in art
The decade of the 1010s involved some significant events in art.


1010s in poetry
Nationality words link to articles with information on the nation's poetry or literature (for instance, Irish or France).


1010s in poetry, Births
Death years link to the corresponding "[year] in poetry" article. There are conflicting or unreliable sources for the birth years of many people born in this period; where sources conflict, the poet is listed again and the conflict is noted:


1010s in poetry, Deaths
Birth years link to the corresponding "[year] in poetry" article:1012:


1011
Year 1011 (MXI) was a common year starting on Monday of the Julian Calendar.


1011 Laodamia
Laodamia (minor planet designation: 1011 Laodamia), provisional designation 1924 PK, is a stony asteroid and sizable Mars-crosser near the innermost regions of the asteroid belt, approximately 7.5 kilometers in diameter. It was discovered on 5 January 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after Laodamia from Greek mythology.


1011 Laodamia, Orbit and classification
Laodamia is a Mars-crossing asteroid, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.666 AU. It orbits the Sun at a distance of 1.6–3.2 AU once every 3 years and 8 months (1,352 days). Its orbit has an eccentricity of 0.35 and an inclination of 5° with respect to the ecliptic.


1011 Laodamia, Orbit and classification
The body's observation arc begins 15 years after its official discovery observation with its identification 1939 FG at Turku Observatory in March 1939. On 5 September 2083, it will pass 0.06186 AU (9,254,000 km; 5,750,000 mi) from Mars.


1011 Laodamia, Physical characteristics
In the Tholen classification, Laodamia is a stony S-type asteroid, while in the SMASS taxonomy, it is a transitional type between the stony S-type and rare R-type asteroids.


1011 Laodamia, Physical characteristics, Rotation period and spin axis
In March 2002, a rotational lightcurve of Laodamia was obtained from photometric observations by French amateur astronomers Laurent Bernasconi and Silvano Casulli. Lightcurve analysis gave a well-defined rotation period of 5.17247 hours with a brightness amplitude of 0.44 magnitude (U=3). Two other lightcurve gave a concurring period of 5.17 and 5.175 hours, respectively (U=2+/3).


1011 Laodamia, Physical characteristics, Rotation period and spin axis
Photometry taken at the Rozhen Observatory over a period of more than a decade allowed to model the asteroid's shape and gave two spin axis of (95.0°, −85.5°) and (272.0°, −88.0°) in ecliptic coordinates (λ, β) (U=n.a. ).


1011 Laodamia, Physical characteristics, Diameter and albedo
According to the survey carried out by NASA's Wide-field Infrared Survey Explorer and its subsequent NEOWISE mission, Laodamia measures 7.56 kilometers in diameter and its surface has an albedo of 0.248, while the Collaborative Asteroid Lightcurve Link adopts an albedo of 0.259 and derives a diameter of 7.39 kilometers based on an absolute magnitude of 12.74.


1011 Laodamia, Physical characteristics, Diameter and albedo
This makes Laodamia one of the largest mid-sized Mars-crossing asteroids comparable with 1065 Amundsenia (9.75 km), 1139 Atami (9.35 km), 1474 Beira (14.9 km), 1727 Mette (5.44 km), 1131 Porzia (7.13 km), 1235 Schorria (5.55 km), 985 Rosina (8.18 km), 1310 Villigera (15.24 km) and 1468 Zomba (7 km), but far smaller than the largest members of this dynamical group, namely, 132 Aethra, 323 Brucia, 1508 Kemi, 2204 Lyyli and 512 Taurinensis, which are all larger than 20 kilometers in diameter.


1011 Laodamia, Naming
This minor planet was named after Laodamia from Greek mythology. The asteroid's name was proposed by Russian astronomer Nikolaj Vasil'evich Komendantov (RI 740), see (3958).


1011 Laodamia, Naming
The name either refers to the daughter of Akastos, who was the wife of Protesilaos, see (3540), and killed in the Trojan War, as narrated by Euripides, see (2930). It may also refer to the daughter of Bellerophon, see (1808) and the wife of Sarpedon, see (2223). She was killed by the arrows of Artemis, see (105). (Source of name researched by the author of the Dictionary of Minor Planet Names, Lutz D. Schmadel).


1011 Woodland
1011 Woodland is the eighth studio album by British new wave band the Fixx, released in 1999. All but the last three tracks are re-recordings of previous songs done by the band, largely in an acoustic and modern form. The final three tracks are live recordings.


1012
Year in topic Year 1012 (MXII) was a leap year starting on Tuesday (link will display the full calendar) of the Julian calendar.


1012 Sarema
1012 Sarema (prov. designation: A924 AD or 1924 PM) is a dark background asteroid from the inner regions of the asteroid belt, approximately 21 kilometers (13 miles) kilometers in diameter. It was discovered on 12 January 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory at Heidelberg, Germany. The asteroid has a rotation period of 10.3 hours and probably an elongated shape. It was named after Sarema, a character in the poem The Fountain of Bakhchisaray by Aleksandr Pushkin, and the protagonist of the opera Sarema by Alexander von Zemlinsky based upon it.


1012 Sarema, Orbit and classification
Sarema is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Nysa family (405), the largest asteroid family of the main belt, consisting of stony and carbonaceous subfamilies. The family, named after 44 Nysa, is located in the inner belt near the Kirkwood gap (3:1 orbital resonance with Jupiter), a depleted zone that separates the central main belt.


1012 Sarema, Orbit and classification
It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.8 AU once every 3 years and 11 months (1,426 days; semi-major axis of 2.48 AU). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic.


1012 Sarema, Orbit and classification
The body's observation arc begins with its first observation as A907 VQ at Heidelberg in November 1907, more than 16 years prior to its official discovery observation.


1012 Sarema, Naming
This minor planet was named after a character in a poem by Aleksandr Pushkin, made into the opera Sarema by Alexander von Zemlinsky. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 97). The asteroid's name was suggested by Russian astronomer Nikolaj Komendantov (also see 3958 Komendantov).


1012 Sarema, Physical characteristics
In the Tholen classification, Sarema is an uncommon F-type asteroid of the carbonaceous C-complex.


1012 Sarema, Physical characteristics, Rotation period and poles
In April 1983, a first rotational lightcurve of Sarema was obtained from photometric observations by American astronomer Richard Binzel. Lightcurve analysis gave a well-defined rotation period of 10.32 hours with a brightness amplitude of 0.81 magnitude (U=3), which is indicative for an elongated, non-spherical shape.


1012 Sarema, Physical characteristics, Rotation period and poles
In 2009 and 2011, two modeled lightcurves gave a concurring sidereal period 10.30708 hours, combining sparse and dense photometric data from the Uppsala Asteroid Photometric Catalogue and other sources. The two studies also determined two spin axis of (45.0°, 67.0°) and (253.0°, 63.0°), as well as (51.0°, 64.0°) and (254.0°, 53.0°) in ecliptic coordinates (λ, β), respectively.


1012 Sarema, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Sarema measures between 16.06 and 22.96 kilometers in diameter and its surface has an albedo between 0.0342 and 0.07. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.045 and a diameter of 21.13 kilometers based on an absolute magnitude of 12.36.


1012 in Scotland
Events from the year 1012 in the Kingdom of Scotland.


10121 Arzamas
10121 Arzamas, provisional designation 1993 BS4, is a dark Themistian asteroid from the outer region of the asteroid belt, approximately 10 kilometers in diameter. The asteroid was discovered on 27 January 1993, by Belgian astronomer Eric Elst at Caussols (010) in southeastern France. It was later named after the Russian city of Arzamas.


10121 Arzamas, Orbit and classification
Arzamas is a member of the Themis family, a dynamical family of outer main-belt asteroids with nearly co-planar ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.7–3.7 AU once every 5 years and 9 months (2,095 days). Its orbit has an eccentricity of 0.15 and an inclination of 1° with respect to the ecliptic.


10121 Arzamas, Orbit and classification
The body's observation arc begins 22 years prior to its official discovery observation, when it was identified as 2118 T-1 at Palomar Observatory during the first Palomar–Leiden Trojan survey in 1971.


10121 Arzamas, Physical characteristics, Lightcurves
In February 2010, two rotational lightcurves of Arzamas were obtained from photometric observations at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 12.1 and 12.1991 hours with a brightness variation of 0.7 and 0.6 magnitude, respectively (U=2/2).


