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The New HiVIS Spectropolarimeter and Spectropolarimetric Calibration of the AEOS Telescope
We have designed, built, and calibrated a new spectropolarimeter for theHiVIS spectrograph (R ~ 12,000-49,000) on the Advanced Electro-OpticalSystem (AEOS) telescope. We have also conducted a polarizationcalibration of the telescope and instrument. In this paper, we introducethe design and use of the spectropolarimeter, in addition to a newdata-reduction package we have developed, and then discuss thepolarization calibration of the spectropolarimeter and the AEOStelescope. We used observations of unpolarized standard stars at manypointings to measure the telescope-induced polarization and compare itwith a Zemax model. The telescope induces polarization of 1%-6%, with astrong variation with wavelength and pointing, consistent with theexpected altitude and azimuth variation. We then used scattered sunlightas a linearly polarized source to measure the telescope'sspectropolarimetric response to linearly polarized light. Finally, wemade an all-sky map of the telescope's polarization response tocalibrate future spectropolarimetry.




An Improved Infrared Passband System for Ground-based Photometry: Realization
We describe new simulations and field trials of the new infraredpassband system developed and discussed by Young, Milone, & Stagg,who discussed and illustrated the state of infrared photometry andsuggested ways in which it could be improved. In particular, theypresented a new set of passbands that minimize the dependence of thephotometry on the water vapor bands of the atmospheric windows, whichdefined the edges of many previous infrared passbands, especially whenused at sites and under conditions for which they were not designed. Inthis paper, we present numerical simulations for three atmosphericmodels, demonstrate a measure of the signal-to-noise ratio in the newpassbands for these models, and present observational data obtained at arelatively low-elevation site. The latter demonstrate the utility ofthis system for most astronomical sites where photometry can beperformed, and permit the transformation of observations to this system.Publications of the Rothney Astrophysical Observatory, No. 74.





An Excess Due to Small Grains around the Nearby K0 V Star HD 69830: Asteroid or Cometary Debris?
Spitzer photometry and spectroscopy of the star HD 69830 reveal anexcess of emission relative to the stellar photosphere between 8 and 35μm dominated by strong features attributable to crystalline silicateswith an emitting surface area more than 1000 times that of our zodiacalcloud. The spectrum closely resembles that of the comet C/1995 O1(Hale-Bopp). Since no excess is detected at 70 μm, the emittingmaterial must be quite warm, be confined within a few AU of the star,and originate in grains with low, long-wavelength emissivity, i.e.,grains much smaller than 70μm/2π~10 μm. The strongmineralogical features are evidence for even smaller, possiblysubmicron-sized grains. This small grain size is in direct contrast tothe 10-100 μm grains that dominate the relatively featureless spectraof our zodiacal dust cloud and most other main-sequence stars withexcesses. The upper limit at 70 μm also implies that any Kuiper Beltanalog must be either very cold or less massive than ~5 times our ownKuiper Belt. With collisional and Poynting-Robertson drag times of lessthan 1000 yr for small grains, the emitting material must either (1) becreated through continual grinding down of material in a dense asteroidbelt, or (2) originate in cometary debris arising from either a single``supercomet'' or a very large number of individual comets arriving froma distant reservoir. In the case of a cometary origin for the emission,the mass requirements for continuous generation by many individualcomets are unreasonable, and we favor the capture of a single supercomet into a 0.5-1 AU orbit, where it can evolve a large number of smallgrains over a 2 Myr period.


Stellar activity cycles: observing the dynamo?
The enormous complexity of the atmospheric structure observed on the Sunmakes it very difficult to compare the Sun with ``solar-type stars''.Clearly, we need to identify parameters that can be observed on the Sunas well as on other stars which can be interpreted unambiguously. Themost widely accepted dynamo signature is the presence of an activitycycle, well documented for the Sun and for main-sequence stars due tothe Mount Wilson Ca II H&K project. Only recently have we detectedspatial information, differential rotation and possibly meridional flowson other stars and thereby adding another constraint for itsinterpretation within a dynamo theory. Again, the picture is notcomplete yet, despite that there is just a single main ingredient thatacts as the driving mechanism for activity in all atmospheric layers andthe convective envelope of a solar-type star: the dynamo-relatedmagnetic field. I stress the importance of mapping stellar surfaces asfingerprints of the underlying dynamo action over long periods of time.

