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# HD 172883

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 Catalogue of averaged stellar effective magnetic fields. I. Chemically peculiar A and B type starsThis paper presents the catalogue and the method of determination ofaveraged quadratic effective magnetic fields < B_e > for 596 mainsequence and giant stars. The catalogue is based on measurements of thestellar effective (or mean longitudinal) magnetic field strengths B_e,which were compiled from the existing literature.We analysed the properties of 352 chemically peculiar A and B stars inthe catalogue, including Am, ApSi, He-weak, He-rich, HgMn, ApSrCrEu, andall ApSr type stars. We have found that the number distribution of allchemically peculiar (CP) stars vs. averaged magnetic field strength isdescribed by a decreasing exponential function. Relations of this typehold also for stars of all the analysed subclasses of chemicalpeculiarity. The exponential form of the above distribution function canbreak down below about 100 G, the latter value representingapproximately the resolution of our analysis for A type stars.Table A.1 and its references are only available in electronic form atthe CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/407/631 and Tables 3 to 9are only available in electronic form at http://www.edpsciences.org Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin iThis work is the second part of the set of measurements of v sin i forA-type stars, begun by Royer et al. (\cite{Ror_02a}). Spectra of 249 B8to F2-type stars brighter than V=7 have been collected at Observatoirede Haute-Provence (OHP). Fourier transforms of several line profiles inthe range 4200-4600 Å are used to derive v sin i from thefrequency of the first zero. Statistical analysis of the sampleindicates that measurement error mainly depends on v sin i and thisrelative error of the rotational velocity is found to be about 5% onaverage. The systematic shift with respect to standard values fromSlettebak et al. (\cite{Slk_75}), previously found in the first paper,is here confirmed. Comparisons with data from the literature agree withour findings: v sin i values from Slettebak et al. are underestimatedand the relation between both scales follows a linear law ensuremath vsin inew = 1.03 v sin iold+7.7. Finally, thesedata are combined with those from the previous paper (Royer et al.\cite{Ror_02a}), together with the catalogue of Abt & Morrell(\cite{AbtMol95}). The resulting sample includes some 2150 stars withhomogenized rotational velocities. Based on observations made atObservatoire de Haute Provence (CNRS), France. Tables \ref{results} and\ref{merging} are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.125.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/393/897 Mercury Elemental and Isotopic Abundances in Mercury-Manganese StarsHg II abundances have been determined for 42 mercury-manganese (HgMn)stars by fitting synthetic spectra to observed spectra of the 3984Å Hg II line. Twenty of the stars had lines sharp enough to allowtheir Hg isotopic abundance mixes to be estimated. The Hg abundance isreported for more HgMn stars here than in any other single work. Nocorrelation was found between Hg II abundance and T_eff or the meancentral wavelength of HgMn lambda3984 stars. The mean central wavelengthof lambda3984 , an indicator of the Hg isotopic mix, is looselycorrelated with T_eff: stars with primarily heavy Hg isotopes tend to becooler, although one star, 46 Aql, has almost pure ^204Hg and T_eff inabout the middle of the temperature range for HgMn stars. We find thatthere is no evidence that any of the HgMn stars have ^196Hg or ^198Hg.For the very sharp-lined stars, the ^204Hg abundance decreases withincreasing T_eff. No correlation is seen between the mean centralwavelength and the surface gravity. No correlation was found between theprojected rotational velocity and the Hg II abundance or the centralwavelength of lambda3984, although this result may be biased by theselection of stars with low reported vsini. Hg I lambda4358 was measuredat high spectral resolution for seven HgMn stars. The isotopic shiftsare too small, and the hyperfine components are too weak to allowunambiguous isotopic abundance ratios to be found. Hg I abundancescorrelate fairly well with Hg II abundances. Some of the Hg isotopicmixtures are difficult to explain using only diffusion. HR 7245 hasapproximately equal abundances of ^199Hg, ^200Hg, ^202Hg, and ^204Hg butvery little ^201Hg, and 11 Per has Hg that is mostly ^199Hg and ^204Hg.Calculations show that hyperfine splitting of ^201Hg changes theradiative forces it feels compared with other isotopes, which may alterdiffusion of that isotope enough to explain its absence in HR 7245, butwe have found no possible explanation for the Hg isotopic mix found in11 Per. These are the first very