10121 Arzamas, Physical characteristics, Diameter and albedo
According to the NEOWISE mission of NASA's space-based Wide-field Infrared Survey Explorer, Arzamas measures 10.8 kilometer in diameter, and its surface has an albedo of 0.08. The Collaborative Asteroid Lightcurve Link also assumes an albedo of 0.08, characterizes it as a C-type asteroid, and calculates a diameter of 10.3 kilometers with an absolute magnitude of 13.4.


10121 Arzamas, Naming
This minor planet was named after the Russian city of Arzamas, a major transit center on the road from Moscow to the eastern parts of the country. It was founded in 1578 by Ivan the Terrible and is located on the Tyosha River, known for making leather and dyeing fabrics ever since. The official naming citation was published by the Minor Planet Center on 24 November 2007 (M.P.C. 61266).


1013
Year in topic Year 1013 (MXIII) was a common year starting on Thursday (link will display the full calendar) of the Julian calendar.


1013 Tombecka
1013 Tombecka (prov. designation: A924 BL or 1924 PQ) is a metallic Mitidika asteroid from the central regions of the asteroid belt, approximately 34 kilometers in diameter. It was discovered on 17 January 1924, by Russian-French astronomer Benjamin Jekhowsky at the Algiers Observatory in North Africa. The asteroid was named after the secretary of the Faculty of Sciences of Paris, D. Tombecka.


1013 Tombecka, Orbit and classification
Tombecka is a member of the Mitidika family, a small asteroid family of carbonaceous asteroids in the central main belt named after 2262 Mitidika. It has also been described generically as a stony Eunomian asteroid (502).


1013 Tombecka, Orbit and classification
The asteroid orbits the Sun in the central main-belt at a distance of 2.1–3.2 AU once every 4 years and 5 months (1,606 days). Its orbit has an eccentricity of 0.21 and an inclination of 12° with respect to the ecliptic. It was first identified as A905 UG at Heidelberg Observatory in October 1905. The body's observation arc begins at Heidelberg in 1931, approximately 7 years after its official discovery observation at Algiers.


1013 Tombecka, Naming
This minor planet was named after D. Tombeck, secretary of the Faculty of Sciences of Paris. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 97).


1013 Tombecka, Physical characteristics, Spectral type
Tombecka has been characterized as a metallic M-type asteroid by the Wide-field Infrared Survey Explorer (WISE). It has also been described as an Xk subtype, that transitions from the X-type to the K-type asteroids. In the Tholen classification, a determination of Tombecka's spectral type was inconclusive: numerical analysis of the asteroid's colors was closest to an X-type (which includes the M-type in this taxonomy), as well as in the vicinity of the C- and S-type asteroids.


1013 Tombecka, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's WISE telescope, Tombecka measures between 31.93 and 36.62 kilometers in diameter and its surface has an albedo between 0.120 and 0.1552.


1013 Tombecka, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.1552 and a diameter of 31.93 kilometers based on an absolute magnitude of 10.12.


1013 Tombecka, Physical characteristics, Mass and density
Tombecka  has an determined mass of (0.17±1.43)×1018 kilograms and a high (metallic) density of 7.50 g/cm3 with no porosity at all. The results correspond to an overall mean-diameter of 35.18 kilometers.


1013 Tombecka, Physical characteristics, Rotation period and poles
In 1986, several rotational lightcurves of Tombecka were obtained from photometric observations. Lightcurve analysis gave a rotation period between 6.0 and 6.0508 hours with a brightness variation of 0.35 to 0.50 magnitude (U=3/3/3/3).


1013 Tombecka, Physical characteristics, Rotation period and poles
In 2006, an international study modeled a lightcurve with a concurring period of 6.05017 hours and determined a spin axis of (4.0°, 62.0°) in ecliptic coordinates (λ,β) (Q=2).


1014
Year in topic Year 1014 (MXIV) was a common year starting on Friday (link will display the full calendar) of the Julian calendar, the 1014th in topic the 1014th year of the Common Era (CE) and Anno Domini (AD) designations, the 14th year of the 2nd millennium, the 14th year of the 11th century, and the 5th year of the 1010s decade.


1014 (film)
1014 (Burmese: ၁၀၁၄), is a Burmese historical drama film starring Kyaw Thu, Daung, Htun Ko Ko, Htoo Aung, Moht Moht Myint Aung, May Myint Mo, and Yadanar Bo. The film, produced by Wa Re Zein Film Production, premiered in Myanmar on December 19, 2019.


1014 Semphyra
1014 Semphyra, provisional designation 1924 PW, is a background asteroid from the central regions of the asteroid belt, approximately 17 kilometers in diameter. It was discovered on 29 January 1924, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The asteroid was named after the character "Semphyra" in a poem by Aleksandr Pushkin.


1014 Semphyra, Orbit and classification
Semphyra has not been associated with any known asteroid family. It orbits the Sun in the central main belt at a distance of 2.2–3.4 AU once every 4 years and 8 months (1,714 days). Its orbit has an eccentricity of 0.20 and an inclination of 2° with respect to the ecliptic.


1014 Semphyra, Orbit and classification
The body's observation arc begins with its official discovery observation at Heidelberg.


1014 Semphyra, Physical characteristics
In the SMASS classification, Semphyra is an Xe-subtype that transitions from the X-type to the bright E-type asteroids, while the Wide-field Infrared Survey Explorer characterizes it as a dark P-type.


1014 Semphyra, Physical characteristics, Rotation period
In February 2004, a rotational lightcurve of Semphyra was obtained from photometric observations by American astronomer Donald Pray at the Carbuncle Hill Observatory, Rhode Island (I00). The observations were made at a low phase angle of 1.6–2.9°. Lightcurve analysis gave a well-defined rotation period of 5.636 hours with a brightness amplitude of 0.12 magnitude (U=3), indicating that the body has a rather spheroidal shape.


1014 Semphyra, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's WISE, Semphyra measures between 14.89 and 17.487 kilometers in diameter and its surface has an albedo between 0.083 and 0.12.


1014 Semphyra, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceous asteroids of 0.057 and calculates a diameter of 23.21 kilometers based on an absolute magnitude of 11.9.


1014 Semphyra, Naming
This minor planet was named after the character "Semphyra" in a poem by Russian Aleksandr Pushkin (1799–1837), who was directly honored with the naming of (2208). The asteroid's official name was proposed by N. Komendantov (RI 740) and mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 97).


10140 Villon
10140 Villon, provisional designation 1993 SX4, is a Nysian asteroid from the inner regions of the asteroid belt, approximately 5 kilometers (3 miles) in diameter. It was discovered on 19 September 1993, by Belgian astronomer Eric Elst at the CERGA Observatory at Caussols in France. It was named after 15th-century French poet François Villon.


10140 Villon, Orbit and classification
Villon is member of the Nysa family (405), one of the largest asteroid families. It orbits the Sun in the inner main-belt at a distance of 2.1–2.7 AU once every 3 years and 9 months (1,375 days; semi-major axis of 2.42 AU). Its orbit has an eccentricity of 0.13 and an inclination of 3° with respect to the ecliptic. The body's observation arc begins with its first observations as 1973 GZ at the Crimean Astrophysical Observatory in April 1973, more than 20 years prior to its official discovery observation at Caussols.


10140 Villon, Physical characteristics
Villon's spectral type has not been determined, Based on its family classification and measured albedo (see below), it is likely a stony S-type asteroid. It has an absolute magnitude of 13.7. As of 2018, no rotational lightcurve of Villon has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.


10140 Villon, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Villon measures 4.785 kilometers in diameter and its surface has an albedo of 0.280.


10140 Villon, Naming
This minor planet was named after medieval French poet François Villon (1431–1463). The official naming citation was published by the Minor Planet Center on 28 July 1999 (M.P.C. 35493).


1015
Year in topic Year 1015 (MXV) was a common year starting on Saturday (link will display the full calendar) of the Julian calendar.


1015 Christa
1015 Christa, provisional designation 1924 QF, is a dark background asteroid from the outermost regions of the asteroid belt, approximately 96 kilometers (60 miles) in diameter. It was discovered on 31 January 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The meaning of this asteroids's name is unknown.