Abundance trends in kinematical groups of the Milky Way's disk

The fundamental parameters of the Algol binary AI Draconis revisited
We present the results of an analysis of our infrared light curves ofthe Algol-type binary AI Draconis in the J, H and K bands, and ofpublished light curves in the B, V and Strömgren uvby bands,together with spectra obtained by us. The analysis of the light curveswas carried out using a code based on ATLAS model atmospheres and Rochegeometry.The small contribution of the secondary cool component to the totallight of the system in the visible, producing light curves with veryshallow secondary eclipses, makes the stellar and orbital parametersderived from light-curve analysis in the visible spectral rangeuncertain. The larger contribution of the secondary star to the infraredfluxes makes this range particularly well suited to the derivation ofprecise orbital and stellar parameters in binaries of Algol type. Fromthe simultaneous solution of the infrared JHK light curves, we derivethe following absolute orbital and stellar parameters for the twocomponents: = 10160 +/- 160 K,Req,1= 2.12 +/- 0.04 Rsolar,log()1= 4.23; = 5586 +/-110 K, Req,2= 2.36 +/- 0.04 Rsolar,log()2= 3.76; M1= 2.86 +/- 0.09Msolar, q=M2/M1= 0.44 +/- 0.03; a= 7.62+/- 0.09 Rsolar, i= 76.53°+/- 0.3°, e~= 0.0. Here, and log() indicate average surfacevalues, Req is the equivalent radius of the deformed star anda is the orbital size.In our light-curve solutions, the secondary star of AI Dra fills itsRoche lobe (as also indicated by the spectroscopy), thus discountingclaims, based on UBV light curves, that both components of the binaryare located within their Roche lobes. The visible and infraredphotometry show no evidence of any significant infrared excess in thesystem, and the distance of AI Dra is estimated as d= 169 +/- 17 pc.Based on the spectra of AI Dra and template stars in the ranges8210-9060, 6250-7130 and 4040-4920 Å, we classify the stellarcomponents of AI Dra and find that the most probable spectral types areA0V (or perhaps A1V) for the primary and F9.5V for the secondary(although it could reach as far as G4V), respectively. From ourspectroscopic observations, the spectral evolution of AI Dra withorbital phase is also presented. Furthermore, we obtain the projectedrotational velocity of the secondary, whose value turns out to becompatible with the star filling its Roche lobe.

Lithium abundances of the local thin disc stars

Stars of Extragalactic Origin in the Solar Neighborhood
For 77 main-sequence F-G stars in the solar neighborhood with publishediron, magnesium, and europium abundances determined from high-dispersionspectra and with the ages estimated from theoretical isochrones, wecalculated the spatial velocities using Hipparcos data and the Galacticorbital elements. A comparison with the orbital elements of the globularclusters that are known to have been accreted by our Galaxy in the pastreveals stars of extragalactic origin. We show that the abundance ratiosof r- and alpha-elements in all the accreted stars differ sharply fromthose in the stars that are genetically associated with the Galaxy.According to current theoretical models, europium is produced mainly inlow-mass type-II supernovae (SNe II), while magnesium is synthesized inlarge quantities in high-mass SN II progenitors. Since all the oldaccreted stars of our sample exhibit a significant Eu overabundancerelative to Mg, we conclude that the maximum masses of the SN IIprogenitors outside the Galaxy were much lower than those inside it. Onthe other hand, only a small number of young accreted stars exhibit lownegative ratios [Eu/Mg] < 0. This can be explained by the delay ofprimordial star formation and the explosions of high-mass SNe II in arelatively small part of extragalactic space. We provide evidence thatthe interstellar medium was weakly mixed at the early evolutionarystages of the Galaxy formed from a single protogalactic cloud, and thatthe maximum mass of the SN II progenitors increased in it with timesimultaneously with the increase in mean metallicity.

Neutron-Capture Elements in Halo, Thick-Disk, and Thin-Disk Stars: Neodymium
We have derived the LTE neodymium abundances in 60 cool stars withmetallicities [Fe/H] from 0.25 to -1.71 by applying a synthetic-spectrumanalysis to spectroscopic observations of NdII lines with a resolutionof λ/Δλ⋍60 000 and signal-to-noise ratios of100 200. We have improved the atomic parameters of NdII and blendinglines by analyzing the corresponding line pro files in the solarspectrum. Neodymium is overabundant with respect to iron in halo stars,[Nd/Fe]=0.33±0.09, with the [Nd/Fe] ratio decreasingsystematically with metallicity when [Fe/H]>-1. This reflects anonset of efficient iron production in type I supernovae during theformation of the thick disk. The [Nd/Ba] and [Nd/Eu] abundance ratiosbehave differently in halo, thick-disk, and thin-disk stars. Theobserved abundance ratios in halo stars, [Nd/Ba]=0.34±0.08 and[Nd/Eu]=-0.27±0.05, agree within the errors with the ratios ofthe elemental yields for the r-process. These results support theconclusion of other authors based on analyses of other elements that ther-process played the dominant role in the synthesis of heavy elementsduring the formation of the halo. The [Nd/Ba] and [Nd/Eu] ratios forthick-disk stars are almost independent of metallicity([Nd/Ba]=0.28(±0.03)-0.01(±0.04) [Fe/H] and[Nd/Eu]=-0.13(±0.03)+0.05(±0.04) [Fe/H]) but are smallerin absolute value than the corresponding ratios for halo stars,suggesting that the synthesis of s-process nuclei started during theformation of the thick disk. The s-process is estimated to havecontributed ⋍30% of the neodymium produced during this stage ofthe evolution of the Galaxy. The [Nd/Ba] ratio decreases abruptly by0.17 dex in the transition from the thick to the thin disk. Thesystematic decrease of [Nd/Ba] and increase of [Nd/Eu] with increasingmetallicity of thin-disk stars point toward a dominant role of thes-process in the synthesis of heavy elements during this epoch.


