On the topic of immigration, here comes a quote from veteran opinion journalist David Frum.

David is not Dissident Right. He's an old-line Buckleyite conservative who wouldn't be seen dead posting at VDARE.com or American Renaissance. He is, though, very smart and unusually honest for a guy at his pay scale; and he has for some years been traveling up a long slow learning curve on the immigration issue.

Well, in the current issue of Atlantic magazine David has a piece under the title, in the print edition of the magazine, "How Much Immigration is Too Much?" For reasons not known to me, the piece was posted online under a different title: "If Liberals Won't Enforce Borders, Fascists Will."

The piece expresses middle-of-the-road good sense on immigration, chewing thoughtfully over the economic and social factors. Nothing in it would strike a VDARE.com reader or a Radio Derb listener as controversial, other than for being too cucky and accommodating. For example, it falls far short of proposing an immigration moratorium, or even of bringing back the restricted, orderly, demographically conservative immigration system that our country was flourishing under sixty and seventy years ago.

And the piece is conventionally anti-Trump, speaking about the administration's good-faith efforts to enforce federal laws as, quote: "the gratuitous brutalities of the Trump administration." There is, in short, plenty of space between David Frum's position and ours.

This mild, carefully inoffensive approach notwithstanding, Frum has come in for some blistering attacks from the open-borders people. Thursday this week Frum published a follow-up piece on the Atlantic website answering back to some of those attacks.

I'll leave you to read that whole follow-up piece for yourself. It's titled: "Faith, Reason, and Immigration." I'm just going to pull out a quote that I think gets to the heart of the matter. Here's David Frum in this latter piece, quote, slightly edited:

The responses to my article express a sense of shock, offense, and outrage that you would not usually expect to see in a debate over public policy. The emotional intensity of the replies makes clear that for many of those reading my article, immigration on the largest feasible scale is a fundamental moral commitment. The arguments given in favor … are so wan that they invite the suspicion that the real arguments are not being articulated. What you're hearing is faith, not reason.

That's exactly right, and wearily familiar to those of us who work the immigration beat. Time and again, when trying to argue our case, we realize that we're up against not the other party's cerebral cortex, but against his limbic system—those parts of the brain that manage emotions, instincts, and moods.

I made the same point ten years ago in Chapter 10 of my intergalactic bestseller We Are Doomed, quotes from self:

Immigration is a difficult topic to discuss … The reason it is so difficult is that it has, more I think than any other aspect of U.S. policy, been moralized, in fact hyper-moralized …

According to this hyper-moralized point of view, [immigration] policy is an expression of America's Intrinsic Goodness and High Principle …

[But] immigration is just a policy, like farm supports, military recruitment, national parks maintenance, and income tax rates. Goodness, as the lady said, has nothing to do with it …

The whole topic, though, is soaked with moralizing and sentimentality. Immigration advocates have their eyes fixed firmly on the past—Ellis Island, Famine Ships. Yet population policy is really all about the future—not about indignities suffered by our grand-parents, but about the kind of nation our grand-children will live in.

I congratulate David Frum on learning what we here in the trenches found out long ago and have been voicing for a decade or two. Who knows?—perhaps, after another ten years' enlightenment, David may be writing for us here at VDARE.com.


Teenager Whose Car Hit Byron Girl is Also Suspect in Burglary

Byron, MN (KROC AM News) - The Rochester teenager who struck a young Byron girl Wednesday after she got off her school bus had been detained just before that as a suspect in a nearby burglary.

Olmsted County Sheriff’s Office Sgt. Kirby Long says the 17-year-old was interviewed about the Byron burglary by a deputy and then released. He was driving down 4th Ave NE near the 10th St intersection when the approaching bus stopped and let the 5-year-old girl off.

She was walking to her home and the driver of the bus could see the teenager was not going to stop, even though the stop sign was extended and the flashing lights were on. Long says the driver of the bus hit his horn but the teen still did not stop and the girl was struck by the side of his car, fell to the ground and one of her legs was run over by the driver’s side rear tire.

Long says the teen stopped and went to the girl’s house where he apologized to her mother and then drove away without leaving his name.

Long says as the teenager was driving away, his father contacted him about the burglary and told him to meet him at the house. A deputy was still there and eventually figured out the teen was the driver of the car that hit the girl.

Long says he expects the teen to face charges in the burglary and the hit-and-run. Long says the girl’s parents took her to St. Marys Hospital to be checked out and she was treated for bruises to her arms and legs.


Sen. Tammy Baldwin Tammy Suzanne BaldwinKeep teachers in the classroom Cher raised million for Biden campaign at LGBTQ-themed fundraiser Democrats seek balance in backing protests, condemning violence MORE (D-Wis.) trounced Republican Leah Vukmir in Wisconsin's Senate race on Tuesday, clearing her way to a second-term in the chamber.

Baldwin's win is welcome news for Democrats, who have touted their strength in Midwestern states that President Trump Donald John TrumpOmar fires back at Trump over rally remarks: 'This is my country' Pelosi: Trump hurrying to fill SCOTUS seat so he can repeal ObamaCare Trump mocks Biden appearance, mask use ahead of first debate MORE won in 2016, including Wisconsin.

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Throughout her general election campaign, Baldwin appeared well positioned to win another term in the Senate. She consistently led in public polls and outraised Vukmir, a state senator, by a wide margin.

But Vukmir also received help from the Republican Party's leader: President Trump himself. The president boosted Vukmir and Wisconsin Gov. Scott Walker during a rally late last month.

Still, Trump's approval rating in Wisconsin remains underwater. A Marquette Law School poll of Wisconsin voters released last month put the president's approval at 47 percent in the state, compared to 50 percent who said they disapprove of the job he's doing in office.

The Cook Political Report put the Wisconsin Senate race in the "Likely" Democratic column.


Brassica hilarionis

Brassica hilarionis is a hairless perennial up to 1 m high with a basal rosette of roundish, fleshy, flat-stalked leaves, upper leaves stalkless and stem-clasping. Has large loose racemes of creamy white flowers with petals up to 2.5 cm long. Narrow beaked pods up to 7 cm. Flowers from March to May.

Distribution
Endemic to the Northern Range from Yayla to Kornos in Northern Cyprus. Common name is Sent Hilarion Lahanası.

References

External links
 http://www.actaplantarum.org/floraitaliae/viewtopic.php?t=57281
 http://www.uni-goettingen.de/admin/bilder/pictures/0655f68d55bb6654329d762d680cfef9.jpg
 https://c2.staticflickr.com/6/5140/5489390104_e8bd80a1da.jpg
 http://www.natureofcyprus.org/detailInfoTur.aspx?cid=5&recid=207&recordid=207&pageindex=10&rowid=53&pagesize=5

hilarionis
Category:Endemic flora of Cyprus


Improving the Lives of Children and Families

Giving parents access to college admissions

Is the college admission process a family affair? Dalina Castellanos’ piece entitled “Help on the road to higher education,” suggests that it is. In this brief piece, Castellanos discusses a 3-year-old parent education program run by the nonprofit Partnership for Los Angeles Schools that is designed to provide low-income and immigrant parents with the knowledge and support necessary to lead their children through the complicated landscape of the college admission process and beyond. “Parent College,” as it is called, is described as “an unusual education effort” for such families that offers “several years” of Saturday workshops on such things as college admissions requirements, financial aid, and the particulars of college life, as well as campus tours and visits.As a developmental psychologist, I believe the movement to college to be a pivotal (yet certainly not inevitable) transition for youth in an increasingly globalized, technological world. On the one hand, I agree that such targeted outreach efforts and programs to assist parents who are not themselves college educated in supporting their youth in this endeavor have great merit; indeed, this transition is both embedded in and exerts an influence on the entire family system, not just the individual child. Further, on any occasion where one must enter unfamiliar territory, it is most often both prudent, helpful, and necessary if the requisite knowledge, behaviors, and “codes” for success in that context are explicitly pointed out and taught to those who do not possess them. For parents and families who are unfamiliar with the college experience, this program holds many potential benefits, and can be a valuable resource in the college access process for youth.

“Both the larger academic literature and my own research with immigrant families attests to the fact that immigrant parents care deeply about their children’s education, and in fact, often possess a more urgent focus on their children acquiring formal education as a way of improving their future opportunities than do native born families.”

However, I also believe that individuals leading programs such as the one featured here must consistently and honestly interrogate the assumptions that might surround their intentions to “help” (note that this is the first word in the article title), lest paternalistic assumptions of “who knows best” lead to strategies and solutions that are not actually grounded in the lived realities of the parents enrolled in the program. Rather, I argue here that for programs such as Parent College to be ecologically valid tools for educating and empowering the families of first-generation college students, they must avoid simplistic, scripted curricula that posit a set of “universal” behaviors, cultural beliefs, and attitudes that are more reflective of the middle and more affluent classes’ experience with the college transition. Instead, such programs must contain sufficient “open” space for parents to integrate necessary, new information into their own cultural, educational, and family circumstances in contextually relevant ways, as well as regular opportunities and time to discover areas of shared expertise on issues such as parenting, experiences with educational institutions, etc. In this way, these programs can realize their potential for supporting and guiding historically marginalized families through this important transition in ways that are authentic, sensitive, and respectful.

Parents and students from Parent College tour UC Irvine. Photo: Barbara Davidson, Los Angeles Times

One of the first misconceptions that the article addresses is that low-income and immigrant parents (who may or may not be from the same group) don’t care about their child’s education. The article features the story of Maria Martinez, an immigrant mother of Mexican descent who herself had no formal education, yet increasingly desires this for her youngest children as they grow up in the U.S. Both the larger academic literature and my own research with immigrant families attests to the fact that immigrant parents care deeply about their children’s education, and in fact, often possess a more urgent focus on their children acquiring formal education as a way of improving their future opportunities than do native born families. In the article here, Ms. Martinez notes that supporting higher education “is the only inheritance we can leave our children.” Interestingly, in my own work with a diverse group of Latino parents in the Boston area, a young mother who had recently immigrated from the Dominican Republic echoed this sentiment almost verbatim, noting that “for me, [formal] education is the inheritance that you give to your children” (see article in spring/summer 2013 edition of The School Community Journal ). Immigrant parents fervently want better for their children than they themselves had; while “better” is undoubtedly contextual, one of the ways it is often defined by recent immigrant parents is through formal education.