1015 Christa, Orbit and classification
Christa is a non-family asteroid from the main belt's background population. It orbits the Sun in the outermost asteroid belt at a distance of 2.9–3.5 AU once every 5 years and 9 months (2,096 days; semi-major axis of 3.21 AU). Its orbit has an eccentricity of 0.09 and an inclination of 9° with respect to the ecliptic.


1015 Christa, Orbit and classification
The asteroid was first observed as A916 UE at the Simeiz Observatory in October 1916. The body's observation arc begins at Heidelberg in February 1924, two days after its official discovery observation.


1015 Christa, Physical characteristics
In the Tholen classification, Christa is a common C-type asteroid, while in the SMASS classification, it is a Xc-subtype that transitions from the carbonaceous C-type to the X-type asteroids. It has also been characterized as a primitive P-type asteroid by the Wide-field Infrared Survey Explorer (WISE).


1015 Christa, Physical characteristics, Rotation period
In April 2005, a first rotational lightcurve of Christa was obtained from photometric observations by French amateur astronomers Raymond Poncy and René Roy. Lightcurve analysis gave a rotation period of 12.189 hours with a brightness variation of 0.20 magnitude (U=2). In January 2009, a refined period of 11.230 hours and an amplitude of 0.12 magnitude was measured by photometrist Brian Warner at his Palmer Divide Observatory in Colorado, United States (U=3-).


1015 Christa, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's WISE telescope, Christa measures between 82.35 and 101.04 kilometers in diameter and its surface has a low albedo between 0.04 and 0.064. The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0459 with a diameter of 96.94 kilometers based on an absolute magnitude of 9.03.


1015 Christa, Naming
Any reference of this minor planet's name to a person or occurrence is unknown.


1015 Christa, Naming, Unknown meaning
Among the many thousands of named minor planets, Christa is one of 120 asteroids, for which no official naming citation has been published. All of these low-numbered asteroids have numbers between 164 Eva and 1514 Ricouxa and were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth (also see category).


1016
Year 1016 (MXVI) was a leap year starting on Sunday (link will display the full calendar) of the Julian calendar.


1016 (album)
1016 is the third studio album by Spanish singer Alfred García. It was released on 14 December 2018 by Universal Music Spain. The album includes the singles "De la Tierra hasta Marte" and "Wonder". The album peaked at number 2 on the Spanish Albums Chart. In support of his debut studio album, 1016, García embarked on the 1016 Tour, which began on February 28, 2019 and ended on November 9, 2019. The album was re-released on 1 November 2019 titled 1016. El Círculo Rojo.


1016 (album), Singles
"De la Tierra hasta Marte" was released as the lead single from the album on 5 December 2018. The song peaked at number 12 on the Spanish Singles Chart. "Wonder" was released as the second single from the album on 7 June 2019. The song peaked at number 95 on the Spanish Singles Chart. "Londres" was released as the third single from the album on 27 September 2019. "Amar volar al invierno" was released as the lead single from the re-released album on 10 November 2019.


1016 Anitra
1016 Anitra, provisional designation 1924 QG, is a stony Florian asteroid and suspected asynchronous binary system from the inner regions of the asteroid belt, approximately 10 kilometers in diameter.


1016 Anitra
It was discovered on 31 January 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was likely named after the fictional character Anitra from Henrik Ibsen's drama Peer Gynt.


1016 Anitra, Orbit and classification
Anitra is a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.


1016 Anitra, Orbit and classification
It orbits the Sun in the inner main-belt at a distance of 1.9–2.5 AU once every 3 years and 4 months (1,208 days). Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic. The asteroid's observation arc begins at Heidelberg, 12 days after to its official discovery observation.


1016 Anitra, Physical characteristics
In the SMASS classification, Anitra is a common, stony S-type asteroid.


1016 Anitra, Physical characteristics, Rotation period
In November 2015, a rotational lightcurve of Anitra was obtained from photometric observations by an international collaborations of astronomers who combined their observational results. Lightcurve analysis gave a rotation period of 5.92951 hours with a brightness amplitude of 0.30 magnitude (U=3).


1016 Anitra, Physical characteristics, Binary system
Anitra is a suspected asynchronous binary asteroid, a system with a fairly large separation, for which tidal forces have been insufficient to synchronize the periods within the system's lifetime. The likely minor-planet moon has a rotation period of 2.609 hours and is thought to orbit its primary every 240 hours. The results, however, are still tentative. More than 100 known binaries from the asteroid belt have already been discovered.


1016 Anitra, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Anitra measures 9.539 and 10.302 kilometers in diameter and its surface has an albedo of 0.2728 and 0.308, respectively.


1016 Anitra, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony S-type asteroids of 0.20 and calculates a diameter of 12.97 kilometers based on an absolute magnitude of 11.8.


1016 Anitra, Naming
This minor planet was probably named after the Arabian dancer Anitra, daughter of a Bedouin chief in Henrik Ibsen's drama Peer Gynt, a five-act play in verse. The music was composed by Edvard Grieg who named one piece "Anitra's Dance". The minor planets (4872) and (5696) are named after Grieg and Ibsen, respectively.


1016 Anitra, Naming
The official naming citation is based on research by Lutz Schmadel and feedback from astronomers R. Bremer and I. van Houten-Groeneveld.


1017
Year 1017 (MXVII) was a common year starting on Tuesday (link will display the full calendar) of the Julian calendar.


1017 AM
The following radio stations broadcast on AM frequency 1017 kHz:


1017 AM, Tonga
This article related to radio communications is a stub. You can help Wikipedia by .


1017 Jacqueline
1017 Jacqueline (prov. designation: A924 CH or 1924 QL) is a dark background asteroid from the central regions of the asteroid belt. It was discovered on 4 February 1924, by Russian-French astronomer Benjamin Jekhowsky at the Algiers Observatory, Algeria, in North Africa. The carbonaceous C-type asteroid has a rotation period of 7.87 hours with a high brightness amplitude of 0.6 magnitude and measures approximately 39 kilometers (24 miles) in diameter. It was named after the French physicist and long-time pupil of the discoverer, Jacqueline Zadoc-Kahn Eisenmann (1904–1998).


1017 Jacqueline, Orbit and classification
Jacqueline is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the intermediate asteroid belt at a distance of 2.4–2.8 AU once every 4 years and 3 months (1,536 days; semi-major axis of 2.61 AU). Its orbit has an eccentricity of 0.08 and an inclination of 8° with respect to the ecliptic. The asteroid's earliest preserved observation dates back to 7 March 1924 at Heidelberg Observatory, where the body's observation arc begins in February 1928, nearly four years after its official discovery observation at Algiers–Bouzaréah.


1017 Jacqueline, Naming
This minor planet was named after Jacqueline Zadoc-Kahn Eisenmann (1904–1998), a French physicist and long-time student of Jekhowsky's. The naming was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 97).


1017 Jacqueline, Physical characteristics
In the Bus–Binzel SMASS classification, Jacqueline is a common, carbonaceous C-type asteroid.


1017 Jacqueline, Physical characteristics, Rotation period
In May 2000, a rotational lightcurve of Jacqueline was obtained from photometric observations by American photometrist Robert Stephens at the Santana Observatory (646) in California. Analysis of the classically shaped bimodal lightcurve gave a well-defined rotation period of 7.87±0.01 hours and a brightness variation of 0.6±0.02 magnitude, indicative of a non-spheroidal shape (U=3). Other measurements by Eric Barbotin and by astronomers at the Palomar Transient Factory gave a similar period of 7.873 and 7.875 hours with an amplitude of 0.72 and 0.43 magnitude, respectively (U=3-/2).


1017 Jacqueline, Physical characteristics, Rotation period
In 2016, a lightcurve was published using modeled photometric data from the Lowell Photometric Database. It gave a concurring sidereal period of 7.87149 hours, as well as two spin axes of (7.0°, 55.0°) and (170.0°, 65.0°) in ecliptic coordinates (λ, β).


1017 Jacqueline, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Jacqueline measures (37.65±3.4), (38.87±0.51) and (40.152±0.199) kilometers in diameter and its surface has an albedo of (0.0544±0.011), (0.051±0.002) and (0.052±0.005), respectively. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0497 and  a diameter of 37.61 kilometers based on an absolute magnitude of 11.0.


