Ýçindekiler
Görüntüler
Resim Yükleyin
DSS Images Other Images
Ýlgili Makaleler
Geneva photometry of the open cluster NGC 2451 and its exceptional Be star HR 2968 satellite.}
During many years, several authors discussed whether NGC2451 was a real open star cluster or not. By using parallaxesand proper motions from Hipparcos satellite, and Geneva multicolourphotometric measurements of 64 stars, the existence of two clusters Aand B is confirmed. Distances and Geneva colour excesses E[B-V] arerespectively 197 pc, 0.01 and 358 pc, 0.12 for NGC2451 A and B. The two clusters have the same age (log t =7.7). A unique Be star, HR 2968, which belongs tocluster B, has been monitored from 1978 to 1998 in Geneva photometry andfrom November 1989 to March 1993 by the Hipparcos satellite. This starshows exceptional luminosity variations: i) The mean luminosity, whichhas been stable since 1978 (normal B-star phase), increased from 1990 to1995 (Be phase), and then decreased until 1998; ii) Also, in 1990started a periodic light variation with a period of 371 d. Five periodsof this mid-term light variation were observed. Hipparcos and Genevaphotometries are in perfect agreement. A model is proposed to explainthis periodic variability: the Be star is the main component of a binarysystem having an eccentric orbit of period 371 d; from 1990, the Be starwas surrounded by matter expelled in its equatorial plane and, at eachperiastron passage, the companion star interacts gravitationally and/orradiatively with the disk. The physical parameters of the Be star andits companion (most probably a main sequence star) are determined byusing their belonging to NGC 2451 B and bycalculating an approximate orbit from published radial velocities. Themean values of the photometric data are only available in electronicform at the CDS via anonymous ftp to cdsarc.u.strasbg.fr (130.79.128.5)or via http://cdsweb.u-strasbg.fr/Abstract.html
| The ROSAT all-sky survey catalogue of optically bright late-type giants and supergiants
We present X-ray data for all late-type (A, F, G, K, M) giants andsupergiants (luminosity classes I to III-IV) listed in the Bright StarCatalogue that have been detected in the ROSAT all-sky survey.Altogether, our catalogue contains 450 entries of X-ray emitting evolvedlate-type stars, which corresponds to an average detection rate of about11.7 percent. The selection of the sample stars, the data analysis, thecriteria for an accepted match between star and X-ray source, and thedetermination of X-ray fluxes are described. Catalogue only available atCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Evolved GK stars near the Sun. 2: The young disk population
From a sample of nearly 2000 GK giants a group of young disk stars withwell determined space motions has been selected. The zero point of theluminosity calibrations, both from the ultraviolet flux (modifiedStroemgren system) and that in the region of 4200 to 4900 A (DDOsystem), show a discontinuity of about a half magnitude at the border ofthe young disk and old disk domains. The population separation is basedon the space velocity components, which are also an age discriminant,with the population interface near 2 x 109 yr, based onmodels with convective overshoot at the core. This age corresponds togiant masses near 1.7 solar mass, near the critical mass separating theyoung stars that do not burn helium in degenerate cores from older starsthat do. Ten percent of both populations show CN anomalies in that thederived value of P(Fe/H) from CN (Cm) and fromFe(M1) differ by more than 0.1 dex and the weak and strong CNstars occur equally in the old disk but the weak CN stars predominate inthe young disk. Peculiar stars, where flux distortions affect theluminosity calibrations, are of the CH+(Ba II) and CH-(weak G band)variety and represent less than 1% of the stars in both populations. Theyoung disk giants are restricted to ages greater than about109 yr, because younger stars are bright giants orsupergiants (luminosity class 2 or 1), and younger than about 2 x109 yr, because the old disk-young disk boundary occurs near1.7 solar mass. The distribution of heavy element abundances, P(Fe/H),for young disk giants is both more limited in range (+/- 0.4 dex) and isskewed toward higher abundances, compared with the nearly normaldistribution for old disk giants. The distribution of (U,V) velocityvectors gives (U,V,W) and their dispersions = (+17.6 +/- 18.4, -14.8 +/-8.4, -6.9 +/- 13.0) and (+3.6 +/- 38.4, -20.7 +/- 27.5, -6.7 +/-17.3)km/s for young and old disk giants, respectively.
| NGC 2451 - What is it?
