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dc.date.accessioned 2019-11-27T17:50:11Z
dc.date.available 2019-11-27T17:50:11Z
dc.date.issued 2016
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/86208
dc.description.abstract Context. GW Virginis stars are a well-studied class of nonradial g-mode pulsators. SDSS J0349-0059 and VV 47 are two PG 1159 star members of this class of variable stars. SDSS J0349-0059 is an interesting GW Vir star that shows a complete pulsation spectrum that includes rotational splitting of some of its frequencies. VV 47 is a pulsating PG 1159 star surrounded by a planetary nebula. This star is particularly interesting because it exhibits a rich and complex pulsation spectrum. Aims. We present an asteroseismological study of SDSS J0349-0059 and VV 47 aimed mainly at deriving their total mass on the basis of state-of-the-art PG 1159 evolutionary models. Methods. We computed adiabatic nonradial g-mode pulsation periods for PG 1159 evolutionary models with stellar masses ranging from 0:515 to 0:741 M, that take into account the complete evolution of the progenitor stars. We first estimated a mean period spacing for both SDSS J0349-0059 and VV 47 and then constrained the stellar mass of these stars by comparing the observed period spacing with the asymptotic period spacing and with the average of the computed period spacings. We also employed the individual observed periods to search for a representative seismological model for each star. Finally, we estimated the rotation period of SDSS J0349-0059. Results. We found a spectroscopic mass of M 0:543 M- for SDSS J0349-0059 and M 0:529 M for VV 47. By comparing the observed period spacing with the asymptotic period spacing, we obtain M 0:569 M for SDSS J0349-0059 and M 0:523 M for VV 47. When we compare the observed period spacing with the average of the computed period spacings, we find M0:535 M for SDSS J0349-0059 and M 0:528 M for VV 47. Searching for the best period fit, we found for SDSS J0349-0059 an asteroseismological model with M = 0:542 M and Tt = 91 255 K. For VV 47, we were unable to find a unique and unambiguous asteroseismological model. Finally, for SDSS J0349-0059, we determined the rotation period to be Prot = 1= 0:407 days. Conclusions. The results presented in this work constitute a further step in the study of GW Vir stars through asteroseismology in the frame of fully evolutionary models of PG 1159 stars. In particular, the potential of asteroseismology to derive stellar masses of PG 1159 stars with an unprecedented precision is shown yet again. en
dc.language en es
dc.subject Stars: evolution es
dc.subject Stars: interiors es
dc.subject Stars: oscillations es
dc.subject White dwarfs es
dc.title Asteroseismology of the GW Virginis stars SDSS J0349-0059 and VV 47 en
dc.type Articulo es
sedici.identifier.other doi:10.1051/0004-6361/201527996 es
sedici.identifier.other eid:2-s2.0-84964727723 es
sedici.identifier.issn 0004-6361 es
sedici.creator.person Calcaferro, Leila Magdalena es
sedici.creator.person Córsico, Alejandro Hugo es
sedici.creator.person Althaus, Leandro Gabriel es
sedici.subject.materias Ciencias Astronómicas es
sedici.description.fulltext true es
mods.originInfo.place Instituto de Astrofísica de La Plata es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
sedici.subtype Articulo es
sedici.rights.license Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
sedici.rights.uri http://creativecommons.org/licenses/by-nc-sa/4.0/
sedici.description.peerReview peer-review es
sedici.relation.journalTitle Astronomy and Astrophysics es
sedici.relation.journalVolumeAndIssue vol. 589 es
sedici.rights.sherpa * Color: green * Pre-print del autor: can * Post-print del autor: can * Versión de editor/PDF:can * Condiciones: >>On author's personal website or institutional website or OAI compliant website >>Some journals require an embargo for deposit in funder's designated repositories (see journal) >>Publisher's version/PDF may be used (see journal) >>Must link to publisher version >>Publisher copyright and source must be acknowledged >>Non-commercial * Link a Sherpa: http://sherpa.ac.uk/romeo/issn/0004-6361/es/


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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) Excepto donde se diga explícitamente, este item se publica bajo la siguiente licencia Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)