1017 Jacqueline, Physical characteristics, Diameter and albedo
Alternative mean-diameter measurements published by the WISE team include (29.523±10.14 km), (30.09±11.84 km), (31.991±0.454 km), (32.631±9.058 km) and (45.056±0.325 km) with corresponding albedos of (0.0670±0.0538), (0.07±0.06), (0.069±0.012), (0.06±0.02) and (0.0380±0.0053).


1017 Mafia: Incarcerated
1017 Mafia: Incarcerated is the thirteenth studio album by American rapper Gucci Mane. The mixtape was released on January 3, 2015, by 1017 Records and 101 Distribution. The tape features guest appearances from Migos, Peewee Longway, Rich The Kid, Waka Flocka Flame, OG Maco, Young Scooter and Young Thug.


1017 Mafia: Incarcerated, Singles
The mixtape's lead single, "Lowest", was released on November 24, 2014, and included guest features from Rich the Kid and OG Maco. The mixtape's second single, "Get Back", was released on December 2, 2014, and includes a guest feature from Raury.


1017 Records
The New 1017 Records, also known as 1017 Global Music, LLC and formerly 1017 Brick Squad, So Icey Entertainment & 1017 Eskimo, is an American record label founded by Gucci Mane after his departure from Mizay Entertainment and the closing of So Icey. The label was home to Ralo, Hoodrich Pablo Juan, and others.


1017 Records, History, 2007–2013
In 2007 Gucci Mane founded his first independent record label, So Icey Entertainment, after signing with Mizay Entertainment. Soon after Gucci released his independent album, Trap-A-Thon. On May 4, 2010, he announced that he was closing So Icey Entertainment and leaving Mizay Entertainment due to business concerns with Debra Antney.


1017 Records, History, 2007–2013
Gucci Mane then stated that he was starting his own record label (1017 Brick Squad) and that his employer, Jerry Alvarado, was already signing a distribution deal with Asylum Records


1017 Records, History, 2007–2013
While still signed to Mizay Entertainment, OJ Da Juiceman and Waka Flocka Flame were first artists signed to 1017 Brick Squad


1017 Records, History, 2007–2013
Juiceman's debut album was unofficially released through the 1017 Brick Squad record label (it was officially released through Asylum Records and Mizay Entertainment). The first mainstream success for 1017 Brick Squad occurred in 2009, when Gucci released The State vs. Radric Davis.


1017 Records, History, 2007–2013
In 2010, Brick Squad artist Waka Flocka Flame released his debut album, Flockaveli, through Brick Squad, Mizay Entertainment, and Warner Bros.


1017 Records, History, 2007–2013
On September 28, 2010, Gucci Mane released his seventh studio album, The Appeal: Georgia's Most Wanted.


1017 Records, History, 2007–2013
On December 16, 2011, while preparing for a music video at an Atlanta recording studio, Brick Squad artist Slim Dunkin was shot and killed while arguing with another person in the building, later identified as Atlanta rapper Young Vito.


1017 Records, History, 2007–2013
On February 25, 2013, Young Vito was acquitted of murdering Slim Dunkin, but he was given a 25-year sentence for aggravated assault and possession of a firearm.


1017 Records, History, 2013–2016
On March 15, 2013, via Twitter, Gucci Mane tweeted that he "dropped" Waka Flocka Flame and that Waka was no longer a member of 1017 Brick Squad.


1017 Records, History, 2013–2016
The next day, Gucci's management claimed his Twitter account was hacked and he did not send the tweet about Waka Flocka.


1017 Records, History, 2013–2016
However, Waka would claim this to be false and later diss Gucci Mane at a Dipset reunion concert in New York City. On March 27, 2013, Waka told MTV that it would be impossible for him to be dropped from 1017 Brick Squad as he owns stake in the company. He also confirmed that there was indeed a feud going on between the rappers and "they would never make music or do business together again."


1017 Records, History, 2013–2016
On September 7, 2013, various members of 1017 Brick Squad and Brick Squad Monopoly argued back and forth on Twitter. This was the culmination of a label-wide communication breakdown and spawned Brick Squad Mafia, the label run by Mack Drama which is where Frenchie, along with a multitude of other Brick Squad Artists, first ended up after splitting from the primary group.


1017 Records, History, 2013–2016
Mack Drama is also known for being the key to Flocka's street credibility. Mack Drama had the young rapper fly out to meet with other OG Elm Street Pirus, and with a nod by the gang in its original location, by its original founding members, Flocka had his approval for repping the gang. As Mack Drama sided with Gucci Mane in the greater dispute within the label, Mack Drama and Waka Flocka have since part ways from one another. Mack Drama then went on to be the driving force behind artists like Don P (Formerly known as Fatal) and "Vee tha Rula" (who was later signed to Kid Ink), Gucci Mane, Frenchie, Wooh da Kid, and OJ da Juiceman.


1017 Records, History, 2013–2016
Gucci Mane would go on to say "fuck brick squad" and accuse his former manager, Waka Flocka's mom Debra Antney, of stealing money from OJ da Juiceman and Frenchie. Frenchie also accused Gucci Mane of paying for Young Vito's lawyer, the accused murderer of former 1017 Brick Squad artist Slim Dunkin, which Gucci denied. Then Frenchie released a diss record toward Gucci the following day.


1017 Records, History, 2016–present
Upon Gucci Mane's latest release from incarceration, he created a new record label, 1017 Eskimo, a partnership venture with Alamo/Empire Distribution. Artists signed to 1017 Eskimo included Hoodrich Pablo Juan and Lil Wop. In 2020, Gucci rebranded his label as 1017 Global Music, LLC, and partnered up with Atlantic to distribute music for his signees. He released a compilation album called Gucci Mane Presents: So Icy Summer in July 2020 introducing his artists. He and his label mates released So Icy Gang Vol.1 in October 2020.


1017 vs. the World
1017 vs. the World is a collaborative EP by American rappers Lil Uzi Vert and Gucci Mane. It was released on November 23, 2016, by Generation Now and GUWOP. The EP features production by Honorable C.N.O.T.E., D. Rich, Mannie Fresh, Zaytoven, DP Beats and GLOhan Beats.


1018
Year 1018 (MXVIII) was a common year starting on Wednesday (link will display the full calendar) of the Julian calendar.


1018 Arnolda
1018 Arnolda, provisional designation 1924 QM, is a stony asteroid from the central regions of the asteroid belt, approximately 16 kilometers in diameter. It was discovered on 3 March 1924, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after physicist Arnold Berliner.


1018 Arnolda, Classification and orbit
Arnolda is not a member of any known asteroid family. It orbits the Sun in the central main belt at a distance of 1.9–3.2 AU once every 4 years and 1 month (1,480 days). Its orbit has an eccentricity of 0.25 and an inclination of 8° with respect to the ecliptic. The body's observation arc begins nine days prior to its official discovery observation at Heidelberg.


1018 Arnolda, Physical characteristics
Arnolda is an assumed stony S-type asteroid, a very common type in the inner and in parts of the central asteroid belt.


1018 Arnolda, Physical characteristics, Lightcurves
In May 2005, the best-rated rotational lightcurve of Arnolda was obtained from photometric observations by Australian astronomers at the Oakley Southern Sky Observatory (E09). Lightcurve analysis gave a rotation period of 14.617 hours with a brightness variation of 0.33 magnitude (U=3). Several other astronomers obtained number of lesser-rated lightcurves with a shorter period (U=n.a./1/2/3-).


1018 Arnolda, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Arnolda measures between 13.68 and 16.557 kilometers in diameter  and its surface has an albedo between 0.29 and 0.439.


1018 Arnolda, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives a high albedo of 0.3760 and a diameter of 16.44 kilometers based on an absolute magnitude of 10.60.


1018 Arnolda, Naming
This minor planet was named after physicist Arnold Berliner (1862–1942), on the occasion of his 70th birthday in 1933. Berliner was the editor of the prominent German periodical scientific magazine Naturwissenschaften (AN 247).


1018 in Scotland
Events from the year 1018 in the Kingdom of Scotland.


1019
Year 1019 (MXIX) was a common year starting on Thursday (link will display the full calendar) of the Julian calendar.


