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Magnetic fields of chemically peculiar stars. I. The catalog of magnetic CP stars
This is the first paper of the series dedicated to the analysis of themagnetism of chemically peculiar (CP) stars of the upper Main Sequence.We use our own measurements and published data to compile a catalog ofmagnetic CP stars containing a total of 326 objects with confidentlydetected magnetic fields and 29 stars which are very likely to possessmagnetic field. We obtained the data on the magnetism of theoverwhelming majority of the stars solely based on the analysis oflongitudinal field component B e . The surface magneticfield, B s , has been measured for 49 objects. Our analysisshows that the number of magnetic CP stars decreases with increasingfield strength in accordance with exponential law, and stars with B e exceeding 5kG occur rarely (about 3% objects of ourlist).
| Lithium in chemically peculiar CP stars with magnetic fields
The problem of lithium in chemically peculiar Ap-CP stars has been thesubject of debate for many years. The main reason for this is a lack ofspectral observations of Ap stars in the neighborhood of the lithiumresonance doublet Li I 6708 Å. An international cooperationproject on “Lithium in cool CP stars with magnetic fields”was started in 1996. Systematic observations of CP stars in spectralregions of the 6708 Å and 6103 Å lines at the ZTSh (CrAO),CAT (ESO), Feros (ESO), and the 74″ telescope of the Mount StromloObservatory (Australia) have been used to analyze spectra of several CPstars studied by the way the 6708 Å lithium line varies with thestars’ rotational phase. Monitoring of the spectra of theoscillating CP stars (group I) HD 83368, HD 60435, and HD 3980, forwhich significant Doppler shifts of the Li I 6708 Å line areobserved led to the discovery of “lithium spots” on thesurface of these stars whose positions are related to the magnetic fieldstructure. Models of the surfaces of these stars with the specialprogram “ROTATE” based on the profiles of the Li I 6708Å line are used to estimate the size of the spots, their positionson the stars’ surface, and the lithium abundances in these spots.A detailed analysis and modelling of the spectra of slowly rotatingoscillating CP stars with strong, invariant lithium 6708 Åemission, including blending with lines of the rare earth elements,reveals an enhanced lithium abundance, with the abundance determinedfrom the lithium 6103 Å line being higher than that determinedfrom the 6708 Å line for all the stars. This may indicate verticalstratification of lithium in the atmospheres of CP stars with ananomalous isotopic composition (6Li/7Li = 0.20.5). HD 101065, an ultraslow rotator (vsini ≈ 1.5) visible from thepoles and with powerful oscillations which cause pulsating linebroadening in its spectrum, is unique among these stars. The amount oflithium in the atmosphere of HD 101065 logN(Li) = 3.1 on a scale oflogN(H) = 12.0 and the isotope ratio 6Li/7Li ≈0.3. The high estimates of 6Li/7Li may beexplained by the production of lithium in spallation reactions and thepreservation of surface 6Li and 7Li by strongmagnetic fields in the upper layers of the atmosphere near the magneticpoles.
| Evolutionary state of magnetic chemically peculiar stars
Context: .The photospheres of about 5-10% of the upper main sequencestars exhibit remarkable chemical anomalies. Many of these chemicallypeculiar (CP) stars have a global magnetic field, the origin of which isstill a matter of debate. Aims: .We present a comprehensivestatistical investigation of the evolution of magnetic CP stars, aimedat providing constraints to the theories that deal with the origin ofthe magnetic field in these stars. Methods: .We have collectedfrom the literature data for 150 magnetic CP stars with accurateHipparcos parallaxes. We have retrieved from the ESO archive 142 FORS1observations of circularly polarized spectra for 100 stars. From thesespectra we have measured the mean longitudinal magnetic field, anddiscovered 48 new magnetic CP stars (five of which belonging to the rareclass of rapidly oscillating Ap stars). We have determined effectivetemperature and luminosity, then mass and position in the H-R diagramfor a final sample of 194 magnetic CP stars. Results: .We foundthat magnetic stars with M > 3 ~M_ȯ are homogeneouslydistributed along the main sequence. Instead, there are statisticalindications that lower mass stars (especially those with M ≤2~M_ȯ) tend to concentrate in the centre of the main sequence band.We show that this inhomogeneous age distribution cannot be attributed tothe effects of random errors and small number statistics. Our datasuggest also that the surface magnetic flux of CP stars increases withstellar age and mass, and correlates with the rotation period. For starswith M > 3~M_ȯ, rotation periods decrease with age in a wayconsistent with the conservation of the angular momentum, while for lessmassive magnetic CP stars an angular momentum loss cannot be ruledout. Conclusions: .The mechanism that originates and sustains themagnetic field in the upper main sequence stars may be different in CPstars of different mass.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Transition probabilities and lifetimes in singly ionized rhenium
Transition probabilities and radiative lifetimes have been obtained for45 transitions of ReII using a combination of radiative lifetime valuesobtained with the laser-induced fluorescence technique (seven levels)and theoretical branching fractions. This new set of results, concerningultraviolet and visible lines, will be useful in the future forinvestigating the composition of chemically peculiar stars.