In the article, Ms. Martinez goes on to describe some of the particulars of the program, highlighting a common tension she often encounters with other Latino parents: their fears of “letting their child go to college.” This might be viewed as an example of how cultural strengths in one context can actually become weaknesses in another. As implied here and consistent with the literature, many Latino families (as well as other immigrant and/or low income families) operate within an interdependent framework that stresses physical and psychological closeness with family, familial obligation, and an orientation toward others- characteristics that are protective and promote resilience when resources are scarce, for example. The typical college experience is undoubtedly framed within an independent perspective- one that stresses individual separateness, self-reliance, and autonomy. This shift in orientation can be a riveting one for parents as they confront the college transition process, as Ms. Martinez notes.

Hence, the opportunity the program offers for parents to connect, talk, and learn from each on issues such as the above is compelling, and I believe this is one of the most powerful potential benefits of programs such as Parent College. If well designed, these programs can provide a space for parents and families to gain what sociologist James Coleman called social capital- collective benefits individuals accrue through their interactions and networks with others. Parents often use this capital in the service of their children, in areas where they might feel less efficacious. Again, my own research with a nationally representative sample of Latino families participating in the Early Childhood Longitudinal Study (see article in Hispanic Journal of Behavioral Sciences , 2011, Volume 33) evidences the relevance of parents’ social capital; in examining factors associated with parents’ physical presence in schools, the number of other parents from their child’s classroom that they reported they knew well enough to talk to was the strongest individual predictor of their school involvement, even after controlling for other factors such as formal education and income.

“If well designed, these programs can provide a space for parents and families to gain what sociologist James Coleman called social capital- collective benefits individuals accrue through their interactions and networks with others.”

Of course, I need not defer only to my professional, researcher self to ponder the relevance of a program like Parent College for parents and students alike. My own experience as a first-generation college student of working-class, Italian-American parents resonates with many of the experiences highlighted in the article. My parents knew nothing of the college admissions process- I mostly relied on myself and my teachers and guidance counselors. On campus tours with other prospective students and families, my parents remained wide-eyed and silent while other parents peppered our guides with what I thought to be perceptive questions (note: my mother is rarely silent and often dominates most conversations with both family and friends). And, I vividly remember the first time those interdependent “bonds” (also often characteristic of Italian families) felt too tight: as we settled into my dorm room, my mother commented, “oh well, anything you forgot you can get next weekend- because you’ll be coming home on the weekends anyway.” When I tentatively (and guiltily) suggested that no, I might not come home every weekend, I remember the panic that spread over my mom’s face- panic that she quickly tried to hide and overcome as she struggled not to burden me with her angst. I argue here that although these feelings might be characteristic of all parents in this situation, it may well be more acute for parents who are unfamiliar with the college experience.

As the article notes, these parents are themselves experiencing this new environment as a “strange, faraway land.” And, to add another layer of complexity, while the “land” my parents were leaving me in may have been “strange” in many respects, it was also predominantly white, as we were. Although ethnic minority enrollment in postsecondary institutions is historically high, they (ethnic minority students) are far from the majority on most college campuses in the U.S. How much more “strange” and “faraway” might this land be for a family who has lived for years in their own ethnic enclave? Thus, programs like Parent College can provide the space for ethnic minority parents to confront and process these fears, and to come to new understandings by sharing experiences, cultural resources, and strategies together.

So how do we design parent programs that are not fundamentally deficit-oriented, but effectively balance the acquisition of new information with the strengths, knowledge, and insights parents already have? A key part of the answer, I believe, lies with parents themselves, whose voices must be at the center of such programs. Although there is a plethora of new, perhaps “standardized” information that will obviously need to be shared with first-generation families embarking on the college transition, there should be ample space and time for the complexities of the experience as it exists in the lives of the participants to be teased out and addressed in contextually relevant ways. I offer a final, illustrative example. My stepdaughter will embark upon the college application process in the next few years. Although her transition to college and campus life will be an emotional upheaval for my husband and I, as upper-middle class, college-educated professionals we will have little difficulty conceptualizing this experience as “her time,” and will fully support her efforts to focus exclusively on her own experiences there. Would this stance be adaptive for the majority of families Parent College seeks to recruit? Indeed, it may be for some, as it appeared to be for Ms. Martinez, but research and my own experience as a Wheelock College professor suggest that many first-generation, immigrant, and/or students from low-income backgrounds simply cannot clearly separate the boundaries between college and home life. These students may have to continue to work or to maintain a physical presence and responsibilities in their homes and/or communities. Families who experience these situations can share ideas and strategies for supporting their children as they navigate these issues, and more. In my brief online research on Parent College, it does indeed seem to be a program where conversations like this can, and do happen, and that parents have a strong, legitimate presence. Similar programs should follow suit, so that “help” for parents embarking on the college transition isn’t simply delivered by “experts,” but offered and shared among and between parents themselves.

Tina Durand is an Associate Professor of Human Development at Wheelock College. She has worked in both rural and suburban public schools as a classroom teacher and Early Childhood Specialist. Her research interests regard ecological factors associated with the early adaptation and success of Latino children and families in schools, ethnic and class-based differences in parental involvement in children’s learning, and children living in poverty. She is also interested in cultural interpretations of human development, and issues of race and class in child and family studies.


---
abstract: |
    We perform a detailed study of the Earth matter effects on supernova neutrinos with neutrino oscillation parameter LMA and small $\theta_{13}$. The Earth effects show significant dependences on the neutrino path length inside the Earth and the value of $\Delta m^{2}_{12}$. We investigate rather optimistically a possibility that we can probe the value of $\Delta m^{2}_{12}$ by the Earth effects. We assume that $\theta_{12}$ and the direction of the supernova are known with enough accuracy and that the resonance that occurs at higher density in supernova envelope is completely nonadiabatic. Further the neutrino spectra before neutrinos go through the Earth are assumed to be known. Then we show that making use of these dependences, we can obtain implication for the value of $\Delta m^{2}_{12}$ by comparing the observed energy spectrum to the predicted one. When SK detects neutrinos from supernova at 10kpc which traveled through the Earth (nadir angle $<$ 80 degree), $\Delta m^{2}_{12}$ can be determined with an accuracy of $\sim 10\%$. In much of the neutrino-detection-time-$\Delta m^{2}_{12}$ plane, $\Delta m^{2}_{12}$ might be determined with an accuracy equal to or better than $\pm 0.5 \times 10^{-5} {\rm eV}^{2}$.

    $PACS:$ 14.60.Pq; 14.60.Lm; 96.40.Tv; 97.60.Bw;

    $Keywords:$ Neutrino oscillation; Supernovae; Earth effects;
author:
- |
    Keitaro Takahashi$^{\rm a}$ and Katsuhiko Sato$^{\rm a,b}$\
    [*$^{\rm a}$Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo,*]{}\
    [*Tokyo 113-0033, Japan*]{}\
    [*$^{\rm b}$Research Center for the Early Universe, University of Tokyo,*]{}\
    [*7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan*]{}
title: Earth effects on supernova neutrinos and their implications for neutrino parameters
---

Introduction
============

A type II supernova is a prodigious source of neutrinos. Almost all of the binding energy, $E_{b} \sim 10^{53}$erg, is radiated away as neutrinos. These neutrinos carry information about both the core collapse process and intrinsic properties of the neutrinos. In fact, the detection of the neutrino burst from SN1987A [@K2_SN1987A; @IMB_SN1987A] induced a number of studies on these areas [@Arafune; @Smirnov1987A; @Sato; @Goldman].

Neutrino oscillation, which is confirmed by the observations of solar and atmospheric neutrinos, can affect the energy spectrum of supernova neutrino drastically. Neutrinos of all flavors are produced in the high dense region of the iron core [@Totani] and interact with matter before emerging from the supernova. The presence of non-zero masses and mixing in vacuum among various neutrino flavors results in strong matter dependent effects, including conversion from one flavor to another. Hence, the observed neutrino flux in the detectors may be dramatically different for certain neutrino flavors and for certain values of mixing parameters, due to neutrino oscillation. Similar matter effect occurs in the Earth, too.

These oscillation effects on neutrino spectra depend strongly on neutrino oscillation parameters: mixing angles and mass spectrum. Some of them are firmly established but others are not. All the existing experimental results on the atmospheric neutrinos can be well described in terms of the $\nu_{\mu} \leftrightarrow \nu_{\tau}$ vacuum oscillation with mass squared difference and the mixing angle given by [@Fukuda], $$\Delta m^{2}_{\rm atm} \approx 7 \times 10^{-3} {\rm eV}^2 \; , \;
\sin^{2} 2 \theta \approx 1 .$$ In contrast, for the observed $\nu_{e}$ suppression of solar neutrinos four solutions are still possible [@Bahcall; @Krastev; @Garcia]: large mixing angle (LMA), small mixing angle (SMA), low $\Delta m^{2}$ (LOW), and vacuum oscillation (VO). $$\begin{aligned}
({\rm LMA}) \;\Delta m^{2}_{\odot} & \approx & (1 \sim 10) \times 10^{-5}  {\rm eV}^2 \; , \;
 \sin^{2} 2 \theta_{\odot} \approx 0.7 \sim 0.95 \\
({\rm SMA}) \;\Delta m^{2}_{\odot} & \approx & (4 \sim 10) \times 10^{-6}  {\rm eV}^2 \; , \;
 \sin^{2} 2 \theta_{\odot} \approx (2 \sim 10) \times 10^{-3} \\
({\rm LOW}) \;\Delta m^{2}_{\odot} & \approx & (0.5 \sim 2) \times 10^{-7}  {\rm eV}^2 \; , \;
 \sin^{2} 2 \theta_{\odot} \approx 0.9 \sim 1.0 \\
({\rm VO}) \;\Delta m^{2}_{\odot} & \approx & (0.6 \sim 6) \times 10^{-10}  {\rm eV}^2 \; , \;
 \sin^{2} 2 \theta_{\odot} \approx 0.8 \sim 1.0 \end{aligned}$$ For $\theta_{13}$, the mixing angle between mass eigenstate $\nu_{1}, \nu_{3}$, only upper bound has been known from reactor experiment [@CHOOZ] and combined three generation analysis [@Fogli; @Yasuda; @MinakataYasuda]. Also the nature of neutrino mass hierarchy (normal or inverted) is still a matter of controversy[@Minakata; @Barger].

Supernova is a completely different system from solar, atmospheric, accelerator, and reactor neutrinos in regard to neutrino energy and flavor of produced neutrinos, propagation length and so forth. Then neutrino emission from a supernova is expected to give valuable information that can not be obtained from neutrinos from other sources.