The Indo-US Library of Coudé Feed Stellar Spectra

The Rise of the s-Process in the Galaxy


Nearby stars of the Galactic disk and halo. III.

Stellar Chemical Signatures and Hierarchical Galaxy Formation

Empirically Constrained Color-Temperature Relations. II. uvby

Sodium abundances in nearby disk stars


Non-LTE Analysis of the Sodium Abundance of Metal-Poor Stars in the Galactic Disk and Halo
We performed an extensive non-LTE analysis of the neutral sodium linesof Na I 5683/5688, 5890/5896, 6154/6161, and 8183/8195 in disk/halostars of types F-K covering a wide metallicity range (-4 <≈[Fe/H] <≈ +0.4), using our own data as well as data collectedfrom the literature. For comparatively metal-rich disk stars (-1<≈ [Fe/H] <≈ +0.4) where the weaker 6154/6161 linesare the best abundance indicators, we confirmed [Na/Fe]  0 with an"upturn" (i.e., a shallow/broad dip around -0.5 <≈ [Fe/H]<≈ 0) as already reported in previous studies. For themetal-deficient halo stars, where the much stronger 5890/5896 or8183/8195 lines subject to considerable (negative) non-LTE correctionsamounting to 0.5 dex have to be used, our analysis suggests mildly"subsolar" [Na/Fe] values down to  -0.4 (with a somewhat largescatter of  ± 0.2 dex) on the average at the typical halometallicity of [Fe/H]  -2, followed by a rise again to a near-solarratio of [Na/Fe]  0 at the very metal-poor regime [Fe/H]  -3to -4. These results are discussed in comparison with the previousobservational studies along with the theoretical predictions from theavailable chemical evolution models.

Observational Constraints on Potassium Synthesis During the Formation of Stars of the Galactic Disk
The non-LTE potassium abundances in the atmospheres of 33 Galactic-diskstars are derived and the parameters of the atmospheres of 23 of thestars are determined. Neglecting departures from LTE results in asystematic overestimation of the potassium abundances and an increase intheir dispersion, even for differential analyses relative to the Sun.The non-LTE corrections are significant ((-0.2) (-0.6) dex) and dependon the surface gravities and effective temperatures of the stars. Themean potassium abundance for a sample of ten stars with [Fe/H]0.0is in agreement with the solar and meteoritic abundances (log ɛȯ(K)=5.12). As the stellar metallicity increases from [Fe/H]=(-1.0)to (0.2) dex, the [K/Fe] ratio decreases systematically from 0.3 dex to-0.1 dex. The derived dependence [K/Fe]-[Fe/H] is in agreement with theresults of published model calculations of the chemical evolution of theGalaxy. This indicates the dominance of explosive oxygen burning inmassive type II supernovae during the synthesis of potassium in theGalactic disk.

Broad-band Multicolor Photometry and Polarimetry of Spotted Stars
We have confirmed the BY Dra-type variability of the active spottedstars MS Ser, LQ Hya, VY Ari, and EK Dra using simultaneous UBVRIphotometric and polarimetric observations. We have also reliablydetected the intrinsic linear polarization of their radiation and itsrotational modulation in U due to the inhomogeneous distribution ofactive magnetized regions over the surfaces of the stars. Modeling ofthe linear polarization based on the Zeeman effect indicates that allthe stars display strong local magnetic fields (about 2 kG, similar tothose in sunspots), with filling factors of up to 40% of the totalstellar surface. The magnetized regions coincide with cool photosphericspots detected in photoelectric observations.

High-Precision Stellar Radial Velocities in the Galactic Center



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距离:15.853 天文距离
B-T magnitude:5.278
V-T magnitude:4.664

适当名称   (Edit)
Bayerχ Her
Flamsteed1 Her
HD 1989HD 142373
TYCHO-2 2000TYC 3057-2021-1
USNO-A2.0USNO-A2 1275-08774476
BSC 1991HR 5914
HIPHIP 77760

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