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Titolo:
Non-linear radiative models of post-AGB stars: Application to HD 56126
Autore:
Fokin, AB; Lebre, A; Le Coroller, H; Gillet, D;
Indirizzi:
Russian Acad Sci, Inst Astron, Moscow 109017, Russia Russian Acad Sci Moscow Russia 109017 Inst Astron, Moscow 109017, Russia Univ Montpellier 2, CNRS, ISTEEM, UMR 5024,Grp Rech Astron & Astrophys Languedoc, F-34095 Montpellier 05, France Univ Montpellier 2 Montpellier France 05 F-34095 Montpellier 05, France CNRS, Observ Haute Provence, F-04870 St Michel, France CNRS St Michel France F-04870 Haute Provence, F-04870 St Michel, France
Titolo Testata:
ASTRONOMY & ASTROPHYSICS
fascicolo: 2, volume: 378, anno: 2001,
pagine: 546 - 555
SICI:
1432-0746(200111)378:2<546:NRMOPS>2.0.ZU;2-1
Fonte:
ISI
Lingua:
ENG
Soggetto:
RV TAURI STARS; PROTOPLANETARY NEBULAE; NONLINEAR PULSATIONS; MASS STARS; VARIABLES; OPACITIES; SAO-96709; OBJECTS;
Keywords:
stars : atmospheres; stars : AGB and post-AGB; line : profiles; stars : oscillations; stars : fundamental parameters; stars : individual : HD 56126;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
36
Recensione:
Indirizzi per estratti:
Indirizzo: Lebre, A Russian Acad Sci, Inst Astron, 48 Pjatnitskaya Str, Moscow 109017, Russia Russian Acad Sci 48 Pjatnitskaya Str Moscow Russia 109017 Russia
Citazione:
A.B. Fokin et al., "Non-linear radiative models of post-AGB stars: Application to HD 56126", ASTRON ASTR, 378(2), 2001, pp. 546-555

Abstract

In order to study in a general manner the pulsations of the post-AGB starswe performed a grid of non-linear radiative low-mass, high-luminosity models in a wide range of T-eff, L and M. Theoretical bolometric light curves and radial velocity curves were computed as well as their associated power spectra. We have also examined the behaviour of these models according to the stellar mass, the chemical composition and the opacity tables we have used in the code. Concerning the carbon rich post-AGB star HD 56126, the models best found to fit its observational characteristics are X = 0.7, Z = 0.004, M = 0.8M., L = 6000-7000 L. and T-eff less than or equal to 5850 K. Models computed with smaller mass fail to reproduce both the period and the pulsational amplitude of HD 56126, which is quite different from the pulsational amplitude of the RV Tauri stars. The previously analysed spectroscopic and photometric variations of HD 56126 appear to be consistent with a non-regular radial pulsation where the dominant pulsation mode is the first overtone. In the course of the pulsation, moderate shock waves are repeatedly generated and they propagate throughout the stellar atmosphere. They provoke a complex, asynchronous motion of the outer layers.

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Documento generato il 01/04/20 alle ore 11:32:54