There have been some studies on the supernova neutrino as an oscillation parameter prober. Dighe and Smirnov [@Dighe] have studied the role the supernova neutrinos can play in the reconstruction of the neutrino mass spectrum. Dutta et al. [@Dutta] showed numerically that the events involving oxygen targets increase dramatically when there is neutrino mixing. We have shown in our previous work [@KT2] that the degeneracy of the solutions of the solar neutrino problem can be broken by the combination of the SK and SNO detections of a future Galactic supernova.

The Earth effects have also been studied by several authors. In our previous work [@KT1], we analyzed numerically the time-integrated energy spectra in a simple case and found the possibility to probe the mixing angle $\theta_{13}$. Lunardini and Smirnov [@SmirnovEarth] performed a study of the Earth effects taking the arrival directions of neutrinos into account and showed that studies of the Earth effects will select the solution of the solar neutrino problem, probe the mixing $U_{e3}$ and identify the hierarchy of the neutrino mass spectrum.

In this paper, we perform a detailed study of the Earth matter effects on supernova neutrinos and show that the detection of Earth matter effects allows us to probe $\Delta m^{2}_{12}$ more accurately than by solar neutrino observations.

Three-flavor formulation
========================

In the framework of three-flavor neutrino oscillation, the time evolution equation of the neutrino wave functions can be written as follows:

$$i\frac{d}{dt}\left(
    \begin{array}{ccc}\nu_e\\ \nu_{\mu}\\ \nu_{\tau}
    \end{array}\right)
= H(t)\left(
    \begin{array}{ccc}\nu_e\\ \nu_{\mu}\\ \nu_{\tau}
    \end{array}\right) \label{Schrodinger}$$

$$\begin{aligned}
H(t)  \equiv
U\left(
    \begin{array}{ccc}
        0 & 0 & 0\\
        0 & \Delta m^2_{21} /2E & 0\\
        0 & 0 & \Delta m^2_{31} /2E
    \end{array}\right)U^{-1}
    +\left(
    \begin{array}{ccc}
        A(t) & 0 & 0\\
        0 & 0 & 0\\
        0 & 0 & 0
    \end{array}\right),\end{aligned}$$

where $A(t)=\sqrt{2}G_{F}n_{e}(t)$, $G_{F}$ is Fermi constant, $n_{e}(t)$ is the electron number density, $\Delta m^2_{ij}$ is the mass squared differences, and $E$ is the neutrino energy. In case of antineutrino, the sign of $A(t)$ changes. Here U is a unitary 3 $\times$ 3 mixing matrix in vacuum: $$U  =  \left(\begin{array}{ccc}
c_{12}c_{13} & s_{12}c_{13} & s_{13}\\
-s_{12}c_{23}-c_{12}s_{23}s_{13} & c_{12}c_{23}-s_{12}s_{23}s_{13}
& s_{23}c_{13}\\
s_{12}s_{23}-c_{12}c_{23}s_{13} & -c_{12}s_{23}-s_{12}c_{23}s_{13}
& c_{23}c_{13}
\end{array}\right)\label{mixing_matrix},$$ where $s_{ij} = \sin{\theta_{ij}}, c_{ij} = \cos{\theta_{ij}}$ for $i,j=1,2,3 (i<j)$. We have here put the CP phase equal to zero in the CKM matrix.

In $H(t)$, the first term is the origin of vacuum oscillation, and the second term A(t), which is the only time-dependent term in H(t), is the origin of MSW effect.

Determination of neutrino oscillation parameters
================================================

In this section we summarize our previous studies on the effects of neutrino oscillation on supernova neutrino and show that future detection of neutrino from Galactic supernova allows us to break the degeneracy of the solutions of the solar neutrino problem and to probe $\theta_{13}$.

In [@KT2], three-flavor neutrino oscillation in the star is studied. We calculated the expected event rate and energy spectra, and their time evolution at the SuperKamiokande(SK) and the Sudbury Neutrino Observatory(SNO). For the calculations of them, we used a realistic neutrino burst model based on numerical simulations of supernova explosions [@Totani; @Wilson] and employed a realistic density profile based on a presupernova model [@Woosley]. The distance between the supernova and the Earth was set to 10kpc.

By solving numerically the differential equations (\[Schrodinger\]) from the center of supernova to the outside of supernova, we obtained conversion probabilities $P(\nu_{\alpha \rightarrow \beta})$, i.e., probabilities that a neutrino of flavor $\alpha$ produced at the center of supernova is observed as a neutrino of flavor $\beta$.

We assumed normal mass hierarchy and used four sets of mixing parameters shown in table \[table:parameter\]. Here $\theta_{12}$ and $\Delta m_{12}^{2}$ correspond to the solutions of solar neutrino problem and $\theta_{23}$ and $\Delta m_{13}^{2}$ correspond to the solution of atmospheric neutrino problem. The value of $\theta_{13}$ is taken to be consistent with current upper bound from reactor experiment [@CHOOZ]. These models are named after their values of mixing angle: LMA-L means that $\theta_{12}$ is set to be LMA of solar neutrino problem and $\theta_{13}$ is large.

We then found that when there is neutrino oscillation, neutrino spectra are harder than those in absence of neutrino oscillation. This is because average energies of $\nu_{e}$ and $\bar{\nu}_{e}$ are smaller than those of $\nu_{x}$(either of $\nu_{\mu}$, $\nu_{\tau}$, and their antineutrinos), and neutrino oscillation produces high energy $\nu_{e}$ and $\bar{\nu}_{e}$ which was originally $\nu_{x}$. This feature was used as a criterion of magnitude of neutrino oscillation. We calculated the following ratio of events at both detectors: $$R_{\rm SK} \equiv \frac{\makebox{number of events at } 30<E<70\rm{MeV}}
        {\makebox{number of events at } 5<E<20\rm{MeV}}$$ $$R_{\rm SNO} \equiv \frac{\makebox{number of events at } 25<E<70\rm{MeV}}
        {\makebox{number of events at } 5<E<20\rm{MeV}}$$ The plots of $R_{\rm SK}$ vs. $R_{\rm SNO}$ are shown in Fig.\[figure:ratio\]. The errorbars include only statistical errors. The difference among the following three groups is clear: (1)LMA-L and LMA-S, (2)SMA-L, and (3)SMA-S and no oscillation.

In [@KT1], the Earth effects on the energy spectra are studied using the result of [@KT2]. For mass squared differences in table \[table:parameter\], the supernova neutrinos arrive at Earth in mass eigenstates. This is because neutrino eigenstates with different masses lose coherence on the way from the supernova to the Earth. Since the eigenstates of Hamiltonian in matter differ from the mass eigenstates in vacuum, supernova neutrinos begin to oscillate again in the Earth. The numbers of neutrinos of each mass eigenstates at the surface of the Earth are determined by neutrino oscillation in the supernova [@KT1].

We analyzed numerically the time-integrated energy spectra of neutrino in a mantle-core-mantle step function model of the Earth’s matter density profile. We assumed that neutrino arrived at the detectors after traveling through the Earth along its diameter. We then found that the Earth matter affects the $\nu_{e}$ spectrum significantly in model LMA-S and $\bar{\nu}_{e}$ spectrum slightly in model LMA-S and LMA-L. In other models, there are no significant Earth effects. We concluded that we can differentiate LMA-L from LMA-S, by observing the Earth matter effect in $\nu_{e}$.

Thus we can distinguish all the four models in table \[table:parameter\]. But there are some ambiguities besides statistical errors. One is the mass of the progenitor star. Supernovae with different progenitor masses may result in different original neutrino spectra and neutrino oscillation effects. Studies on this point are now in progress. But dependence of shape of neutrino spectra on progenitor mass is not so large [@mass] and we would still be able to distinguish the models.

Supernova model which we use does not consider rotation of the progenitor star. In general, however, stars rotate through their lives and recent numerical simulation indicates that the rotation facilitate supernova explosion [@Shimizu]. Rotation of the progenitor star can affect its density profile and the dynamics of the neutrino oscillation in supernova.

Another ambiguity is the direction of supernova. The trajectories of neutrinos change according to the location of the supernova, the position of the detector and the time $t$ of the day at which the burst arrives at the Earth [@SmirnovEarth]. Fig \[figure:distance\] shows the dependence of the length $d$ of neutrino trajectory on the time $t$ for the three detectors, SK, SNO and LVD. $d$ is in unit of the diameter of the Earth. Neutrino trajectory can also be described by the nadir angle $\theta_{n}$ of the supernova with respect to the detector. In the next section, we perform a detailed study of the Earth matter effect.

Detailed study of the Earth matter effect
=========================================

In this section, we concentrate on model LMA-S and discuss the dependence of the Earth matter effect on the distance which neutrinos travel in the Earth and $\Delta m^{2}_{12}$. We consider three detectors: SK, SNO and LVD. But energy spectra at SK and LVD in model LMA-L are the same as in model LMA-S, since most of the events at SK and LVD are induced by $\bar{\nu}_{e}$s which are influenced by the Earth matter in both LMA-L and LMA-S. The dependence on $\Delta m^{2}_{12}$ is expected because the oscillation length in the Earth between mass eigenstates $\nu_{1}$ and $\nu_{2}$ is comparable $(\sim 1000 {\rm km})$ to the diameter of the Earth in LMA-S model [@KT1].

Here we use the realistic Earth density profile [@profile], while we used step-like model in our previous work [@KT1]. By solving (\[Schrodinger\]) along the Earth density profile numerically, we obtain conversion probability $P_{\nu_{i} \rightarrow
\nu_{\alpha}}$, i.e. probability that $i$th mass eigenstate at the surface of the Earth is detected as neutrino of flavor $\alpha$. Then combining these probabilities with the result of neutrino oscillation in supernova [@KT2], we obtain neutrino flux and at each detector.

neutrino events at SuperKamiokande
----------------------------------

SuperKamiokande (SK) is a water Cherenkov detector with 32,000 ton pure water based at Kamioka in Japan. The relevant interactions of neutrinos with water are as follows: $$\begin{aligned}
\bar{\nu_e} +p & \rightarrow & n + e^+ \quad(\rm{CC})
\label{interaction:anuep}\\
\nu_e + e^- & \rightarrow & \nu_e + e^- \quad(\rm{CC \quad and \quad NC})\\
\bar{\nu_e} + e^- & \rightarrow & \bar{\nu_e} + e^-
\quad(\rm{CC \quad and \quad NC})\\
\nu_x + e^- & \rightarrow & \nu_x + e^- \quad(\rm{NC})\\
\nu_e + {\rm O} & \rightarrow & {\rm F} + e^- \quad(\rm{CC})\\
\bar{\nu_e} + {\rm O} & \rightarrow & {\rm N} + e^+
\quad(\rm{CC})\label{interaction:nuebarO}\end{aligned}$$ where CC and NC stand for charged current and neutral current interactions, respectively. For the cross sections of these interactions, we refer to [@SKcross].