1019 (album)
1019 is the debut studio album by Taiwanese singer Jolin Tsai. It was released on 10 September 1999, by Universal Music Taiwan. Tsai emerged champion at an MTV singing competition at the age of 18, and it kickstarted her singing career and paved the way to her journey in becoming a teen idol. In March 1999, Tsai signed a recording deal with Universal. After she signed with the label, Tsai's debut single, "Living with the World", was released in July 1999.


1019 (album)
The single was a big success, and led to the release of the album, which has sold more than 400,000 copies in Taiwan alone. Referred to as the "Teenage Boy Killer", Tsai became an instant hit among teenagers in Taiwan. The lead single, "I Know You're Feeling Blue", reached number 30 on the Hit FM Top 100 Singles of the Year.


1019 I Can Concert
1019 I Can Concert (Chinese: 1019我可以演唱會) is the first live album by Taiwanese singer Jolin Tsai. It was released on 26 March 2000, by Universal Music Taiwan. It chronicles Tsai's 1019 I Can Concert at Nankang 101 in Taipei, Taiwan on 4 December 1999.


1019 Strackea
1019 Strackea, provisional designation 1924 QN, is a stony Hungaria asteroid of the inner asteroid belt, approximately 8 kilometers in diameter. It was discovered on 3 March 1924, by astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany. It is named for German astronomer Gustav Stracke.


1019 Strackea, Classification and orbit
Strackea is a member of the Hungaria group, a dynamical group forming the innermost dense concentration of asteroids in the Solar System. It is, however, a non-family asteroid of the background population, and not a member of the (collisional) Hungaria family. It orbits the Sun at a distance of 1.8–2.0 AU once every 2 years and 8 months (965 days). Its orbit has an eccentricity of 0.07 and an inclination of 27° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg in 1924.


1019 Strackea, Physical characteristics
In the Tholen classification, Strackea is a common, stony S-type asteroid.


1019 Strackea, Physical characteristics, Lightcurve
The first valid rotational lightcurve of Strackea with a period of 4.05 hours and a brightness variation of 0.17 magnitude was obtained by French amateur astronomer Laurent Bernasconi in February 2006 (U=2). Since then, several well-defined lightcurves with a period between 4.044 and 4.052 hours and an amplitude of 0.15 to 0.25 magnitude were obtained by astronomers Brian Warner, Richard Schmidt, as well as by the group of astronomers Pierre Antonini, Raoul Behrend, Roberto Crippa and Federico Manzini (U=3/3-/3-/3/3).


1019 Strackea, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Strackea measures between 7.169 and 8.79 kilometers in diameter and its surface has an albedo between 0.206 and 0.39. The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.2236 and a diameter of 8.37 kilometers with an absolute magnitude of 12.63.


1019 Strackea, Naming
This minor planet was named after German astronomer Gustav Stracke (1887–1943), who was in charge of the minor planet department at the Berlin-based Astronomical Calculation Institute, despite his wish that he not be honored in this fashion. Previously, the discoverer had circumvented Stracke's wish by accordingly naming a consecutively numbered sequence of asteroids, so that their first letters form the name "G. Stracke". These minor planets, in the number range from 1227 to 1234, were:


1019 Strackea, Naming
Naming citation was first published by Paul Herget in The Names of the Minor Planets in 1955 (H 97).


101955 Bennu
101955 Bennu (provisional designation 1999 RQ36) is a carbonaceous asteroid in the Apollo group discovered by the LINEAR Project on 11 September 1999. It is a potentially hazardous object that is listed on the Sentry Risk Table and tied for the highest cumulative rating on the Palermo Technical Impact Hazard Scale. It has a cumulative 1-in-1,800 chance of impacting Earth between 2178 and 2290 with the greatest risk being on 24 September 2182. It is named after the Bennu, the ancient Egyptian mythological bird associated with the Sun, creation, and rebirth.


101955 Bennu
101955 Bennu has a mean diameter of 490 m (1,610 ft; 0.30 mi) and has been observed extensively with the Arecibo Observatory planetary radar and the Goldstone Deep Space Network.


101955 Bennu
Bennu was the target of the OSIRIS-REx mission which is intended to return its samples to Earth in 2023 for further study. On 3 December 2018, the OSIRIS-REx spacecraft arrived at Bennu after a two-year journey. It orbited the asteroid and mapped out Bennu's surface in detail, seeking potential sample collection sites. Analysis of the orbits allowed calculation of Bennu's mass and its distribution.


101955 Bennu
On 18 June 2019, NASA announced that the OSIRIS-REx spacecraft had closed in and captured an image from a distance of 600 metres (2,000 ft) from Bennu's surface.


101955 Bennu
In October 2020, OSIRIS-REx successfully touched down on the surface of Bennu, collected a sample using an extendable arm, secured the sample and prepared for a return trip to Earth. On 10 May 2021, OSIRIS-REx successfully completed its departure from the Bennu asteroid while still carrying the sample of the asteroid rubble.


101955 Bennu, Discovery and observation
Bennu was discovered on 11 September 1999 during a Near-Earth asteroid survey by the Lincoln Near-Earth Asteroid Research (LINEAR). The asteroid was given the provisional designation 1999 RQ36 and classified as a near-Earth asteroid. Bennu was observed extensively by the Arecibo Observatory and the Goldstone Deep Space Network using radar imaging as Bennu closely approached Earth on 23 September 1999.


101955 Bennu, Discovery and observation, Naming
The name Bennu was selected from more than eight thousand student entries from dozens of countries around the world who entered a "Name That Asteroid!" contest run by the University of Arizona, The Planetary Society, and the LINEAR Project in 2012. Third-grade student Michael Puzio from North Carolina proposed the name in reference to the Egyptian mythological bird Bennu. To Puzio, the OSIRIS-REx spacecraft with its extended TAGSAM arm resembled the Egyptian deity, which is typically depicted as a heron.


101955 Bennu, Discovery and observation, Naming
Its features will be named after birds and bird-like creatures in mythology.


101955 Bennu, Physical characteristics
Bennu has a roughly spheroidal shape, resembling a spinning top. Bennu's axis of rotation is tilted 178 degrees to its orbit; the direction of rotation about its axis is retrograde with respect to its orbit. While the initial ground based radar observations indicated that Bennu had a fairly smooth shape with one prominent 10–20 m boulder on its surface, high resolution data obtained by OSIRIS-REx revealed that the surface is much rougher with more than 200 boulders larger than 10 m on the surface, the largest of which is 58 m across.


101955 Bennu, Physical characteristics
The boulders contain veins of high albedo carbonate minerals believed to have formed prior to the formation of the asteroid due to hot water channels on the much larger parent body. The veins range from 3 to 15 centimeters wide, and can be over one meter in length, much bigger than carbonate veins seen in meteorites.


101955 Bennu, Physical characteristics
There is a well-defined ridge along the equator of Bennu. The presence of this ridge suggests that fine-grained regolith particles have accumulated in this area, possibly because of its low gravity and fast rotation. Observations by the OSIRIS-REx spacecraft has shown that Bennu is rotating faster over time. This change in Bennu's rotation is caused by the Yarkovsky–O'Keefe–Radzievskii–Paddack effect, or the YORP effect. Due to the uneven emission of thermal radiation from its surface as Bennu rotates in sunlight, the rotation period of Bennu decreases by about one second every 100 years.


101955 Bennu, Physical characteristics
Observations of this minor planet by the Spitzer Space Telescope in 2007 gave an effective diameter of 484±10 m, which is in line with other studies. It has a low visible geometric albedo of 0.046±0.005. The thermal inertia was measured and found to vary by approximately 19% during each rotational period. It was based on this observation scientists (incorrectly) estimated a moderate regolith grain size, ranging from several millimeters up to a centimeter, evenly distributed. No emission from a potential dust coma has been detected around Bennu, which puts a limit of 106 g of dust within a radius of 4750 km.


101955 Bennu, Physical characteristics
Astrometric observations between 1999 and 2013 have demonstrated that 101955 Bennu is influenced by the Yarkovsky effect, causing the semimajor axis of its orbit to drift on average by 284±1.5 meters/year. Analysis of the gravitational and thermal effects has given a bulk density of ρ = 1190±13 kg/m3, which is only slightly denser than water. Therefore, the predicted macroporosity is 40±10%, suggesting the interior has a rubble pile structure or even hollows. The estimated mass is (7.329±0.009)×1010 kg.