| A catalog of stellar magnetic rotational phase curves
Magnetized stars usually exhibit periodic variations of the effective(longitudinal) magnetic field Be caused by their rotation. Wepresent a catalog of magnetic rotational phase curves, Be vs.the rotational phase φ, and tables of their parameters for 136stars on the main sequence and above it. Phase curves were obtained bythe least squares fitting of sine wave or double wave functions to theavailable Be measurements, which were compiled from theexisting literature. Most of the catalogued objects are chemicallypeculiar A and B type stars (127 stars). For some stars we also improvedor determined periods of their rotation. We discuss the distribution ofparameters describing magnetic rotational phase curves in our sample.All tables and Appendix A are only available in electronic form athttp://www.edpsciences.org
| Catalogue of averaged stellar effective magnetic fields. I. Chemically peculiar A and B type stars
This 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
| Characteristic Features of the Spectrum of the Unique roAp Star HD 101065 near the 6708 Å Lithium Resonance Doublet
Synthetic spectrum of the peculiar roAp star HD 101065(Przybylski’s Star) have been computed in the wavelength interval6705.8 6708.7 Å in order to describe the observed spectrum in thevicinity of the 6708 Å lithium line. Our detailed computations ofthe synthetic spectrum allowing for the hyperfine structure of thelithium line, lithium isotopic composition, and blending due to lines ofrare-earth elements (CeII, NdII, SmII, and others) have yieldedestimates of the atmospheric lithium abundance of the star and its6Li/7Li isotopic ratio.
| Multiplicity among chemically peculiar stars. II. Cool magnetic Ap stars
We present new orbits for sixteen Ap spectroscopic binaries, four ofwhich might in fact be Am stars, and give their orbital elements. Fourof them are SB2 systems: HD 5550, HD 22128, HD 56495 and HD 98088. Thetwelve other stars are: HD 9996, HD 12288, HD 40711, HD 54908, HD 65339,HD 73709, HD 105680, HD 138426, HD 184471, HD 188854, HD 200405 and HD216533. Rough estimates of the individual masses of the components of HD65339 (53 Cam) are given, combining our radial velocities with theresults of speckle interferometry and with Hipparcos parallaxes.Considering the mass functions of 74 spectroscopic binaries from thiswork and from the literature, we conclude that the distribution of themass ratio is the same for cool Ap stars and for normal G dwarfs.Therefore, the only differences between binaries with normal stars andthose hosting an Ap star lie in the period distribution: except for thecase of HD 200405, all orbital periods are longer than (or equal to) 3days. A consequence of this peculiar distribution is a deficit of nulleccentricities. There is no indication that the secondary has a specialnature, like e.g. a white dwarf. Based on observations collected at theObservatoire de Haute-Provence (CNRS), France.Tables 1 to 3 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/394/151Appendix B is only available in electronic form athttp://www.edpsciences.org
| Experimental and theoretical studies of DyIII: radiative lifetimes and oscillator strengths of astrophysical interest
The lifetimes of three short-lived levels belonging to the4f96p configuration and of two long-lived levels of the4f95d configuration of DyIII have been measured for the firsttime using time-resolved laser-induced fluorescence techniques. They arein good agreement with theoretical values calculated within theframework of a pseudo-relativistic configuration interactionapproximation. Using the experimental lifetimes and the theoreticalbranching fractions, a first set of transition probabilities ofastrophysical interest has been obtained for DyIII.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Theoretical Oscillator Strengths inPr III and Application to Some CP Stars
A set of transition probabilities is obtained for the first time formany transitions of Pr III of astrophysical interest. A relativisticHartree-Fock method, combined with a least-squares fitting of theavailable experimental levels, including a large number of newlydetermined values, has been used for the calculations in whichconfiguration interaction and core-polarization effects have beenintroduced. The interest of the new data set is illustrated byconsidering the chemical composition of the chemically peculiar (CP)stars HD 101065 (Przybylski's star) and HD 141556 (χ Lupi).
