2019
DOI: 10.1134/s1063773719080024
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Evolution and Pulsations of Population I Post-AGB Stars

Abstract: Evolutionary calculations of population I stars with initial masses M 0 = 1M ⊙ , 1.5M ⊙ and 2M ⊙ were carried out up to the stage of the proto-planetary nebula. Selected models of post-AGB evolutionary sequences with effective temperatures 3.6 × 10 3 K T eff 2 × 10 4 K were used as initial conditions in calculations of self-escited stellar oscillations. For the first time the sequences of hydrodynamic models of radially pulsating post-AGB stars were computed using the self-consistent solution of the equations … Show more

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Cited by 7 publications
(5 citation statements)
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“…As in our preceding work on pulsating post-AGB stars (Fadeyev 2019 , 1998, 2009). If we assume that FG Sge is on the stage of its maximum radius then its mass, radius and effective temperature are M = 0.565M ⊙ , R = 126R ⊙ and T eff = 4445 K, respectively.…”
Section: Results Of Stellar Pulsation Calculationsmentioning
confidence: 73%
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“…As in our preceding work on pulsating post-AGB stars (Fadeyev 2019 , 1998, 2009). If we assume that FG Sge is on the stage of its maximum radius then its mass, radius and effective temperature are M = 0.565M ⊙ , R = 126R ⊙ and T eff = 4445 K, respectively.…”
Section: Results Of Stellar Pulsation Calculationsmentioning
confidence: 73%
“…The mean period change rate evaluated in the present study Π = 0.96 day/yr is more than three times smaller than that of FG Sge: Π = 3.32 day/yr. Taking into account the growth of post-AGB evolution rate with increasing stellar mass (Miller Bertolami, 2016;Fadeyev, 2019) one can suppose that better agreement between the theory and observations could be obtained with somewhat higher mass of the post-AGB star undergoing the final helium flash. A possible solution of this problem could be found on the base of more extensive grid of evolutionary tracks computed with various assumptions on the mass loss rates during the stage of red giant before AGB as well as during the AGB stage.…”
Section: Results Of Stellar Pulsation Calculationsmentioning
confidence: 99%
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“…In Fig.1they are marked by filled circles as 1 and 2. As seen from Fig.3, nonlinear oscillations of RU Cam before significant decrease of the oscillation amplitude are somewhat irregular which is a typical feature of pulsating post-AGB stars(Fadeyev 2019b).…”
mentioning
confidence: 81%
“…The goal of the present study is to establish evolutionary status of W Vir pulsating variables on the basis of consistent stellar evolution and nonlinear stellar pulsation calculations. Methods of the solution are discussed in our earlier papers devoted to studies of classical Cepheids (Fadeyev 2018) and post-AGB stars (Fadeyev 2019a(Fadeyev , 2019b.…”
Section: Introductionmentioning
confidence: 99%