101955 Bennu, Physical characteristics, Photometry and spectroscopy
Photometric observations of Bennu in 2005 yielded a synodic rotation period of 4.2905±0.0065 h. It has a B-type classification, which is a sub-category of carbonaceous asteroids. Polarimetric observations show that Bennu belongs to the rare F subclass of carbonaceous asteroids, which is usually associated with cometary features. Measurements over a range of phase angles showed a phase function slope of 0.040 magnitudes per degree, which is similar to other near-Earth asteroids with low albedo.


101955 Bennu, Physical characteristics, Photometry and spectroscopy
Before OSIRIS-REx, spectroscopy indicated a correspondence with the CI and/or CM carbonaceous chondrite meteorites, including carbonaceous-chondrite mineral magnetite. Magnetite, a spectrally prominent water product but destroyed by heat, is an important proxy of astronomers including OSIRIS-REx staff.


101955 Bennu, Physical characteristics, Water
Predicted beforehand, Dante Lauretta (University of Arizona) then stated that Bennu is water-rich- already detectable while OSIRIS-REx was still technically in approach.


101955 Bennu, Physical characteristics, Water
Preliminary spectroscopic surveys of the asteroid's surface by OSIRIS-REx confirmed magnetite and the meteorite-asteroid linkage, dominated by phyllosilicates. Phyllosilicates, among others, hold water. Bennu's water spectra were detectable on approach, reviewed by outside scientists, then confirmed from orbit.


101955 Bennu, Physical characteristics, Water
OSIRIS-REx observations have resulted in a (self-styled) conservative estimate of about 7 x 108 kg water in one form alone, neglecting additional forms. This is a water content of ~1 wt.%, and potentially much more. In turn this suggests transient pockets of water beneath Bennu's regolith. The surficial water may be lost from the collected samples. However, if the sample return capsule maintains low temperatures, the largest (centimeter-scale) fragments may contain measurable quantities of adsorbed water, and some fraction of Bennu's ammonium compounds.


101955 Bennu, Physical characteristics, Activity
Bennu is an active asteroid, sporadically emitting plumes of particles and rocks as large as 10 cm (3.9 in), (not dust, defined as tens of micrometers). Scientists hypothesize the releases may be caused by thermal fracturing, volatile release through dehydration of phyllosilicates, pockets of subsurface water, and/or meteoroid impacts.


101955 Bennu, Physical characteristics, Activity
Before the arrival of OSIRIS-REx, Bennu had displayed polarization consistent with Comet Hale-Bopp and 3200 Phaethon, a rock comet. Bennu, Phaethon, and inactive Manx comets are examples of active asteroids. B-type asteroids displaying a blue color in particular, may be dormant comets. If the IAU declares Bennu to be a dual-status object, its comet designation would be P/1999 RQ36 (LINEAR).


101955 Bennu, Physical characteristics, Surface features
All geological features on Bennu are named after various species of birds and bird-like figures in mythology. The first features to be named were the final four candidate OSIRIS-REx sample sites, which were given unofficial names by the team in August 2019. On 6 March 2020 the IAU announced the first official names for 12 Bennu surface features, including regiones (broad geographic regions), craters, dorsa (ridges), fossae (grooves or trenches) and saxa (rocks and boulders).


101955 Bennu, Physical characteristics, Surface features, Candidate sample sites
On 12 December 2019, after a year of mapping Bennu's surface, a target site was announced. Named Nightingale, the area is near Bennu's north pole and lies inside a small crater within a larger crater. Osprey was selected as the backup sample site.


101955 Bennu, Origin and evolution
The carbonaceous material that composes Bennu originally came from the breakup of a much larger parent body—a planetoid or a proto-planet. But like nearly all other matter in the Solar System, the origins of its minerals and atoms are to be found in dying stars such as red giants and supernovae. According to the accretion theory, this material came together 4.5 billion years ago during the formation of the Solar System.


101955 Bennu, Origin and evolution
Bennu's basic mineralogy and chemical nature would have been established during the first 10 million years of the Solar System's formation, where the carbonaceous material underwent some geologic heating and chemical transformation inside a much larger planetoid or a proto-planet capable of producing the requisite pressure, heat and hydration (if need be)—into more complex minerals. Bennu probably began in the inner asteroid belt as a fragment from a larger body with a diameter of 100 km. Simulations suggest a 70% chance it came from the Polana family and a 30% chance it derived from the Eulalia family. Impactors on boulders of Bennu indicate that Bennu has been in near earth orbit (separated from the main asteroid belt) for 1–2.5 million years.


101955 Bennu, Origin and evolution
Subsequently, the orbit drifted as a result of the Yarkovsky effect and mean motion resonances with the giant planets, such as Jupiter and Saturn. Various interactions with the planets in combination with the Yarkovsky effect modified the asteroid, possibly changing its spin, shape, and surface features.


101955 Bennu, Origin and evolution
Cellino et al. have suggested a possible cometary origin for Bennu, based on similarities of its spectroscopic properties with known comets. The estimated fraction of comets in the population of near Earth objects is 8%±5%. This includes rock comet 3200 Phaethon, originally discovered as, and still numbered as an asteroid.


101955 Bennu, Orbit
Bennu currently orbits the Sun with a period of 1.20 years (437 days). Earth gets as close as about 480,000 km (0.0032 au) from its orbit around 23 to 25 September. On 22 September 1999 Bennu passed 0.0147 au from Earth, and six years later on 20 September 2005 it passed 0.033 au from Earth. The next close approaches of less than 0.09 au will be 30 September 2054 and then 23 September 2060, which will perturb the orbit slightly. Between the close approach of 1999 and that of 2060, Earth completes 61 orbits and Bennu 51.


101955 Bennu, Orbit
An even closer approach will occur on 25 September 2135 around 0.0014 au (see below). In the 75 years between the 2060 and 2135 approaches, Bennu completes 64 orbits, meaning its period will have changed to 1.17 years (427 days). The Earth approach of 2135 will increase the orbital period to about 1.24 years (452 days). Before the 2135 Earth approach, Bennu's maximum distance from the Earth occurs on 27 November 2045 at a distance of 2.34 AU (350 million km).


101955 Bennu, Orbit, Possible Earth impact
On average, an asteroid with a diameter of 500 m (1,600 ft; 0.31 mi) can be expected to impact Earth about every 130,000 years or so. A 2010 dynamical study by Andrea Milani and collaborators predicted a series of eight potential Earth impacts by Bennu between 2169 and 2199. The cumulative probability of impact is dependent on physical properties of Bennu that were poorly known at the time, but was found to not exceed 0.071% for all eight encounters. The authors recognized that an accurate assessment of 101955 Bennu's probability of Earth impact would require a detailed shape model and additional observations (either from the ground or from spacecraft visiting the object) to determine the magnitude and direction of the Yarkovsky effect.


101955 Bennu, Orbit, Possible Earth impact
The publication of the shape model and of astrometry based on radar observations obtained in 1999, 2005, and 2011 made possible an improved estimate of the Yarkovsky acceleration and a revised assessment of the impact probability. In 2014, the best estimate of the impact probability was a cumulative probability of 0.037% in the interval 2175 to 2196. This corresponds to a cumulative score on the Palermo scale of −1.71. If an impact were to occur, the expected kinetic energy associated with the collision would be 1,200 megatons in TNT equivalent (for comparison, TNT equivalent of Little Boy was approx 0.015 megaton).


101955 Bennu, Orbit, Possible Earth impact
The 2021 orbit solution extended the virtual impactors from the year 2200 to the year 2300 and slightly increased the cumulative Palermo impact scale to −1.42. The solution even included the estimated masses of 343 other asteroids and represents about 90% of the total mass of the main asteroid belt.


101955 Bennu, Orbit, 2060/2135 close approaches
Bennu will pass 0.005 au (750,000 km; 460,000 mi) from Earth on 23 September 2060, while the Moon's average orbital distance (Lunar Distance, LD) is 384,402 km (238,856 mi) today and will be 384,404 km in 50 years time. It will be too dim to be seen with common binoculars. The close approach of 2060 causes divergence in the close approach of 2135. On 25 September 2135, the Earth approach distance is 0.00136 au (203,000 km; 126,000 mi) ±20 thousand km. There is no chance of an Earth impact in 2135. The 2135 approach will create many lines of variations and Bennu may pass through a gravitational keyhole during the 2135 passage which could create an impact scenario at a future encounter. The keyholes are all less than ~20 km wide with some keyholes being only 5 meters wide.