| Lifetime Measurements for Ground Term Transitions in TA II, W II, and RE II
Lifetime measurements have been made for the radiation emitted in theground term transitions of the nominal form5s^25p^65d^x6s-5s^25p^65d^x6p in Ta II (x=3), W II (x=4), and Re II(x=5). Supporting theoretical calculations have also been performed tocharacterize configuration interaction and to estimate the degree ofdecay branching of the upper levels. The lifetime measurements have beencombined with these theoretical considerations and with branchingfractions deduced from the emission measurements of Corliss & Bozmanto specify the oscillator strengths of these transitions. The resultsare discussed in the context of spectroscopic data obtained fromorbiting telescopes and applied to Hubble Space Telescope spectra toestimate the tungsten abundance in Sirius.
| A search for rapid oscillations in chemically peculiar A-type stars
In 1995 we initiated a Northern Hemisphere survey for rapidlyoscillating Ap stars. This paper presents the results including one newroAp star (HD 122970), the confirmation of rapid oscillations of HD99563 and apparent null results for other stars. Using Hipparcos data astatistical analysis of the absolute magnitudes and galacticdistributions of all known roAp and noAp stars (also taken from theliterature) was made. A systematic trend for most of the program starsin a M_{ V} vs. beta (index of the Strömgren uvbybeta system)diagram was detected leading to the conclusion that beta issystematically influenced by the chemical peculiarity and/or magneticfield. Three roAp stars are outside the delta Scuti instability stripwhich implies that the driving mechanism of the two classes of pulsatingstar is different. This is also suggested by new pulsation models. Nostatistical difference between the galactic distribution of roAp andnoAp stars was found.
| On the HIPPARCOS photometry of chemically peculiar B, A, and F stars
The 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 HR-diagram from HIPPARCOS data. Absolute magnitudes and kinematics of BP - AP stars
The HR-diagram of about 1000 Bp - Ap stars in the solar neighbourhoodhas been constructed using astrometric data from Hipparcos satellite aswell as photometric and radial velocity data. The LM method\cite{luri95,luri96} allows the use of proper motion and radial velocitydata in addition to the trigonometric parallaxes to obtain luminositycalibrations and improved distances estimates. Six types of Bp - Apstars have been examined: He-rich, He-weak, HgMn, Si, Si+ and SrCrEu.Most Bp - Ap stars lie on the main sequence occupying the whole width ofit (about 2 mag), just like normal stars in the same range of spectraltypes. Their kinematic behaviour is typical of thin disk stars youngerthan about 1 Gyr. A few stars found to be high above the galactic planeor to have a high velocity are briefly discussed. Based on data from theESA Hipparcos astrometry satellite and photometric data collected in theGeneva system at ESO, La Silla (Chile) and at Jungfraujoch andGornergrat Observatories (Switzerland). Tables 3 and 4 are onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The observed periods of AP and BP stars
A 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.
| The Cape rapidly oscillating AP star survey - III. Null results of searches for high-overtone pulsation.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1994MNRAS.271..129M&db_key=AST
| Catalogue of CP stars with references to short time scale variability
A catalogue was compiled which contains all references in the literaturesince 1962 related to variations of CP stars on time scales shorter thanthe rotation period. The role of this catalogue lies in the unbiasedlisting of all available references, and not in a critical evaluation.
| A new list of effective temperatures of chemically peculiar stars. II.
Not Available
| Some problems of non-reversive CP stars. I. Spatial distribution.
Not Available
| Wich is the Star V380 Per?