SK is not available now due to the unfortunate accident [@SKaccident] but is expected to be restored within the year. Since the number of PMTs will decrease to half the original, energy threshold and energy resolution will become worse. The detection efficiency is expected to be 90% at 8MeV[@SKefficiency]. In the above interactions, the $\bar{\nu_e}p$ CC interaction \[Eq.(\[interaction:anuep\])\] has the largest contribution to the detected events at SK. Hence the energy spectrum detected at SK (including all the reactions) is almost the same as the spectrum derived from the interaction Eq.(\[interaction:anuep\]) only.

neutrino events at SNO
----------------------

Sudbury Neutrino Observatory(SNO) is a water $\check{\rm{C}}$herenkov detector based at Sudbury, Ontario. SNO is unique in its use of 1000 tons of heavy water, by which both the charged-current and neutral-current interactions can be detected. The interactions of neutrinos with heavy water are as follows, $$\begin{aligned}
\nu_e + d & \rightarrow & p + p + e^-\quad(\rm{CC})\label{eq:SNO_CC_nue}\\
\bar{\nu_e} + d & \rightarrow & n + n + e^+\quad(\rm{CC})
    \label{eq:SNO_CC_anue}\\
\nu_x + d & \rightarrow & n + p + \nu_x\quad(\rm{NC})\\
\bar{\nu_x} + d & \rightarrow & n + p + \bar{\nu_x}\quad(\rm{NC})\end{aligned}$$ The two interactions written in Eqs.(\[eq:SNO\_CC\_nue\]) and (\[eq:SNO\_CC\_anue\]) are detected when electrons emit $\check{\rm{C}}$herenkov light. These reactions produce electrons and positrons whose energies sensitive to the neutrino energy, and hence the energy spectra of electrons and positrons give us the information on the original neutrino flux. In this work, we mainly take into account these two charged current interactions, since the number of neutral current events does not change by neutrino oscillation. For the cross sections, we refer to [@SNOcross]. The efficiency of detection is set to be one, because we have no information about it.

The SNO detector has also 7,000 tons of light water which can be used to detect neutrinos. This can be considered to be a miniature of SuperKamiokande (32,000 tons of light water). Then the number of events detected by light water at SNO is 7/32 of that at SuperKamiokande.

neutrino events at LVD
----------------------

The Large Volume Detector (LVD) in the Gran Sasso Underground Laboratory is a $\nu$ observatory mainly designed to study low energy neutrinos from gravitational stellar collapse. LVD consists of 2 kinds of detectors, namely: liquid scintillator, for a total mass of 1840 tons, and streamer tubes for a total surface of about $7000 {\rm m}^{2}$.

The bulk of events is due to the capture reaction: $$\bar{\nu}_{e} + p \rightarrow n + e^{+} \; \; \; \; \; \;
n + p \rightarrow d + \gamma_{2.2 {\rm MeV}}$$ Further, about $5\%$ of the events are due to neutral current interactions with ${}^{12}$C which deexcites emitting a 15.1 MeV $\gamma$. Moreover, $3\%$ of events are due to elastic scattering of all neutrino flavours on electrons, and less than $1\%$ to charged current interactions of $\nu_{e}$ and $\bar{\nu}_{e}$ with ${}^{12}$C nuclei. For the cross sections, we refer to [@LVDcross]. The appropriate detection efficiency curve is also taken into account [@SmirnovEarth].

nadir angle dependence of energy spectra
----------------------------------------

Fig.\[figure:SK\_angle\], \[figure:SNO\_angle\] and \[figure:LVD\_angle\] shows the nadir angle dependence of neutrino spectrum at SK, SNO and LVD, respectively. Neutrino oscillation parameters are set to the values in model LMA-S except $\Delta m^{2}_{12} = 2 \times 10^{-5} {\rm eV}^{2}$. Since the oscillation lengths are comparable to the radius of the Earth, the Earth effects are strongly dependent on the nadir angle.

$\Delta m^{2}_{12}$ dependence of energy spectra and determination of $\Delta m^{2}_{12}$
=========================================================================================

method
------

Fig.\[figure:SK\_mass\], \[figure:SNO\_mass\] and \[figure:LVD\_mass\] shows the $\Delta m^{2}_{12}$ dependence of energy spectrum at SK, SNO and LVD. Neutrino oscillation parameters are set to the values in model LMA-S except $\Delta m^{2}_{12}$. Nadir angle is set to 0 degree. The larger $\Delta m^{2}_{12}$ results in higher-frequency oscillation in the energy spectra with respect to the energy. This is because the neutrino oscillation length is proportional to the inverse of $\Delta m^{2}$.

As can be seen, there is significant dependence of the Earth effect on $\Delta m^{2}_{12}$. Making use of this dependence, we can probe $\Delta m^{2}_{12}$ by the observations of the supernova neutrino spectra more accurately than by the observations of solar neutrino, if neutrino oscillation parameters are as in model LMA-S.

We assume that the direction of the supernova is given by direct optical observations or by the experimental study of the neutrino scattering on electrons [@direction1; @direction2]. Other parameters of neutrino oscillation except $\Delta m^{2}_{12}$ are also assumed to be known with enough accuracy. But in fact, $\theta_{23}$ does not affect the Earth matter effects and $\theta_{13}$ affects only the magnitude of the Earth matter effects through the adiabaticity of the H-resonance in supernova envelope[@Dighe]. If $\sin^{2}{\theta_{13}} {\lower.5ex\hbox{$\; \buildrel < \over \sim \;$}}10^{-5}$, the H-resonance is completely nonadiabatic for broad range of $\Delta m_{13}^{2}$ and in this case the Earth matter effects do not depend on the value of $\theta_{13}$. So what we need with enough accuracy is $\theta_{12}$ only if we assume the H-resonance is completely nonadiabatic.

Comparing the observed neutrino spectra to the predicted spectra of various values of $\Delta m^{2}_{12}$, we can determine the value of $\Delta m^{2}_{12}$. We perform Monte Carlo simulation to obtain the expected observed spectra at each detector. Here we take statistical fluctuation in number of neutrino events and energy resolution of each detector into account. Energy spectra are then binned according to the energy resolution. For the value of the energy resolution, we refer to [@SmirnovEarth] but that of SK after restoration is expected to be $\sqrt{2}$ times as bad as before the accident[@SKefficiency]. The energy resolution of each detector is shown in Fig.\[figure:resolution\].

The simulated spectrum is compared to the predicted spectrum with a $\chi^{2}$ method. The definition of the reduced $\chi^{2}$, which is a function with respect to $\Delta m^{2}_{12}$, is, $$\chi^{2}(\Delta m^{2}_{12}) = \frac{1}{d} \mathop{\sum}^{d}_{i=1}
\frac{(N^{\rm sim}_{i}-N^{\rm pre}_{i}(\Delta m^{2}_{12}))^{2}}
{N^{\rm pre}_{i}(\Delta m^{2}_{12})},$$ where $d$ is the number of bins and $N^{\rm sim}_{i}$ and $N^{\rm pre}_{i}(\Delta m^{2}_{12})$ are the simulated and predicted number of events in $i$th bin, respectively. The $\Delta m^{2}_{12}$ with the least $\chi^{2}(\Delta m^{2}_{12})$ is considered to be the value determined by this method.

representative results
----------------------

We make 1000 “supernovae” and “observe” the neutrino spectra assuming that the true value of $\Delta m^{2}_{12}$ is $4 \times 10^{-5} {\rm eV}^{2}$. Fig.\[figure:representative\] show the representative results of $\Delta m^{2}_{12}$ determination by the method described above. These are relative frequencies that the observed spectrum is identified with the theoretical spectrum with the various values of $\Delta m^{2}_{12}$. The nadir angle is set to be 0 degree at each detector and the $\chi^{2}$ method is performed with the data of each detector only.

As can be seen, if the supernova occur at the direction which the nadir angle is 0 degree at SK or SNO, $\Delta m^{2}_{12}$ can be determined with a high accuracy $(4.00 \pm 0.07) \times 10^{-5}
{\rm eV}^{2}$ or $(4.00 \pm 0.20) \times 10^{-5} {\rm eV}^{2}$ in case of SK and SNO, respectively. However, in case of LVD, it is difficult to determine $\Delta m^{2}_{12}$. The difference in the accuracy of determination of $\Delta m^{2}_{12}$ is due to the difference in the properties of the detectors. Here the properties of the detectors mean the energy resolution, the detectability of $\nu_{e}$ and the number of events.

Since the Earth effects are large in $\nu_{e}$ channel and relatively small in $\bar{\nu}_{e}$ channel, SK and LVD, at which most of events are $\bar{\nu}_{e}$, are disadvantageous. But the statistical error is very small at SK due to the large event number, $\sim 10000$ (10 kpc), and SK is the most efficient to identify the Earth effects. SNO is also efficient due to its high energy-resolution and detectability of $\nu_{e}$ although the number of events is small. Then LVD is not favorable for detecting the Earth effects. The properties of the detectors are summarized in the Table \[table:detector\].

It should be noted that the effectiveness of determining $\Delta m^{2}_{12}$ depend on the value of $\Delta m^{2}_{12}$ itself and nadir angle. These dependences are discussed in the following subsection.

determination of $\Delta m^{2}_{12}$
------------------------------------

Fig.\[figure:SNO\_best\_mass\] shows the relative frequencies at SNO that the simulated spectrum based on the theoretical spectrum with $\Delta m^{2}_{12} = 2 {\rm (solid)}, 4 {\rm (dashed)}, 6 {\rm (long-dashed)}
\times 10^{-5} {\rm eV}^{2}$ is identified with the theoretical spectrum with the various values of $\Delta m^{2}_{12}$. The nadir angle is set to be 0 degree. When $\Delta m^{2}_{12}$ is large, the oscillation in energy spectrum becomes rapid and then statistical errors make it difficult to identify the Earth effect and determine $\Delta m^{2}_{12}$. However at SK, its large number of events allows us to determine $\Delta m^{2}_{12}$ rather accurately irrespective of the true value of $\Delta m^{2}_{12}$ (Fig.\[figure:SK\_best\_mass\]).

Fig.\[figure:SNO\_best\_angle\] shows the relative frequencies at SNO at various nadir angles: 15 (solid), 80 (dashed) and 85 (long-dashed). The value of $\Delta m^{2}_{12}$ is set to be $4 \times 10^{-5} {\rm eV}^{2}$. Since the oscillation length of 60 MeV $\nu$ in Earth matter is $\sim 6000$km [@KT1], the Earth effects do not appear unless nadir angle is smaller than $\sim 80$ degree.

