The Initial-Final Mass Relationship From White Dwarfs In Common Proper Motion Pairs

dc.contributor.utaustinauthorPrieto, C. A.en_US
dc.creatorCatalan, S.en_US
dc.creatorIserns, J.en_US
dc.creatorGarcia-Berros, E.en_US
dc.creatorRibas, I.en_US
dc.creatorPrieto, C. A.en_US
dc.creatorBonanoss, A. Z.en_US
dc.date.accessioned2016-04-22T19:44:13Z
dc.date.available2016-04-22T19:44:13Z
dc.date.issued2008-01en
dc.description.abstractContext. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of paramount importance for different aspects of modern astrophysics. From an observational perspective, most of the studies up to now have been done using white dwarfs in open clusters. Aims. In order to improve the initial-final mass relationship, we explore the possibility of deriving a semi-empirical relation studying white dwarf's in common proper motion pairs. If these systems are comprised of a white dwarf and a FGK star, the total age and the metallicity of the progenitor of the white dwarf can be inferred from the detailed analysis of the companion. Methods. We have performed an exhaustive search for common proper motion pairs containing a DA white dwarf and a FGK star using the available literature and crossing the SIMBAD database with the Villanova White Dwarf Catalog. We have acquired long-slit spectra of the white dwarf members of the selected common proper motion pairs, as well as high resolution spectra of their companions. From these observations, a full analysis of the two members of each common proper motion pair leads to the initial and final masses of the white dwarfs. Results. These observations have allowed us to provide updated information for the white dwarfs, since some of them were misclassified. In the case of the DA white dwarfs, their atmospheric parameters, masses, and cooling times have been derived using appropriate white dwarf models and cooling sequences. From a detailed analysis of the FGK star spectra we have inferred the metallicity. Then, using either isochrones or X-ray luminosities we have obtained the main-sequence lifetime of the progenitors, and subsequently their initial masses. Conclusions. This work is the first one using common proper motion pairs to improve the initial-final mass relationship, and has also allowed us to cover the poorly explored low-mass domain. As in the case of studies based on white dwarfs in open clusters, the distribution of the semi-empirical data presents a large scatter, which is higher than the expected uncertainties in the derived values. This suggests that the initial-final mass relationship may not be a single-valued function.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipNASA NAG5-13057, NAG5-13147en_US
dc.description.sponsorshipMEC AYA05–08013–C03–01en_US
dc.description.sponsorshipEuropean Unionen_US
dc.description.sponsorshipAGAURen_US
dc.identifierdoi:10.15781/T2DB88
dc.identifier.citationCatalan, Silvia, J. Isern, E. García-Berro, I. Ribas, C. Allende Prieto, and A. Z. Bonanos. >The initial-final mass relationship from white dwarfs in common proper motion pairs.> Astronomy & Astrophysics, Vol. 477, No. 1 (Jan., 2008): 213-221.en_US
dc.identifier.doi10.1051/0004-6361:20078111en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/2152/34328
dc.language.isoEnglishen_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectstars : evolutionen_US
dc.subjectstars : white dwarfsen_US
dc.subjectopen clusters and associationsen_US
dc.subject: individual : common proper motion pairsen_US
dc.subjectbinaries : visualen_US
dc.subjectgravitational redshift determinationsen_US
dc.subjectblanketed model atmospheresen_US
dc.subjectbolometric correctionsen_US
dc.subjectspectroscopic surveyen_US
dc.subjectrotation velocitiesen_US
dc.subjecttemperature scaleen_US
dc.subjectbinary-systemsen_US
dc.subjectgalactic disken_US
dc.subjectnearby starsen_US
dc.subjectopen-clusteren_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Initial-Final Mass Relationship From White Dwarfs In Common Proper Motion Pairsen_US
dc.typeArticleen_US

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