During the last decade, a debate has arisen whether the grouping ofstars called NGC 2451 is a real star cluster. We investigate thecorresponding area of the sky kinematically, using proper motions of thePPM catalogue. The group of stars that was originally called NGC 2451shows a large scatter of their proper motions, which proves that they donot form a cluster. However, close-by we find a group of 24 PPM starswith common proper motion. A colour-magnitude diagram of 19 of theseshows an extremely well-defined main sequence, giving a distance ofabout 220 pc. This cluster is not NGC 2451. We tentatively call itPuppis Moving Group (PMG). There is strong indication for a secondcluster at about 400 pc. Photometry, radial velocities and propermotions of stars fainter than the magnitude limit of PPM are needed tofurther investigate the matter.
| Large and kinematically unbiased samples of G- and K-type stars. IV - Evolved stars of the old disk population
Modified Stromgren and (R,I) photometry, along with DDO and Genevaphotometry, are presented for a complete sample of evolved old-disk Gand K giants in the Bright Star Catalogue. Stars with ages of between1.5 x 10 to the 9th and 10 to the 10th yr are found to have anear-normal distribution of heavy element abundances, centered on anFe/H abundance ratio of -0.1 dex. The old disk clusters NGC 3680 and IC4651 contain red-straggler young-disk giants that are probablycontemporaries of the blue stragglers in the clusters.
| Large and kinematically unbiased samples of G- and K-type stars. II - Observations of evolved stars in the Bright Star sample. III - Evolved young disk stars in the Bright Star sample
Four color and RI observations were obtained for a large sample ofG-type and K-type stars in the Bright Star Catalogue. Data are firstpresented for 110 evolved stars. Photometry of evolved young diskpopulation stars have then been calibrated for luminosity, reddening,and metallicity on the basis of results for members of the Hyades andSirius superclusters. New DDO results are given for 120 stars.
| Membership and photometric abundances of red evolved stars in open clusters
UBV and DDO photometric observations of 31 red evolved stars toward 11open clusters, obtained with the 41-cm and 91-cm telescopes at CerroTololo Interamerican Observatory on four nights in 1978, are reported.The data are compiled in tables and characterized for each cluster, andtwo criteria are used to determine the probability that a star is amember of a cluster. Six of the clusters are found to contain oneevolved red star, one has two, one has four, and three have none; theother 19 stars are seen as red field objects. The estimated cluster Fe/Habundance ratios range from -0.2 to +0.3, and the red giants in theclusters NGC 2335 and NGC 2567 are found to have CN strengths like thoseseen in Hyades giants. The unusual weakness of the 421.6-nm band of CNfor star 108 in NGC 2548 is attributed either to unusual composition andproper motion or to its nonmembership in the cluster despite meeting thephotometric criteria.
| Radial velocities of southern stars obtained with the photoelectric scanner CORAVEL. III - 790 late-type bright stars
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1985A&AS...59...15A&db_key=AST
| DDO photometry on red giants in the open clusters NGC 2232, NGC 2287, and NGC 2451
From DDO photometry combined with U, B, V photometry of red stars in theopen clusters NGC 2232, NGC 2287, and NGC 2451, the mean color excess E(B-V), the distance modulus, and the mean metal abundance (Fe/H) werederived for the clusters. The physical parameters, surface gravity,effective temperature, and spectral type were also obtained for the redstars. Estimation of age yielded 1.1 x 10 to the 8th yr for NGC 2287,and for NGC 2451, 4.8 x 10 to the 8th. The cluster NGC 2232 should beolder than 10 to the 9th yr.
| Photoelectric Photometry of NGC 2451
Not Available
|
Yeni bir Makale Öner
Ýlgili Baðlantýlar
Yeni Bir Baðlantý Öner
sonraki gruplarýn üyesi:
|
Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Pupa |
| Sað Açýklýk: | 07h43m07.00s |
| Yükselim: | -38°51'51.0" |
| Görünürdeki Parlaklýk: | 6.89 |
| Uzaklýk: | 355.872 parsek |
| özdevim Sað Açýklýk: | -13.5 |
| özdevim Yükselim: | 4.1 |
| B-T magnitude: | 8.177 |
| V-T magnitude: | 6.996 |
Kataloglar ve belirtme:
|
INHABITED SKY