high resolution measurements of Hg IIlambda3984 for HR 7245 and 11 Per. Although diffusion may be acting inHgMn stars, either there are one or more other mechanisms acting to helpproduce the overabundances and isotopic mixtures seen or ourunderstanding of diffusion is lacking on some important point. Speckle Interferometry of New and Problem HIPPARCOS BinariesThe ESA Hipparcos satellite made measurements of over 12,000 doublestars and discovered 3406 new systems. In addition to these, 4706entries in the Hipparcos Catalogue correspond to double star solutionsthat did not provide the classical parameters of separation and positionangle (rho,theta) but were the so-called problem stars, flagged G,''O,'' V,'' or X'' (field H59 of the main catalog). An additionalsubset of 6981 entries were treated as single objects but classified byHipparcos as suspected nonsingle'' (flag S'' in field H61), thusyielding a total of 11,687 problem stars.'' Of the many ground-basedtechniques for the study of double stars, probably the one with thegreatest potential for exploration of these new and problem Hipparcosbinaries is speckle interferometry. Results are presented from aninspection of 848 new and problem Hipparcos binaries, using botharchival and new speckle observations obtained with the USNO and CHARAspeckle cameras. On the HIPPARCOS photometry of chemically peculiar B, A, and F starsThe Hipparcos photometry of the Chemically Peculiar main sequence B, A,and F stars is examined for variability. Some non-magnetic CP stars,Mercury-Manganese and metallic-line stars, which according to canonicalwisdom should not be variable, may be variable and are identified forfurther study. Some potentially important magnetic CP stars are noted.Tables 1, 2, and 3 are available only in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html The observed periods of AP and BP starsA catalogue of all the periods up to now proposed for the variations ofCP2, CP3, and CP4 stars is presented. The main identifiers (HD and HR),the proper name, the variable-star name, and the spectral type andpeculiarity are given for each star as far as the coordinates at 2000.0and the visual magnitude. The nature of the observed variations (light,spectrum, magnetic field, etc.) is presented in a codified way. Thecatalogue is arranged in three tables: the bulk of the data, i.e. thosereferring to CP2, CP3, and CP4 stars, are given in Table 1, while thedata concerning He-strong stars are given in Table 2 and those foreclipsing or ellipsoidal variables are collected in Table 3. Notes arealso provided at the end of each table, mainly about duplicities. Thecatalogue contains data on 364 CP stars and is updated to 1996, October31. This research has made use of the SIMBAD database, operated at CDS,Strasbourg, France. UBV photometry of Be stars at Hvar: 1972--1990A summary of results of the systematic UBV photoelectric monitoring ofbright northern Be stars carried out at the Hvar Observatory between1972 and 1990 is presented. Altogether, 76 Be stars of all luminosityclasses were observed and 13,848 UBV measurements secured.Simultaneously, 9,648 UBV measurements of 48 check stars (most of themof early spectral types) were obtained. A careful transformation of allobservations into the standard Johnson system allowed detection andmonitoring of even very mild long-term light and colour variations ofthese objects. Almost all early-type Be stars in the sample turned outto be variable. For several stars phase-locked light variations relatedto their binary nature were established. Sudden brightenings, on a timescale of a few days, were detected for o Cas and QR Vul. Tables 2 and 3are only available in electronic form at CDS via ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html The photoelectric astrolabe catalogue of Yunnan Observatory (YPAC).The positions of 53 FK5, 70 FK5 Extension and 486 GC stars are given forthe equator and equinox J2000.0 and for the mean observation epoch ofeach star. They are determined with the photoelectric astrolabe ofYunnan Observatory. The internal mean errors in right ascension anddeclination are +/- 0.046" and +/- 0.059", respectively. The meanobservation epoch is 1989.51. The Relation between Rotational Velocities and Spectral Peculiarities among A-Type StarsAbstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995ApJS...99..135A&db_key=AST Reality Tests of Superclusters in the Young Disk PopulationAbstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1995AJ....110.2862E&db_key=AST Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with. A new list of effective temperatures of chemically peculiar stars. II.Not Available Reliable photometric reductions to the standard UBV (or uvby) system and accurate UBV magnitudes of bright standard stars from the northern part of the international Be programA modified method of computer reduction of UBV (or