Now we consider the problem, ’How accurately can we determine $\Delta m^{2}_{12}$ when the true value of $\Delta m^{2}_{12}$ and the arrival time of neutrinos are given?’

As is discussed above, when the nadir angle at SK is smaller than 80 degree (time $= 0 \sim 8$ and $19 \sim 24$ hour), the value of $\Delta m^{2}_{12}$ can be determined accurately using only the SK data irrespective of the value of $\Delta m^{2}_{12}$ in the allowed region of the solar neutrino problem. When the nadir angle is smaller than 80 degree at SNO and greater than 80 degree at SK (time $= 10 \sim 19$ hour), the value of $\Delta m^{2}_{12}$ can be determined accurately using only the SNO data if the true value of $\Delta m^{2}_{12}$ is smaller than $\sim 4 \times 10^{-5} {\rm eV}^{2}$. However, if $\Delta m^{2}_{12} > 4 \times 10^{-5} {\rm eV}^{2}$, the single data of SNO is not sufficient. We performed then a $\chi^{2}$ method combining data of various detectors for time $= 8 \sim 19$ hour.

Fig.\[figure:contour\] is the contour map of the probability that the value $\Delta m^{2}_{12}$ can be determined with an accuracy equal to or better than $\pm 0.5 \times 10^{-5} {\rm eV}^{2}$. The probability is more than 0.7 for three fifths of the time-$\Delta m^{2}_{12}$ plane.

Discussion and conclusion
=========================

In this paper, we performed a detailed study of the Earth matter effects on supernova neutrinos with neutrino oscillation parameter LMA and small $\theta_{13}$. We showed that we can probe $\Delta m^{2}_{12}$ accurately by comparing the observed energy spectra to the predicted one. In much of the time-$\Delta m^{2}_{12}$ plane, $\Delta m^{2}_{12}$ can be determined with an accuracy equal to or better than $\pm 0.5 \times 10^{-5} {\rm eV}^{2}$. When SK detect neutrinos from supernova at 10kpc which traveled through the Earth (nadir angle $<$ 80 degree), $\Delta m^{2}_{12}$ can be determined with an accuracy of $\sim 10\%$. This accuracy is amazing compared to that from current solar neutrino experiments, which determine only the order of $\Delta m^{2}_{12}$. But as we stated before, $\theta_{12}$ and the direction of the supernova need to be known with enough accuracy. How much our results are affected by the uncertainties of the other parameters will be our future work.

$\Delta m^{2}_{12}$ can also be probed by KamLAND experiment[@KamLAND]. If the solution of solar neutrino problem is LMA, $\Delta m^{2}_{12}$ is expected to be known by three-year data-taking as precisely as by supernova neutrino discussed above. There is some possibility that we can know it from a Galactic supernova before the completion of the KamLAND experiment. Even if the results of KamLAND experiment is earlier than future galactic supernova, it is important to cross-check the results of ground-based experiments by astrophysical observations. Furthermore, it is meaningful itself to notice that we can obtain implication for $\Delta m^{2}$ from supernova neutrino.

We assumed in this paper that the neutrino spectra at the surface of the Earth were given. But since the original fluxes based on the numerical supernova model have some ambiguities, the sensitivity to $\Delta m_{12}^{2}$ might be worse than our estimation. Estimation of uncertainties of the numerical supernova model is hard because there is currently no successful simulation other than that by the Lawrence Livermore group [@Wilson]. There are, however, some studies about the temperatures of the produced neutrinos. According to them, they are typically[@Janka], $$\langle E_{\nu_{e}} \rangle = 10 - 12 {\rm MeV}, \;\;
\langle E_{\bar{\nu}_{e}} \rangle = 14 - 17 {\rm MeV}, \;\;
\langle E_{\nu_{x}} \rangle = 24 - 27 {\rm MeV}.$$ On the other hand, in the model that we used, they are $$\langle E_{\nu_{e}} \rangle \sim 13 {\rm MeV}, \;\;
\langle E_{\bar{\nu}_{e}} \rangle \sim 16 {\rm MeV}, \;\;
\langle E_{\nu_{x}} \rangle \sim 23 {\rm MeV}, \;\;$$ although the spectra are not exactly the Fermi-Dirac distribution[@Totani]. These values seem close to the typical values and the analysis taking these uncertainties into account will be performed in our future work.

Furthermore, supernova neutrino spectra depend on the mass of the progenitor star. However, we will be able to reconstruct the neutrino fluxes at the surface of the Earth from the data from the detector which detect the neutrinos directly from the supernova. Although the statistical errors then become larger and the accuracy of the determination of $\Delta m^{2}_{12}$ becomes worse, the Earth effects on the supernova neutrinos will still give valuable information which cannot be obtained from the other neutrino sources.

Acknowledgments
===============

We would like to thank A.Suzuki for advice on cross sections of neutrino interaction in scintillator experiment. We also thank Super Kamiokande people including Y. Totsuka, Y. Suzuki, T.Kajita, M. Nakahata and Y. Fukuda for showing the most recent SK data, and fruitful discussion. This work was supported in part by Grants-in-Aid for Scientific Research provided by the Ministry of Education, Science and Culture of Japan through Research Grant No.07CE2002.

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   model   $\sin^{2} 2 \theta_{12}$   $\sin^{2} 2 \theta_{23}$   $\sin^{2} 2 \theta_{13}$   $\Delta m_{12}^{2}({\rm eV}^{2})$   $\Delta m_{13}^{2}({\rm eV}^{2})$   $\nu_{\odot}$ problem
  ------- -------------------------- -------------------------- -------------------------- ----------------------------------- ----------------------------------- -----------------------
   LMA-L             0.87                       1.0                       0.043                   $7.0 \times 10^{-5}$                $3.2 \times 10^{-3}$                   LMA
   LMA-S             0.87                       1.0                $1.0 \times 10^{-6}$           $7.0 \times 10^{-5}$                $3.2 \times 10^{-3}$                   LMA
   SMA-L     $5.0 \times 10^{-3}$               1.0                       0.043                   $6.0 \times 10^{-6}$                $3.2 \times 10^{-3}$                   SMA
   SMA-S     $5.0 \times 10^{-3}$               1.0                $1.0 \times 10^{-6}$           $6.0 \times 10^{-6}$                $3.2 \times 10^{-3}$                   SMA

             detector                        SNO                    SK                LVD
  ------------------------------ --------------------------- ----------------- -----------------
            main event            ${\nu}_{e},\bar{\nu}_{e}$   $\bar{\nu}_{e}$   $\bar{\nu}_{e}$
   number of events (10[kpc]{})              300                   10000              800
        energy resolution                 $<$ 3 MeV              $<$ 6 MeV         $<$ 7 MeV


Tuesday, October 20, 2015

Formula E Season Two Guide: The Cars

This season, Formula E takes it's first steps away from being a one-spec series, and gives the teams their first opportunities to succeed through technological developments. As part of our Formula E season two guide, we take you through the vehicular changes for season two and what effect they're likely to have on the running order this season.

So, what's changed for season two?

The aim of the series was to gradually, season-by-season, allow the teams develop their own technologies. Eight manufacturers have now been permitted to design their own powertrains, which include the e-motor, the gearbox, the inverter and the cooling system.

Wait, aren't there ten teams?

Yes, the teams who submitted applications to create their own powertrains are:

ABT Sportsline

Andretti

Mahindra

Motomatica (Trulli)

NEXTEV TCR

Renault Sport

Venturi Automobiles

Virgin Racing Engineering

This means that Team Aguri and Dragon Racing won't be developing their own powertrains this season. Team Aguri will continue to use McLaren's season one powertrain, and Dragon Racing will be buying from Venturi.

Dragon Racing.Picture: Octane Photographic Ltd.

So, will Team Aguri and Dragon Racing be at a disadvantage this season?

If the Venturi package is competitive, then Dragon Racing should be competitive. They were believed to have been talking to a couple of manufacturers about season two powertrains, so they were in a position to pick what they thought was the best solution.

Team Aguri's decision to run a season one powertrain is the bigger risk. They've been put off by the development costs, but are confident that they can have some success with continuity and reliability, which could be the case in the first half of the season, but as teams perfect their cars, that advantage may be quickly reduced.

How have the cars changed then?

The main gains will be on the grounds of efficiency and minimising the energy losses between the battery and the wheels. The interesting thing is how the teams have gone in different directions to achieve this. The season one units had five gears, but some teams have gone down to four gears, three gears and even one gear (or 'direct drive').

NEXTEV TCR confirmed long ago that they'll be running a 'dual motor' layout, too. Which is also on the grounds of efficiency and being able manipulate the power exactly how they want to. DS Virgin Racing are believed to be doing the same thing and it was thought the Renault e.Dams team were going to follow suit, but elected for a single motor.

Mahindra RacingPicture: Octane Photographic Ltd.

So, what's the best solution?

Nobody knows yet! In the first season of opening up the powertrains rules, everybody has different ideas about which way to go. Does having multiple gears give better performance refinement? Or are there bigger gains to made in minimising the losses through a 'direct drive' system? Maybe we'll have some tracks which suit one powertrain layout, and other tracks which are ideal for other configurations.

Who's looked good in testing?

The Abt, Renault e.Dams, and DS Virgin Racing teams have all taken turns at topping the pre-season test timesheets, with Venturi, Dragon Racing and Mahindra often mixing it in the top five. As is the case with all motorsport test sessions, it's hard to know which teams are completely holding back, but it's easier to see which teams are having dramas.

Andretti had so many problems with their season two challenger, that they decided to revert back to the season one powertrain, meaning their first problem-free test day was only on the final day. Trulli, who are running the Motomatica powertrain, have also struggled to get going, but are persisting with it regardless. The team of the reigning world champion, Nelson Piquet, are also having reliability issues with this season's NEXTEV TCR car, but after a slow start, they look to be getting to grips and were managing decent mileage by the end of the test, even if they weren't making any headline times.

So are the cars faster this year?

They are. The previous best lap time at Donington Park was beaten by over a second, and people are expecting bigger gains on the street circuits for which the Formula E cars are designed.

Amlin Andretti's Simona de Silvestro being towed back to the garage.Picture: Octane Photographic Ltd.