101955 Bennu, Orbit, 2060/2135 close approaches, 2182
The most threatening virtual impactor is on 24 September 2182 when there is a 1 in 2,700 chance of an Earth impact, but the asteroid could be as far as the Sun is from Earth. To impact Earth on 24 September 2182 Bennu needs to pass through a keyhole roughly 5 km wide on 25 September 2135. The next two biggest risks occur in 2187 (1:14,000) and 2192 (1:26,000). There is a cumulative 1 in 1,800 chance of an Earth impact between 2178 and 2290.


101955 Bennu, Orbit, Long term
Lauretta et al. reported in 2015 their results of a computer simulation, concluding that it is more likely that 101955 Bennu will be destroyed by some other cause:


101955 Bennu, Orbit, Long term
The orbit of Bennu is intrinsically dynamically unstable, as are those of all NEOs. In order to glean probabilistic insights into the future evolution and likely fate of Bennu beyond a few hundred years, we tracked 1,000 virtual "Bennus" for an interval of 300 Myr with the gravitational perturbations of the planets Mercury–Neptune included. Our results ... indicate that Bennu has a 48% chance of falling into the Sun. There is a 10% probability that Bennu will be ejected out of the inner Solar System, most likely after a close encounter with Jupiter. The highest impact probability for a planet is with Venus (26%), followed by the Earth (10%) and Mercury (3%). The odds of Bennu striking Mars are only 0.8% and there is a 0.2% chance that Bennu will eventually collide with Jupiter.


101955 Bennu, Orbit, Meteor shower
As an active asteroid with a small minimum orbit intersection distance from Earth, Bennu may be the parent body of a weak meteor shower. Bennu particles would radiate around 25 September from the southern constellation of Sculptor. The meteors are expected to be near the naked eye limit and only produce a Zenith hourly rate of less than 1.


101955 Bennu, OSIRIS-REx
The OSIRIS-REx mission of NASA's New Frontiers program was launched towards 101955 Bennu on 8 September 2016. On 3 December 2018, the spacecraft arrived at the asteroid Bennu after a two-year journey. One week later, at the American Geophysical Union Fall Meeting, investigators announced that OSIRIS-REx had discovered spectroscopic evidence for hydrated minerals on the surface of the asteroid, implying that liquid water was present in Bennu's parent body before it split off.


101955 Bennu, OSIRIS-REx
On 20 October 2020, OSIRIS-REx descended to the asteroid and "pogo-sticked off" it while successfully collecting a sample. OSIRIS-REx is expected to return samples to Earth in 2023 via a capsule-drop by parachute, ultimately, from the spacecraft to the Earth's surface in Utah on 24 September. On 7 April 2021, OSIRIS-REx completed its final flyover of the asteroid and began slowly drifting away from it. On 10 May 2021, the departure was completed with OSIRIS-REx while still managing to contain the asteroid sample.


101955 Bennu, OSIRIS-REx, Selection
The asteroid Bennu was selected from over half a million known asteroids by the OSIRIS-REx selection committee. The primary constraint for selection was close proximity to Earth, since proximity implies low impulse (Δv) required to reach an object from Earth orbit. The criteria stipulated an asteroid in an orbit with low eccentricity, low inclination, and an orbital radius of 0.8–1.6 au. Furthermore, the candidate asteroid for a sample-return mission must have loose regolith on its surface, which implies a diameter greater than 200 meters. Asteroids smaller than this typically spin too fast to retain dust or small particles. Finally, a desire to find an asteroid with pristine carbon material from the early Solar System, possibly including volatile molecules and organic compounds, reduced the list further.


101955 Bennu, OSIRIS-REx, Selection
With the above criteria applied, five asteroids remained as candidates for the OSIRIS-REx mission, and Bennu was chosen, in part for its potentially hazardous orbit.


101955 Bennu, Gallery
A compilation of radar images of asteroid Bennu (left) and a corresponding 3D shape model. (right)


101955 Bennu, Gallery
This picture, taken by the OSIRIS-REx spacecraft on November 2, 2018, was part of a sequence of frames collected to show asteroid 101955 Bennu rotating. Bennu is approximately 200 pixels wide in this shot.


101955 Bennu, Gallery
Animation of OSIRIS-REx collecting a sample from the surface of Bennu.


10199 Chariklo
10199 Chariklo /ˈkærɪkloʊ/ is the largest confirmed centaur (small body of the outer Solar System). It orbits the Sun between Saturn and Uranus, grazing the orbit of Uranus. On 26 March 2014, astronomers announced the discovery of two rings (nicknamed as the rivers Oiapoque and Chuí) around Chariklo by observing a stellar occultation, making it the first minor planet known to have rings.


10199 Chariklo
Chariklo was discovered by James V. Scotti of the Spacewatch program on February 15, 1997. Chariklo is named after the nymph Chariclo (Χαρικλώ), the wife of Chiron and the daughter of Apollo.


10199 Chariklo
A photometric study in 2001 was unable to find a definite period of rotation. Infrared observations of Chariklo indicate the presence of water ice, which may in fact be located in its rings.


10199 Chariklo
Michael Brown's website lists it as possibly a dwarf planet with a measured diameter of 232 km.


10199 Chariklo, Size and shape
Chariklo is currently the largest known centaur, with an equivalent diameter of 252 km. Its shape is probably elongated with dimensions 296 × 264 × 204 km. (523727) 2014 NW65 is likely to be the second largest with 225 km (140 mi) and 2060 Chiron is likely to be the third largest with 220 km (140 mi).


10199 Chariklo, Orbit
Centaurs originated in the Kuiper belt and are in dynamically unstable orbits that will lead to ejection from the Solar System, an impact with a planet or the Sun, or transition into a short-period comet.


10199 Chariklo, Orbit
The orbit of Chariklo is more stable than those of Nessus, Chiron, and Pholus. Chariklo lies within 0.09 AU of the 4:3 resonance of Uranus and is estimated to have a relatively long orbital half-life of about 10.3 Myr. Orbital simulations of twenty clones of Chariklo suggest that Chariklo will not start to regularly come within 3 AU (450 Gm) of Uranus for about thirty thousand years.


10199 Chariklo, Orbit
During the perihelic oppositions of 2003–04, Chariklo had an apparent magnitude of +17.7. As of 2014, Chariklo was 14.8 AU from the Sun.


10199 Chariklo, Rings
A stellar occultation in 2013 revealed that Chariklo has two rings with radii 396 and 405 km and widths of about 7 km and 3.5 km respectively. The rings are approximately 9 km apart. This makes Chariklo the smallest known object to have rings. These rings are consistent with an edge-on orientation in 2008, which can explain Chariklo's dimming before 2008 and brightening since. Nonetheless, the elongated shape of Chariklo explains most of the brightness variability resulting in darker rings than previously determined. Furthermore, the rings can explain the gradual disappearance of the water-ice features in Chariklo's spectrum before 2008 and their reappearance thereafter if the water ice is in Chariklo's rings.


10199 Chariklo, Rings
The existence of a ring system around a minor planet was unexpected because it had been thought that rings could only be stable around much more massive bodies. Ring systems around minor bodies had not previously been discovered despite the search for them through direct imaging and stellar occultation techniques. Chariklo's rings should disperse over a period of at most a few million years, so either they are very young, or they are actively contained by shepherd moons with a mass comparable to that of the rings. However, other research suggests that Chariklo's elongated shape combined with its fast rotation can clear material in an equatorial disk through Lindblad resonances and explain the survival and location of the rings, a mechanism valid also for the ring of Haumea.


10199 Chariklo, Rings
The team nicknamed the rings Oiapoque (the inner, more substantial ring) and Chuí (the outer ring), after the two rivers that form the northern and southern coastal borders of Brazil. A request for formal names will be submitted to the IAU at a later date.


10199 Chariklo, Rings
It has been speculated that 2060 Chiron may have a similar pair of rings.


10199 Chariklo, Exploration
Camilla is a mission concept published in June 2018 that would launch a robotic probe to perform a single flyby of Chariklo and drop off a 100 kg (220 lb) impactor made of tungsten to excavate a crater approximately 10 m (33 ft) deep for remote compositional analysis during the flyby. The mission would be designed to fit under the cost cap of NASA's New Frontiers program, although it has not been formally proposed to compete for funding.