uvby) photoelectricobservations to standard systems, which combines advantages of what hasso far been achieved in this area, is described in detail. A completereduction of over 46000 UBV observations obtained at Hvar Observatorybetween 1972 and 1991, and of nearly 5000 UBV observations secured atSkalnate Pleso Observatory between 1980 and 1987, was carried out usingthe new technique. It is argued that replacing the original Johnson'sUBV values for the non-variable stars that were observed by the meanvalues based on repeated observations over several years and applyingthe new reduction technique can ensure a stable reproduction of UBVmagnitudes, obviously quite close to the standard Johnson's ones, overmany years and from observatories situated at very different altitudesabove sea level within about 0.01mag in all three UBV magnitudes. A listof new accurate mean UBV values of 191 stars which were regularlyobserved at Hvar - and a part of them also at Skalnate Pleso - ascomparison, check and standard stars in the Be- and Ap-star observingprograms, is included for future use by photometric observers in theNorthern Hemisphere. For a number of these stars, we can guaranteesecular constancy within 0.mag01 during the past 5 to 15 years. Third supplement to the catalogue of observed periods of AP starsNew data on the periods of Ap stars with references are presented.Twelve further stars are introduced for which a periodic variability hasrecently been discovered or not reported in previous issues of thiscatalog. For many stars also present in previous issues of the catalognew determinations of the periods are given. Recently attributedvariable star names are also quoted. Long-term monitoring of active stars. I - 1988-89 UBV photometry with the PHOENIX APTAs part of a large program aimed at studying the global properties andevolution of active star atmospheres, high-precision UBV photometry ofselected RS CVn, BY Dra, and FK Com-type systems has been carried outsince early 1988 by using the Phoenix 25-cm Automatic PhotoelectricTelescope at Whipple Observatory on Mt. Hopking (USA, AZ). We presentthe results of systematic obsrvations of nine active stars monitoredduring the years 1988 and 1989. Significant evolution of the wave-likelight curves for most of the observed stars, both in amplitude andshape, is found. These photometric data can give important clues on thelifetimes of spotted areas and associated magnetic structures,differential rotation and solar-like cycles, and are required to addressthe question of spatial and physical correlations between confinedstructures in active star photospheres and outer atmospheres, the latterderived from chromospheric and transition region spectral signatures atother wavelengths. Evidence of long-term variability for most of theobserved stars is also presented. Magnetic Fields and Other Parameters of Chemically Peculiar Stars - Part TwoNot Available Photoelectric monitoring of bright Be starsThe paper describes and summarizes BV photometric observations of 34bright, active Be stars made at various times between 1981 and 1987 witha 0.4-m telescope at the University of Toronto. These observationsdemonstrate the photometric variability of Be stars on time scales ofhours to years. Stellar activity in synchronized binaries. II - A correlation analysis with single starsThe interdependences between various measures of activity and a numberof relevant stellar parameters are investigated for a sample of largelypostmain-sequence late-type binaries with orbital periods from 1-100days, and the stars are compared with single dwarfs having similarperiods. Activity for these binaries is found to depend primarily onstellar rotation, with the surface flux being the preferred means ofexpressing activity. The normalized luminosity parameter and the totalluminosity are shown to be less desirable means for expressing activity.The binaries and single stars are found to exhibit similar dependencesof activity on either their rotation periods or Rossby numbers. The Chemically Peculiar Star W-Ursae - Part One - Identification of Spectral LinesAbstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985CoSka..13....9H&db_key=AST The local system of early type stars - Spatial extent and kinematicsPublished uvby and H-beta photometric data and proper motions arecompiled and analyzed to characterize the structure and kinematics ofthe bright early-type O-A0 stars in the solar vicinity, with a focus onthe Gould belt. The selection and calibration techniques are explained,and the data are presented in extensive tables and graphs and discussedin detail. The Gould belt stars of age less than 20 Myr are shown togive belt inclination 19 deg to the Galactic plane and node-lineorientation in the direction of Galactic rotation, while the symmetricaldistribution about the Galactic plane and kinematic properties (purecircular