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The plasma membrane protein Rch1 and the Golgi/ER calcium pump Pmr1 have an additive effect on filamentation in Candida albicans.
Pmr1 is the Golgi/ER calcium pump, while Rch1 is a newly identified negative regulator of calcium influx in the plasma membrane of yeast cells. We show here that CaRch1 plays a dominant role over CaPmr1 in response of Candida albicans to SDS and tunicamycin stresses, while CaPmr1 has a major role in cell wall stress. Deletion of CaRCH1 increases the calcium/calcineurin signaling level in cells lacking CaPMR1. Calcineurin function is required for the role of CaRch1 in SDS stresses, while it is required for the function of CaPmr1 under all conditions examined. Disruption of CaRCH1 alone does not reduce the cell wall chitin, mannan or β-glucan content, but lack of CaRCH1 slightly decreases the chitin content of cells lacking CaPMR1. Furthermore, CaRch1 and CaPmr1 have an additive effect on filamentation of C. albicans cells in vitro. Cells lacking both CaRCH1 and CaPMR1 and cells lacking CaPMR1 alone show a similar degree of virulence attenuation, being much more attenuated than cells lacking CaRCH1 alone. Therefore, CaRch1 genetically interacts with CaPmr1 in the regulation of in vitro filamentation in C. albicans.


Ask HN: How do I choose the right set of tools for web app development? - zazibar
I have an idea for a side project that is essentially a web app but I'm struggling to find the right tools for the job.
The number of frameworks/libraries for web app development is quite overwhelming and it's difficult to determine which one I should be using.
Should I go the "pure" route with React and its related libraries (Redux, etc.)? Should I use something that tries to provide everything out of the box like Ember or Vue? Ditch it all and just roll vanilla JS? I could go on but my point is that I honestly don't know which of these is right.
For context the web app I want to build is essentially a chat app at the core. I already know what I'll be building the backend with (Phoenix/Elixir) but the frontend remains a mystery for now.
Any insight on the issue would be appreciated.
======
onion2k
At the beginning of a project building _something_ is far more important than
building _the right thing_. If you wait until you've figured out the perfect
framework to build with you'll have wasted a lot of time and you'll probably
find you're wrong anyway as you discover things along the journey to Version
1.0.

Just build something.

------
quaunaut
Just as a bit of knowledge: The current Phoenix channels implementation should
work alright with React, but you'll have to work it into what you're wanting
to do.

In a few months, an Ember addon should be available that provides Phoenix
support, built by Chris McCord himself!


In the field of medical technology, image output devices are used to display for a user volume data images, particularly slice images, derived from volume data of a target tissue region. By way of example, such volume data can be obtained with the aid of tomography devices, such as computed tomography scanners, magnetic resonance imaging scanners, or else other imaging devices such as ultrasound installations. There are different display modes for such volume data images obtained from volume data. For example, they show different slice or sectional perspectives of the imaged tissue region in different projections or display depths. These include the multiplanar reconstruction (MPR) and the maximum intensity projection (MIP). The multiplanar reconstruction is a sectional imaging method in which the hollow organ is placed into a plane in a virtual fashion and shown with depth resolution in a virtually three-dimensional fashion. By contrast, the maximum intensity projection is a sectional imaging method in which sections of a tissue region, situated one behind the other or one above the other, are illustrated in a two-dimensional fashion. In the process, superimposed structures are illustrated together and a contrast is formed where that part of the tissue volume which causes the greatest measurement intensity in the imaging measurement produces the highest degree of coloring in the projection illustration. Like a back projection onto a focusing screen, structures positioned behind one another can in this fashion be illustrated in a plane.
An important field of application which uses volume data images generated by the abovementioned imaging devices is the diagnosis of hollow organs or hollow organ sections, e.g. vessels, in particular coronary vessels on the heart or vessels in the brain, or other tubular hollow organs such as the colon or the bronchi. In particular, a problem in diagnosing such structures lies in the fact that lesions can usually be found in edges of the hollow structure or in the walls of the hollow organ. A typical example of such a lesion is a stenotic region in a vessel section.
These days, such hollow organ sections are usually diagnosed using a pre-calculated profile line through the hollow organ. In the following text, a “profile line” is a line which follows the profile of the observed hollow organ. This generally is a central line running right through the middle of the hollow organ, the so-called “centerline”. The literature already discloses different relevant methods for pre-calculating such centerlines. Likewise, within the scope of computer aided diagnosis methods, there already are different methods for automatically selecting slice planes through the hollow organ such that possible lesions are illustrated in the view suitable for a post-evaluation. Thus, EP 0 961 993 B1 (=WO 98/37517) describes a method in which regions of an intestine with an abnormal wall thickness are automatically recognized as possible lesions and are then visualized in a particularly marked fashion in a wire model. In the process, slices are also generated along the profile line such that the lesions are clearly identifiable. U.S. Pat. No. 6,643,533 B2 suggests placing slice images along the profile plane through a blood vessel such that in a narrowing the smallest diameter of the blood vessel lies in the slice plane, i.e. the slice plane is selected such that the slice image shows the smallest lumen dimension. In the case of dilation, the slice image can be placed along the profile plane such that the largest diameter of the blood vessel is situated in the slice plane.
During the conventional diagnosis by an expert at an image output device, this centerline is used as a path for a virtual movement through the hollow organ section. Depending on the type of profile line or centerline calculation, this can consist of a number of individual points aligned next to one another, or else it can be constructed as a continuous line or a polygonal chain. During a virtual movement through the hollow organ along the centerline, different slice images can then be displayed on a diagnosis workstation at different observation points which can, for example, be the individual points from which the “centerline” is composed or, in the case of a continuous “centerline”, points at a certain step-size and can be observed by the user.
A typical screen surface for such diagnosis is illustrated in FIG. 1. On the left-hand side there is an image display field BF in which four different illustrations of the hollow organ section HO of interest, in this case the right coronary artery, are illustrated. To the right thereof there is a parameter display bar PL, acting as a user interface, on which the observer can adjust certain parameters with the aid of mouse clicks. In this case, a three-dimensional volume image VR of the heart, in which the relevant coronary artery is clearly visible, is displayed at the bottom on the right-hand side of the image display field BF. To the left thereof an orthogonal slice OS is shown at a certain point on the “centerline” along the coronary artery (the “centerline” itself is not illustrated in this case). The two upper images show two tangential slice images TS1, TS2. The orthogonal slice plane and the tangential slice planes are selected such that they respectively are mutually perpendicular. Here, the orthogonal slice plane is situated perpendicular to the profile line at a given point on the profile line and the tangential slice planes correspond to longitudinal slices along the hollow organ section and can be tangent to the profile line at e.g. this point, or can comprise this point. When moving along the “centerline” from one observation point to the next, a new orthogonal slice, which is perpendicular to the “centerline” at the respective observation point, and the two tangential slice images TS1, TS2 perpendicular thereto are illustrated at all observation points. By moving forward and backward along the “centerline”, for example by operating virtual pushbuttons on the parameter display bar with the aid of the mouse pointer, the complete hollow organ section can be successively observed within the scope of this profile display.
However, the problem with such a conventional procedure is that there are very big jumps in the tangential planes, particularly in the case of strongly curved structures and/or in the case of structures with frequent changes in curvature. When passing through the structure along the profile line, this leads to a bumpy, very vigorously “shaking” display of the tangential slice images. This harbors the risk of the observer easily losing the focus and the orientation in the image. This can lead to relevant structural changes being overlooked.


Arsenal are set to play in front of their lowest-ever attendance for a Premier League fixture against West Bromwich Albion on Thursday night.

Approximately 2,500 tickets were offered to club members while a few hundred more were placed on general sale but, due to a lack of interest, many have remained unsold.

A number of season ticket holders are also expected to stay at home after Sky Sports’ request to move the game to a Thursday night was granted.

The Gunners’ poor form is thought to be one of the reasons behind the slow uptake in sales, as Arsene Wenger’s side lie fourth in the table, unsure of a place in next season’s Champions League.

As many as 20,000 seats could be empty, according to Arsenal Supporters Trust’s Tim Payton, who told The Times that the club will face an “apathy boycott” on Thursday.

Arsenal, like most clubs, base attendance figures on the number of tickets sold rather than the number of people in attendance. The official figure will therefore include season ticket holders, whether they are at the game or not.


Ferris Wheel Spotted from a Crow’s Nest

Only dream
on the last night
in each bed, a dream
of shipping crates,
lifted and sat down by
the hand of a crane
I feel the difference
between winning and
not winning
a prize for you
in these moments
when life is contained
There’s a fair
you wanted
to go to. To be fair
I always assumed
we would go
It magically appeared
on the side
of I-35, opening
like a way home
once it is remembered
There are lights
when some people
can’t see lights
Lights in the carnival
Lights in the compromise
I always thought
it was light
that let you lie to our
guests about
the door I broke
The type of light
that spins, stopping
momentarily
at the top, then
tipping over


/*
 * Licensed to the Apache Software Foundation (ASF) under one
 * or more contributor license agreements.  See the NOTICE file
 * distributed with this work for additional information
 * regarding copyright ownership.  The ASF licenses this file
 * to you under the Apache License, Version 2.0 (the
 * "License"); you may not use this file except in compliance
 * with the License.  You may obtain a copy of the License at
 *
 *  http://www.apache.org/licenses/LICENSE-2.0
 *
 * Unless required by applicable law or agreed to in writing,
 * software distributed under the License is distributed on an
 * "AS IS" BASIS, WITHOUT WARRANTIES OR CONDITIONS OF ANY
 * KIND, either express or implied.  See the License for the
 * specific language governing permissions and limitations
 * under the License.
 */
package org.apache.struts2.convention.actions.result;

import org.apache.struts2.convention.annotation.ParentPackage;

/**
 * Used to test that <global-results> in struts.xml are are overridden when a matching result location can be
 * found.  For example, action-error.jsp overrides a global "error" result.
 *
 * @author Mark Woon
 */
@ParentPackage("class-level")
public class GlobalResultOverrideAction {

    public String execute() {
        return "error";
    }
}


North Korea’s leader Kim Jong Un has issued orders to drive out foreign-made products from markets in the country and prohibit the import of others that the isolated nation can manufacture, sources inside the country said.

The directive followed on the heels of earlier calls by Kim Jong Un in January and May for North Koreans to use only domestic products.

“As the rumor spreads that the North Korean government will crack down on all foreign-made products in the local markets after local election for delegates, people making a living from trade have become very worried about it,” a source in Chagang province, who declined to be identified, told RFA’s Korean Service.

Elections to provincial, municipal, city, county and district people's assemblies are scheduled to be held on July 19 — the first such voting since Kim Jong Un took power in late 2011, the state-run Korean Central News Agency announced last week. North Korean elections offer only one candidate on the ballot.