Not Available
| A seven-year northern sky survey of AP stars for rapid variability
A high-speed photometric survey of 120 Ap stars in the northern sky, hasbeen conducted, between 1985 and 1991, in order to search for rapidvariability. Stars of spectral types, namely from B8 to F4, have beenselected for the survey. The selected pulsational variable stars occupythe hotter regions of the instability strip of the Hertzsprung-Russeldiagram. Noted is the absence of pulsations in the hotter B8-A3 Apstars; this does not, however, preclude the existence of pulsations,since HD 218495 was recently discovered to be a rapidly oscillating Ap(roAp) star. The primary result of this study is that variouscombinations of photometric indices, while pointing towards roAp starshaving the characteristic signatures of cool, SrCrEu stars, still failto isolate the roAp phenomenon from similar nonpulsating Ap stars.Color-magnitude and color-color diagrams are presented in order tocomplete this survey.
| Teff and log g determinations for 25 CP stars from Hβ profiles.
Not Available
| On the origin of the statistical correlation between rotation periods and apparent radii for CP 2 stars
Apparent rotational velocities and rotation periods for CP 2 stars areused to study the 'apparent' radius distribution of R sin i. It impliesa distribution for the radii of CP 2 stars which is almost normal fortheir temperatures when compared to main sequence stars. However, astatistical correlation exists between rotation period P and R sin i. Itis argued that, at least in the case of silicon stars, neitherconservation of angular momentum on the main sequence, nor bias in themeasured v sin i values are able to induce a correlation of the observedstrength. Thus, one has to postulate either additional rotationalbraking depending statistically on R, or a detection bias dependingstatistically on i. It is shown that the correlation might be explainedin both ways and the implications of each possibility are discussed.
| Spectrum variability of the silicon AP star HD 192913
The metal lines in the spectrum of the silicon Ap star HD 192913 arefound to change with the photometric period. Many commonly found atomicspecies have lines which vary together in phase. The spectrum containslines of most of the doubly ionized rare earth elements.
| Radii and space orientation of the rotational axes of AP stars
The inclination of the rotation axis to the line of sight (i) has beendetermined for a carefully selected sample of Ap stars with reliablevalues of periods of rotation, and values of the stellar radius (R)times sin i have been compared with values of normal main-sequencestars. The findings that none of the obtained R x sin i values aresignificantly larger than the upper limit for the radius of a mainsequence stars and that the mean radius of Ap stars is close to thenormal main sequence value suggest that most Ap stars are main-sequenceobjects. The observed i distribution implies that the distribution ofthe rotational axes of Ap stars in space is random.
| A search for the age-dependency of AP star parameters
Some observational data of the sample of the magnetic chemicallypeculiar stars (MCP stars) are investigated statistically. For the MCPstars of spectral types later than A2, both the frequency distributionand the (R) sin i-values suggest the existence of a linear relationbetween stellar diameter and rotation period. The MCP stars of spectraltypes earlier than B9 show an overpopulation of small (R) sin i whichmay indicate the existence of a second group with smaller radius in thissample. The equatorially symmetric rotator is used as the magneticmodel. With respect to its temporal behavior, the effective magneticfield is separated into dipolar and quadrupolar contribution. Both signsof the axisymmetric quadrupole moment appear with equal frequency. Thedipole moment which produces the amplitude of the Beff(t) curve formsfor longer periods two groups which are separated by a distinct gap.Both of the groups exhibit magnetic fields which are the stronger thegreater the stellar radius is, contrary to what is expected forfrozen-in fields. The dominance of magnetic curves without polarityreversal for longer-period stars is in accordance with predictions ofthe dynamo theory.
| The Magnetic Fields and another Parameters of the Chemically Peculiar Stars - Part One
Not Available
| Statistical Investigation of Chemically Peculiar Stars - Part One - the Stars with Known Periods
Not Available
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| Csillagkép: | Perszeusz |
| Rektaszcenzió: | 04h03m10.86s |
| Deklináció: | +38°03'17.3" |
| Vizuális fényesség: | 7.835 |
| Távolság: | 144.928 parszek |
| RA sajátmozgás: | -9.8 |
| Dec sajátmozgás: | -1.1 |
| B-T magnitude: | 7.898 |
| V-T magnitude: | 7.841 |
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