differential rotation) of the belt stars over 60 Myr oldresemble those of fainter nonbelt stars of all ages. The unresolveddiscrepancy between the expansion observed in the youngest nearby starsand the predictions of simple models of expansion from a point isattributed to the inhomogeneous distribution of interstellar matter. Radial velocities of northern Mercury starsAbout 200 radial velocities of 96 bright northern Hg-Mn or candidateHg-Mn stars are presented. Past and present data have been reexaminedfor periodic variability in cases that were neither previously known tobe binaries with well determined orbits nor were considered to haveconstant velocity. One definite new orbit was found (that of HR 3361)and several possible orbital solutions are given. A catalogue and bibliography of Mn-Hg starsAbstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1981A&AS...44..137S&db_key=AST Properties and nature of Be and shell stars. X - Light and colour variations of CX DRANot Available Stellar abundances from line statisticsThe method of linear statistical modeling has been combined with arudimentary model of stellar photospheres to obtain abundance estimatesfor a large member of normal and peculiar upper-main-sequence stars. Theadopted standard abundances, obtained from published fine analyses, canbe fitted by the algorithms with about 0.5 dex as the standarddeviation. A major advantage of the technique introduced here, based onwavelength coincidences, is that the statistical presence ofintrinsically faint stellar lines plays a key role. This can minimizesystematic errors due to curve-of-growth-saturation effects. Errors dueto misidentified features are also minimized. In spite of theseadvantages, the present method is advocated as an ancillary tool foruse, ultimately, in the improvement of results obtained by moretraditional methods. Abundances, rounded to the nearest 0.5 dex, arereported for Cr, Mn, Fe, and Y. The largest ranges of abundances arefound for chromium and yttrium. A remarkable constancy has been foundfor iron. Absolute ultraviolet spectrophotometry from the TD1 satellite. X - The ultraviolet spectrum of the AP starsThe UV Bright Star Spectrophotometric Catalog, developed withobservations from the TD-1 satellite, provides data for comparing 77 Apstars with 344 normal stars in the ultraviolet from 1350 to 2550 A. TheBalmer and Paschen continua in the Ap stars are connected by means of along basis (2100 versus 5500 A) index. For discriminating Ap stars fromnormal ones, as well as for detecting new Ap stars, a flux deficiency at1400 A proves to be very valuable; the 1400 A feature appears to stemeither from Fe II lines in cooler Ap stars or from Si II autoionization.Domination of the Si and SrCrEu star spectra by metallic lines is alsodiscussed. A photometric peculiarity index in the AP starsIntermediate-band photoelectric observations obtained to study the broadabsorption features recently discovered in the continua of the Ap starsare reported. The observations extend the spectral range from 3200 to8500 A with a spectral coverage of 82% in a search for previouslyundetected features. No new features were found. Observations of thestrength of the 5300-A feature for 56 Ap stars are reported. For severalstars having multiple observations, variability of the 5300-A featurewas observed. Is star formation bimodal ? II. The nearest early-type stars.Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977PASP...89..187E&db_key=AST Spectral classification from the ultraviolet line features of S2/68 spectra. II - Late B-type starsAbstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977A&AS...30...71C&db_key=AST The spectroscopic binary characteristics of the mercury-manganese stars.Not Available Isotopic abundances of HG in mercury stars inferred from the HG II line at 3984 AWavelengths of the Hg II absorption feature at 3984 A in 30 Hg stars aredistributed uniformly from the value for the terrestrial mix to a valuethat corresponds to nearly pure Hg-204. The wavelengths are correlatedloosely with effective temperatures inferred from Q(UBV). Relativeisotopic abundances derived from partially resolved profiles of the3984-A line in iota CrB, chi Lup, and HR 4072 suggest thatmass-dependent fractionation has occurred in all three stars. It issupposed that such fractionation occurs in all Hg stars, and a schemewhereby isotopic compositions can be inferred from a comparison ofstellar wavelengths and equivalent widths with those calculated for afamily of fractionated isotopic mixes. Theoretical profiles calculatedfor the derived isotopic composition agree well with high-resolutioninterferometric profiles obtained for three of the stars.

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 星座: 天龍座 右阿森松: 18h39m52.80s 赤纬: +52Â°11'46.0" 视星: 6 距离: 172.712 天文距离 右阿森松适当运动: 7.6 赤纬适当运动: 21.8 B-T magnitude: 5.909 V-T magnitude: 5.981