Security officers and custodians in charge of markets have been checking how many domestic and foreign-made goods — especially daily necessities — are being sold, adding to merchants’ anxiety, the source said.

An official in North Hamgyong province told RFA that North Korea has cracked down on Chinese products because it intends to drive them out of the country, but has left the customs clearance of such items alone to avoid a conflict with its neighbor that could turn into tariff action.

“I was told by North Korea’s central authorities not to stop travelers from bringing in products from China through customs, but to strictly prohibit the sales of the products in the market.”

North Korea is manufacturing many light industry products such as confectionery, cooking oil, medical supplies and clothes using raw material from China, he said.

Yet, the prices for these North Korean products, which are clearly marked as being made in the country, are much higher than those of similar ones manufactured in China, he said.

Sources inside North Korea also said Kim Jong Un’s instructions to drive out foreign-made goods meant eliminating private business because the government’s intention is to collect all money which is now circulating in the market.

North Korea has intensified its crackdown on foreign-made products since last November when Kim Jong Un declared at a cabinet meeting that the “preference for imports could lead to national ruin.”

A couple months later during his New Year’s speech, Kim Jong Un encouraged all citizens to use domestic products, saying that it was the “best form of patriotism to love and use our products.”

But a slogan publicized during the North Korean’s ruling Workers’ Party meeting on February 10 best summed up the leader’s goal in eliminating foreign goods from the country: “By getting rid of a preference for imports and localizing raw materials and facilities, our Workers’ Party is determined to create the best civilization that will be the envy of the world!”

Reported by Sung-hui Moon for RFA’s Korean Service. Translated by Yunju Kim. Written in English by Roseanne Gerin.


In multiple attacks two days ahead of the Prime Minister's visit to Jammu and Kashmir, militants stormed an Army camp in Uri in Baramulla district, killing 11 security personnel, including a Lt Col, and targeted a police party in Shopian while a top LeT commander was killed in an encounter.

In a daring pre-dawn attack ahead of third phase of elections in Jammu and Kashmir on December 9, heavily armed militants killed 8 Army men and three policemen around 3.10 AM at the camp in Mohra in Uri tehsil of north Kashmir's Baramulla district.

Six militants were also killed in the attack at the Army camp which is 20 km from the Line of Control (LoC), official sources said.

A Lt Colonel and seven Army personnel were among the dead. While bodies of four army personnel were charred, one had burn injuries and the other three had bullet injuries, the sources said.

In Delhi, Defence Minister Manohar Parrikar said, "We have killed three of them (militants) and we will eliminate the remaining.The ones who are left are trapped." "It is possible that this has happened because of elections," he said.

In Soura in the outskirts of the city, top Lashkar-e- Taiba commander Qari Israr was killed by security personnel when he was trying to enter the city, police said.

Encounter breaks out in Soura area of Srinagar. One militant has been killed and the firing between the police and militants is still underway.

'Militant attack on army desperate attempt to disrupt peace', says Jammu and Kashmir CM Omar Abdullah

Jammu and Kashmir Chief Minister Omar Abdullah today said the attack on the army camp in Uri area of Baramulla district was a "desperate attempt" to disrupt peace and normalcy. "Once again shows the desperate levels militants will go to disrupt peace and normalcy," Omar wrote on micro-blogging site twitter.

Militants have struck an army camp in North Kashmir between Baramulla and Uri. Security force casualties are feared. It's an ongoing encounter

On December 2, Army foiled an infiltration bid in Handwara area of Kupwara district killing six militants while one army personnel was also killed. The infiltration bid was foiled even as people in Kupwara district were voting to elect their representatives

Prime Minister Narendra Modi is slated to campaign in Srinagar and Samba on December 8 for third phase of the five-stage assembly elections in Jammu and Kashmir.


Q:

Can we change Earth's orbit with modern technology?

It is well known that, according to Newton's 3rd law, spacecrafts entering or leaving Earth provoke tiny (insignificant) changes to Earth's orbit (see related question here).
My question is about significant changes. For instance, say we would like to shift the Earth's orbit closer to that of Mars (forget about the ecological consequences of this). Do we currently have the technology capable of doing this? For instance, something like a huge nuclear explosion? This question only deals with "natural", non-human ways to change a planet's orbit. I am interested about technology-based changes.

A:

No, we cannot.
It's relatively simple math to show that we are a very long shot from changing Earth's orbit by anything significant at all: consider the kinetic energy of Earth in its current orbit, and do the same math for that in the desired orbit:
$ E_{kin} = \frac{m_E}{2}v^2 \approx \frac{m_E}{2}\frac{GM_S}{a}$
where $m_E = 6\cdot 10^{24}$kg is Earth's mass, $M_S=2\cdot 10^{30}$kg is the solar mass and $a=150\cdot 10^9$m is the distance from Earth to sun. I used the approximation in calculating orbital velocity $v = \sqrt{\frac{GM_S}{a}}$ that the Earth mass, is much smaller than the Sun's mass. So current orbital velocity is (using numbers as above) $29822$m/s.
Now, changing oribital distance outward by 1%, thus by $1.5\cdot 10^9$m, to $151.5\cdot 10^9$m yields a speed of $29674$m/s - and in energy that subsequently gives a difference of $2.64\cdot 10^{31}$J to move Earth's orbit about 1% to further from the Sun.
Annual world primary energy production currently is around $10^{20}$J - so we "just" need to produce 100.000.000.000 times the yearly energy production of the entire world to change Earth's orbit about 1%. And that implies that we have a technique to transfer energy 100% into Earth orbital velocity - something which cannot exist either due to simple thermodynamic argument.
Edit to add: Another way to argue is the rocket way: typical speed of conventional rocket exhausts are a few km/s, which is less than needed to leave Earth's orbit - that's why you need multi-stage rockets to get anything into orbit. But if you want to move the whole Earth with a rocket motor, you need a propellant which is fast enough that it directly leaves Earth's gravitational field - or you will not be able to create any effective change of momentum and only move around mass in the Earth system itself. So you need to make some substantial technological advances here, too - or some entirely different technique.

A:

I'll go out on a speculative limb and say yes, maybe, depending on the definition of "significant".
Planetmaker's answer notes the infeasibility of raising Earth's orbit if nothing else changes.  But what if we also lower some other body's orbit at the same time?
First, let the orbital energy of an object with mass $m$ orbiting the Sun with mass $M_S$ at an average distance of $a$ be its kinetic plus potential energy with respect to the Sun:
$E_k + U = \frac{1}{2}m v^2 - \frac{G M_S m}{a} = \frac{1}{2} m (\sqrt{\frac{GM_S}{a}})^2 = \frac{G M_S m}{2a} - \frac{G M_S m}{a} = -\frac{G M_S m}{2a} $
Our goal is to raise the Earth's average orbital radius by 1%.  Using the above equation and the specific values listed at the end, we need $2.62 \times 10^{31} \ \mathrm{J}$ to do that.  (This is all consistent with planetmaker's calculation, I just want to show my own work.)
Where can we get this energy? Let's try stealing Ceres.  If we drop its orbital radius down to match Earth's, we gain $2.65 \times 10^{29} \ \mathrm{J}$.  That's only 1% of the required energy.  But if we instead are content to change Earth's orbit by 0.01% (is that "significant"?) then we have enough energy to do it in Ceres.  If not, we need to get more bodies involved.  (Since Ceres alone is already about 30% of the asteroid belt mass, they will need to come from elsewhere.)
How do we transfer energy from Ceres to Earth?  We arrange for a series (no pun intended) of Gravitational slingshots between the two bodies, each time letting Ceres pass just ahead of the Earth, thereby transferring energy to the latter.  (As an outline of the encounter plan, my basic idea is we start by lowering its periapsis to match Earth, then all encounters happen at Ceres periapsis, thus preserving the possibility of future encounters.)
How do we change the orbit of Ceres to cause these slingshots?  We apply the same technique, recursively if needed.  Find something else nearby, presumably also in the asteroid belt, whose orbit we can perturb to cause encounters with Ceres, gradually steering it toward the eventual encounter with Earth.  The bottom of the recursion is some object small enough to be pushed (perhaps slowly) into an encounter with the next object using existing spacecraft and propulsion technology.
This would of course take a long time, at least tens to hundreds of thousands of years, but still well short of the hundred billion years planetmaker cited to move Earth using terrestrial energy sources.
At the core of this idea is the observation that N-body gravitational systems are chaotic, meaning that small changes in initial conditions can cause very large changes in later system state.  To move the world, Archimedes asked for a lever and a fulcrum.  But with modest technology, accurate foresight, and ample patience, in principle we should be able to manipulate the solar system almost at will without either.
The Wikipedia Asteroid capture article discusses some related concepts.
Specific numbers used in calculations (generally taken from Wikipedia):

$G = 6.67 \times 10^{-11} \frac{\mathrm{m}^3}{\mathrm{kg} \ \mathrm{s}^2}$
$M_S = 1.99 \times 10^{30} \ \mathrm{kg}$
$m_\mathrm{Earth} = 5.97 \times 10^{24} \ \mathrm{kg}$
$a_\mathrm{Earth} = 150 \times 10^9 \ \mathrm{m}$
$m_\mathrm{Ceres} = 2.38 \times 10^{20} \ \mathrm{kg}$
$a_\mathrm{Ceres} = 414 \times 10^9 \ \mathrm{m}$


7 Closed-Box Loudspeaker Systems7.1 ModelingtheBox7.2 The Analogous Circuits.7.3 The Volume Velocity Transfer Function.7.4 The On-Axis Pressure Transfer Function.7.5 Effect of the Box on the System Response.7.6 Sensitivity of the Lower Cutoff Frequency.7.7 System Design with a Given Driver.7.8 System Verification.7.9 System Design From Specifications. .7.10 A SPICE Simulation Example.7.11 Problems


Q:

Issue when checking if current viewController class is ABPersonViewController in IOS 7

I am loading ABPeoplePickerNavigationController. On the click of a contact in the peoplepicker, I am checking a condition
if([navigationController isKindOfClass:[ABPeoplePickerNavigationController class]]
   && [viewController isKindOfClass:[ABPersonViewController class]]){

  //Statements

}

But in IOS 7 I have noticed that, the second condition, that is
[viewController isKindOfClass:[ABPersonViewController class]

returns NO all the time. I know that the viewcontroller that is loaded is ABPersonViewController.
This was/is working fine until IOS 6. What could be the problem? Is there anyway I can get around this issue.
Edit:
The condition is checked inside UINavigationController Delegate
- (void)navigationController:(UINavigationController *)navigationController willShowViewController:(UIViewController *)viewController animated:(BOOL)animated

And the viewController class is shown as ABContactViewController when logged.

