J/A+A/588/A25 Post-AGB and CSPNe evolutionary models (Miller Bertolami, 2016)
New models for the evolution of post-asymptotic giant branch stars and central
stars of planetary nebulae.
Miller Bertolami M.M.
<Astron. Astrophys. 588, A25 (2016)>
=2016A&A...588A..25M 2016A&A...588A..25M (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Stars, giant ; Planetary nebulae
Keywords: stars: AGB and post-AGB - stars: low-mass - stars: evolution -
planetary nebulae: general
Abstract:
The post-asymptotic giant branch (AGB) phase is arguably one of the
least understood phases of the evolution of low- and intermediate-
mass stars. The two grids of models presently available are based on
outdated micro- and macrophysics and do not agree with each other.
Studies of the central stars of planetary nebulae (CSPNe) and post-AGB
stars in different stellar populations point to significant
discrepancies with the theoretical predictions of post-AGB models.
We study the timescales of post-AGB and CSPNe in the context of our
present understanding of the micro- and macrophysics of stars. We want
to assess whether new post-AGB models, based on the latter
improvements in TP-AGB modeling, can help us to understand the
discrepancies between observation and theory and within theory itself.
In addition, we aim to understand the impact of the previous AGB
evolution for post-AGB phases.
We computed a grid of post-AGB full evolutionary sequences that
include all previous evolutionary stages from the zero age main
sequence to the white dwarf phase. We computed models for initial
masses between 0.8 and 4M☉ and for a wide range of initial
metallicities (Z0= 0.02, 0.01, 0.001, 0.0001). This allowed us to
provide post-AGB timescales and properties for H-burning post-AGB
objects with masses in the relevant range for the formation of
planetary nebulae (∼0,5-0,8M☉). We included an updated treatment
of the constitutive microphysics and included an updated description
of the mixing processes and winds that play a key role during the
thermal pulses (TP) on the AGB phase.
Description:
We compute a grid of post-AGB full evolutionary sequences that are
derived from full evolutionary models which include all previous
evolutionary stages from the Zero Age Main Sequence to the White Dwarf
phase. Models are computed for initial masses between 0.8 and
4M☉ and for a wide range of initial metallicities. Two grids of
post-AGB models are provided. The main grid of 24 H-burning post-AGB
sequences corresponds to the sequences presented in table 3 of the
article. Each file contains all the sequences with a given initial
metallicity and are named as 0200_T03.dat, 0100_T03.dat 0010_T03.dat
and 0001_T03.dat (corresponding to metallicities Z=0.02, 0.01, 0.001
and 0.0001 in table 3).
The second grid corresponds to the sequences presented in Appendix B,
table B.2 (originally presented in Miller Bertolami, M. M. 2015, in
ASPCS, Vol. 493, 83) and are named as 0100_TB2.dat and 0010_TB2.dat
(corresponding to metallicities Z=0.01 and 0.001 in table B2)
All sequences are presented at equivalent evolutionary points to allow
easy interpolation:
Sequences are presented until their luminosity drops to 1 solar
luminosity or until a late helium flash develops.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 102 6 List of models
models/* . 6 *Individual files
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Note on models/*: Inside each file each sequence is started with a short header
(7 lines) indicating the nature of the model (post-AGB, H-burner),
composition and the initial and final masses of the original simulation.
Different evolutionary sequences are separated by 2 empty lines.
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- FileName Name of the table in subdirectory models
14-102 A89 --- Title Title of the table
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Byte-by-byte Description of file (#): models/*
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- N Track point number
7- 15 F9.6 [Lsun] logL logarithm of the stellar luminosity
17- 25 F9.6 [K] logTeff logarithm of the effective temperature
27- 35 F9.6 [cm/s2] logg logarithm of the surface gravity
40- 51 F12.4 yr t Age since the point at LogTeff=3.85
53- 61 F9.6 --- Menv Fractional mass of the envelope
63- 71 F9.6 Msun Mstar Total mass of the star
73- 82 F10.6 [Msun/yr] log(-dM/dt) Logarithm of the Mass Loss Rate,
log(-dMstar/dt)
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Acknowledgements:
Marcelo Miguel Miller Bertolami, marcelo(at)MPA-Garching.MPG.DE
(End) Patricia Vannier [CDS] 11-Jan-2016