101: The Airborne Invasion of Normandy
101: The Airborne Invasion of Normandy is a 1998 computer wargame developed by Interactive Simulations and published by Empire Interactive. Key members of the team had previously worked at Random Games, developer of Soldiers at War and Wages of War.


101: The Airborne Invasion of Normandy, Gameplay
101: The Airborne Invasion of Normandy is a turn-based computer wargame that simulates combat at the squad level, in a manner that has been compared to games such as X-COM. The game recreates the 101st Airborne Division's use of paratroopers during the Invasion of Normandy in World War II.


101: The Airborne Invasion of Normandy, Development
101 was developed by Interactive Simulations, Inc. (ISI), a team started by former members of Random Games, creator of Soldiers at War and Wages of War. ISI president Tim Brooks said that he founded the studio to obtain "more control over deciding what went into the game and what didn't go into the game." 101 was released in October 1998.


101: The Airborne Invasion of Normandy, Reception
101 sold 10,000 copies in the United States by April 1999, according to Tim Brooks. James Fudge of Computer Games Strategy Plus called the game "semi-popular" by that time, while Wargamer's Mario Kroll dubbed it a commercial flop in 2003. He explained that it had failed to secure the retail shelf space necessary to succeed: "copies of the game weren't available over Christmas after the release, and shortly thereafter its developer went belly-up, completely abandoned by its publisher", he wrote. Kroll noted that 101's distribution issues were part of a trend for less established development teams at the time.


101: The Airborne Invasion of Normandy, Reception
According to Kroll, 101 "received plenty of positive press". CNET Gamecenter, GameSpot and Computer Games Strategy Plus nominated it for their respective "Wargame of the Year" prizes, which went variously to The Operational Art of War I: 1939–1955 and People's General.


101: The Airborne Invasion of Normandy, Reception
In Computer Games Strategy Plus, David Finn offered 101 a glowing review and hailed it as "probably the first tactical squad level wargame with this scope of realism and detail." William R. Trotter of PC Gamer US was also positive. Writing for GameSpot, Alan Dunkin remarked, "While the scope is limited and the level of detail can intimidate some, 101: The Airborne Invasion of Normandy is a winner."


101: The Airborne Invasion of Normandy, Reception
Tim Carter of Computer Gaming World and Ian Marsh of Britain's PC Gaming World were critical of 101. Marsh argued that "the gameplay sucks", a complaint largely echoed by Carter: he wrote that the design "might be realistic, but it makes for a lousy game—especially with the incredible number of technical flaws that you are subjected to."


101FM
101 FM (callsign 4CBL) is a community radio station broadcasting from Logan City, Queensland. Regular transmissions started in November 1988 and continue up until the present day. The station's transmitter is situated at Springwood and its coverage area includes the Sunshine Coast and Gold Coast regions of eastern Queensland.


101FM, History
Radio Logan Incorporated was established in 1984 after Logan City Council advertised for interested persons to establish a community radio station. The push for a municipal radio station was spearheaded by then Division 10 Councillor Tom O'Neil and the Council Public Relations Department, with the reasoning that as Logan had reached "city" status, a local radio station was needed. The issue was debated at a public meeting, attended by a small group of Logan residents, that the council convened in 1984.


101FM, History
The purpose of creating Radio Logan Incorporated was to provide the Logan community with news, entertainment, music, current affairs and information on local events and issues affecting the lifestyle of the community of which it serves.


101FM, History
Within the first year of the organisation's establishment, council gave access to broadcast from the council premises at 4 Karrawatha Street, Springwood, where the water towers are situated, which happens to be the highest point in Logan City.


101FM, History
After two years and four test transmissions, Radio Logan Incorporated was granted its licence in September 1988 with the start of permanent transmission on 18 November 1988.


101FM, History
The first on-air announcer was David Jull, who, before entering politics, worked in commercial radio and television.


101FM, History
The station's first test transmission took place at the residence of J. Horrocks (101 FM technical director). Three further tests and initial permanent broadcasting were done from a demountable studio situated behind the water tower in Karrawatha Street, Springwood.


101FM, History
We stayed on this land for seven years; this site is where the transmitter is still situated (along with a number of others) on top of one of the water towers.


101FM, History
In 1992 the state government wanted to build a new police precinct, so did a deal with Logan City Council. Council would get the land and premises of the old police station, plus two other properties in return for another parcel of later further down the road on which to build the new police Station.


101FM, History
The deal was made, and as council knew how we were trying to find a more suitable place to relocate our studio to, offered us the use of the old police station at 8 Railway Parade, Logan Central. So once refurbishment was completed we moved in, in 1993.


101FM, History
The station's call sign is 4CBL which aligns it with the areas of primary service: the communities of Logan, Beenleigh and Beaudesert. However, its signal is heard south to the New South Wales border, north to the Sunshine Coast, east to the islands of Moreton Bay and West to the Toowoomba Ranges.


101P/Chernykh
101P/Chernykh is a periodic comet which was first discovered on August 19, 1977, by Nikolaj Stepanovich Chernykh.


101P/Chernykh
In 1991, 101P/Chernykh was observed to split. JPL concluded that the comet split in April 1991, when 3.3 AU from the Sun.


101P/Chernykh
The primary nucleus is 5.6 km (3.5 mi) in diameter and was last observed in 2020. Fragment B has not been observed since 1996.


101st (Northumbrian) Regiment Royal Artillery
101 (Northumbrian) Medium Regiment Royal Artillery is part of the Army Reserve and has sub units throughout Northumbria. It is equipped with M270 Multiple Launch Rocket System (MLRS).


101st (Northumbrian) Regiment Royal Artillery, History
The origins of the Regiment can be traced back to 1860 when Artillery Volunteer units were raised in the United Kingdom, as a result of threats of a French invasion. This continued through the formation of the Territorial Force in 1908, and the re-forming of the Territorial Army in 1947.


101st (Northumbrian) Regiment Royal Artillery, History
The Regiment was formed on the restructuring of the Territorial Army in April 1967. It was formed from 272 Field Regiment RA (Northumbrian) TA (formed in 1916, known as 72 Field Regiment until 1947 and based at the Barrack Road drill hall in Newcastle upon Tyne), 274 Field Regiment (Northumbrian) RA (TA) (formed in 1938, known as 74 Field Regiment until 1947 and based at South Shields), 324 Heavy Air Defence Regiment RA (TA) (raised in 1947 and based in Gosforth) and 439 Light Air Defence Regiment (formed in 1955 and based in Tynemouth).


101st (Northumbrian) Regiment Royal Artillery, History
The new regiment was equipped with BL 5.5-inch Medium Guns and had its headquarters at the Army Reserve centre at Barrack Road in Newcastle upon Tyne. In 1976, it was redesignated as a Field Regiment and re-equipped with the 105mm light gun. Around 1990, the regimental headquarters moved to Gateshead. In 2006, 269 (West Riding) Battery Royal Artillery was transferred from 106th (Yeomanry) Regiment Royal Artillery to this regiment.


101st (Northumbrian) Regiment Royal Artillery, History
Under Army 2020, its role is more specific. All batteries were re-roled to the M270 Multiple Launch Rocket System. It was paired with 39 Regiment until the end of March 2015, and with 3 RHA afterwards. It will also support 1 RHA, 19 and 26 RA.


101st (Northumbrian) Regiment Royal Artillery, Freedoms
The Regiment has received the Freedom of several locations throughout its history; these include:


101st Air Refueling Wing
The 101st Air Refueling Wing (101 ARW) is a unit of the Maine Air National Guard, stationed at Bangor Air National Guard Base, Bangor, Maine. If activated to federal service with the United States Air Force, the 101 ARW is operationally-gained by the Air Mobility Command (AMC).


101st Air Refueling Wing, Units
In the late 2010s the wing consists of the following major units:


101st Air Refueling Wing, History
The mission of the 101st FIW was the air defense of New England. Its assigned squadrons were dispersed and equipped as follows:


101st Air Refueling Wing, References, Bibliography
This article incorporates public domain material from the Air Force Historical Research Agency website .