A:

When checking your class you will find that iOS7 returns a different type.
Review the logic for which you need the check. You should not have to use introspection to react appropriately to a people picker action. Just implement the standard delegate method from ABPeoplePickerNavigationControllerDelegate. In particular, you have to implement:
- (BOOL)peoplePickerNavigationController:
    (ABPeoplePickerNavigationController *)peoplePicker
     shouldContinueAfterSelectingPerson:(ABRecordRef)person;


Q:

How to control animation speed in iosSlider?

I am using iosSlider in my website. I need to change the animation speed of slider.
I have read documentation in iosSlider. I found I've to use autoSlideTransTimer for controlling slider speed. But I couldn't achieve that.
Here is my JavaScript code:
function InitImageSlider() {
$('.iosSlider').iosSlider
    desktopClickDrag: true,
    snapToChildren: true,
    infiniteSlider: true,
    navSlideSelector: '.slider .navigation li',
    onSlideComplete: function(args) {
        if(!args.slideChanged) return false;

        $(args.sliderObject).find('.slider-info').attr('style', '');

        $(args.currentSlideObject).find('.slider-info').animate({
            left: '15px',
            opacity: '.9'
        }, 'easeOutQuint');
    },
    onSliderLoaded: function(args) {
        $(args.sliderObject).find('.slider-info').attr('style', '');

        $(args.currentSlideObject).find('.slider-info').animate({
            left: '15px',
            opacity: '.9'
        }, 'easeOutQuint');
    },
    onSlideChange: function(args) {
        $('.slider .navigation li').removeClass('active');
        $('.slider .navigation li:eq(' + (args.currentSlideNumber - 1) + ')').addClass('active');
    },
    autoSlide: true,
    scrollbar: true,
    scrollbarContainer: '.sliderContainer .scrollbarContainer',
    scrollbarMargin: '0',
    scrollbarBorderRadius: '0',
    keyboardControls: true
});
}

A:

I am using iosSlider as well and this works for me:
$('.iosSlider').iosSlider({
        snapToChildren: true,
        scrollbar: false,
        scrollbarHide: true,
        desktopClickDrag: true,
        infiniteSlider: true,
        autoSlideTransTimer: 2000,
        navPrevSelector: '#sl-left',
        navNextSelector: '#sl-right',
        onSlideChange: slideChange,
        onSliderLoaded: slideChange,
        responsiveSlideContainer: false,
        responsiveSlides: false,
        autoSlide: true
    });

is significantly slower than:
$('.iosSlider').iosSlider({
        snapToChildren: true,
        scrollbar: false,
        scrollbarHide: true,
        desktopClickDrag: true,
        infiniteSlider: true,
        autoSlideTransTimer: 100,
        navPrevSelector: '#sl-left',
        navNextSelector: '#sl-right',
        onSlideChange: slideChange,
        onSliderLoaded: slideChange,
        responsiveSlideContainer: false,
        responsiveSlides: false,
        autoSlide: true
    });

So autoSlideTransTimer works for me!


Q:

How do Microsoft (and other software companies with a large installed base) manage patch dependencies?

OS (usually security-based) patches and hotfixes that Microsoft releases to the community normally consist of, in my understanding, a series of updated DLLs or other binaries.
How does Microsoft, and other companies like it, ensure that that hotfixes don't clash with each other?  Do they always go for a cumulative patch approach, where a single hotfix will includes all of the fixes in previous hotfixes?  This doesn't seem to be the case, because many hotfixes seem to be focused on fixing specific problems.  If they are focused hotfixes, how do they prevent one hotfix from trashing another one (e.g. incompatible DLLs being installed with each other).
I have always admired Microsoft's ability to manage this process.  The company I work for is much smaller, and when I worked on the patch process a few years ago, we always went for the cumulative approach, where a single patch immediately superseded all previous patches based on that release.  This meant that the patches got progressively larger in size, until the next "official" release came out.
What are some good practices for managing patch dependencies?

A:

First off, Microsoft Windows Installer has the ability to patch binaries directly.  Given known earlier states of a file, it can bring them to a known current state.  We used to do this for our Large Commercial Product, but after a couple of releases, it was taking upwards of 24 hours for our four-way systems to produce a patch - which isn't good when you have (or want to have) nightly builds.
After a while, we opted for cumulative fixes where we merely allowed upgrades.  We check that you're at a lower level, and then basically replace the entire product.  (We also had the case whereby the second or third "delta" was basically everything anyway.)
On Unix/Linux, we can't use MSWI, obviously, so we provide another installer which basically does the same thing: move all the files out of the way, install as if brand new, and then delete the backup.  The reality is, for us in our business, this is sufficient.  We haven't gotten any complaints that I'm aware of (and those complaints would hit me pretty quickly based on my current job) with people unhappy enough to actually call in and complain.  Mostly, they want to get the newer level with the patches so they can get on with their real business.  Oddly enough, their business isn't installing patches.


Solofill V1 GOLD CUP 24K Plated Refillable Filter Cup for Coffee Pod

Product prices and availability are accurate as of 2018-11-14 17:12:06 UTC and are subject to change. Any price and availability information displayed on http://www.amazon.com/ at the time of purchase will apply to the purchase of this product.

Not only you can save up to 80% by using your own favorite coffee, you also help save the environment from being polluted with plastic cups. The innovative Decaflo Spray Head combined with our proprietary Micro Foil filter pattern give you a perfectly brewed cup of rich and full-bodied coffee every time.


Clusterin accumulates in dying neurons following status epilepticus.
Clusterin is a protein that has been implicated in cell death and remodelling in a number of different tissues. To further investigate the role of clusterin in nerve cell death its expression was measured in the rat brain at various times after status epilepticus (SE) induced by 1 h of hippocampal stimulation, by using in situ hybridization, immunocytochemistry, and immunoblotting. SE lead to a dramatic time-dependent increase in clusterin mRNA in non-nerve cells resembling astrocytes in the hippocampus beginning after 24 h. There was also an earlier induction of clusterin mRNA in dentate granule cells, that survive SE. Only a low mRNA signal was observed over the CA1 pyramidal cells, which die after SE. In contrast to these mRNA results, massive clusterin-like immunoreactivity was observed in CA1 pyramidal cells and dentate hilar neurons (and both of these neuronal populations die after SE), but not in dentate granule cells. We speculate that astrocytes produce clusterin after SE and that the clusterin is then secreted and taken up by hippocampal neurons destined to die. Thus, the role of clusterin in nerve cell death/ regeneration warrants further investigation.


In vivo inhibition by a site-specific catalytic RNA subunit of RNase P designed against the BCR-ABL oncogenic products: a novel approach for cancer treatment.
One major obstacle to the effective treatment of cancer is to distinguish between tumor cells and normal cells. The chimeric molecules created by cancer-associated chromosomal abnormalities are ideal therapeutic targets because they are unique to the disease. We describe the use of a novel approach based on the catalytic RNA subunit of RNase P to destroy specifically the tumor-specific fusion genes created as a result of chromosome abnormalities. Using as a target model the abnormal BCR-ABL p190 and p210 products, we constructed M1-RNA with guide sequences that recognized the oncogenic messengers at the fusion point (M1-p190-GS and M1-p210-GS). To test the effectiveness and the specificity of M1-p190-GS and M1-p210-GS, we studied in vitro and in vivo effects of these RNA enzymes against BCR-ABL(p190) and BCR-ABL(p210), bearing in mind that both fusion genes share the ABL sequence but differ in the sequence coming from the BCR gene. We showed that M1-p190-GS and M1-p210-GS can act as sequence-specific endonucleases and can exclusively cleave target RNA that forms a base pair with the guide sequence (GS). We also demonstrated that when M1-p190-GS and M1-p210-GS were expressed in proper mammalian cell models, they abolished the effect of BCR-ABL by specifically decreasing the amount of the target BCR-ABL mRNA and preventing the function of the BCR-ABL oncogenes. These data clearly demonstrate the usefulness of the catalytic activity of M1-GS RNA to cleave specifically the chimeric molecules created by chromosomal abnormalities in human cancer and to represent a novel approach to cancer treatment.


1. Field of the Invention
The invention relates to automotive brake systems particularly for parking brakes. These brake systems are typically hand or foot actuated to impart tension on a strand which in turn imparts a force to set a brake or brakes. This invention uses a reactive slide enclosed in a housing to simultaneously impart tension to two or more strands to actuate brake mechanism.
2. Background Art
The use of lever actuated strands to set brakes is known in the art. Strands may act between two fixed points to impart a force to brake drums or calipers when one end is pulled by a setting lever that may be hand or foot activated. Sheathed strands, or cables, may be used in a similar fashion with the advantage that the strand itself is protected. Both implementations rely upon an actuating hand or foot mechanism and commonly employ, a bracket joining two brake strands so that they may be commonly actuated to impart uniform brake force to a drum or caliper. This construction requires that the assembly to achieve this either be housed within the vehicle to protect it from weathering or in the alternative, disposed beneath the vehicle where it is exposed to weathering. It is desirable to have a simplified brake system that is easily assembled to a motor vehicle and has the features of simplicity and weather resistance. The brake systems heretofore have not achieved this result.


In the late 1990s, the Hong Kong Polytechnic University and Tsinghua University took the lead in the pioneering research of fingerprint identification technology. Fingerprint identification has advantages such as high accuracy, fast speed, low price and high user acceptability, so it has attracted full academic attention since it was pioneered. Universities and research institutions both domestic and abroad have joined in this research field and made a series of achievements.
At present, fingerprint identification functions are incorporated into more and more display products. The structure of such a display product is usually implemented by adding a control transistor and a photosensitive element (such as a photoresistance or photosensitive diode) to a display pixel. That is, the control transistor controls the photosensitivity of the photosensitive element to achieve identification of fingerprints.
However, according to an existing control scheme for the photosensitive element, the control transistor is usually controlled individually. For example, scan lines for the control transistor are arranged separately and the control transistor is controlled individually by scanning. Meanwhile, transistors and scan lines used for displaying function in the display product are arranged separately for controlling normal display of pixels in the display product.
However, with such design of fingerprint identification, image display and fingerprint identification cannot be carried out synchronously. In other words, a fingerprint cannot be identified when a display image is viewed, and a special scan time for fingerprint identification is required. In actual applications such as fingerprint unlocking and fingerprint identification payment in which a screen or a payment interface is triggered by fingerprints, the fingerprint identification functions cannot be achieved with the image displayed normally, which leads to great inconvenience in the actual applications.