ADC/CDS Standard Document for Catalog:/journal_tables/ApJS/92/125/
ADC/CDS Standard Document for Catalog:| 1. Use the ADC Data Viewer Suite to visualize the data. |
|
| 2. Get the data files via anonymous FTP. (See Note.) |
|
J/ApJS/92/125 Post-AGB evolution (Vassiliadis+, 1994)
================================================================================
Post-asymptotic giant branch evolution of low- to intermediate-mass stars
Vassiliadis E., Wood P.R.
<Astrophys. J. Suppl. Ser. 92, 125 (1994)>
=1994ApJS...92..125V (SIMBAD/NED Reference)
================================================================================
ADC_Keywords: Models, evolutionary; Mass loss; Nebulae, planetary
Keywords: Magellanic Clouds - planetary nebulae: general - stars: evolution -
stars: interiors
Abstract:
In this paper, we present the results for the post-AGB phases of
stellar evolutionary sequences, complete from the main-sequence phase,
through the AGB phase, and on into the planetary nebula and white
dwarf regimes. Mass loss has been included using an empirical
formalism derived from observed mass-loss rates of planetary nebula
nuclei available in the literature and from radiation-pressure-driven
stellar wind theory. Models are calculated for initial masses 0.89,
0.95, 1.0, 1.5, 2.0, 2.5, 3.5, and 5.0M_{sun}_, and metallicities
0.016, 0.008, 0.004, and 0.001. These abundance and mass values were
chosen to allow comparison with Galactic, and Magellanic Cloud planetary
nebulae and their nuclei. The post-AGB evolutionary sequences fall
into two distinct groups depending on when the planetary nebula nuclei
leave the AGB: one group where helium-shell burning is dominant, and
the other group where hydrogen-shell burning is dominant. Of the 27
computed sequences: 17 are hydrogen-burners, and 10 are helium-burners.
In only five cases was any effort made to control the phase of departure
from the AGB. Lower mass models are more likely to leave the AGB burning
helium, as the preceding AGB evolution has a mass-loss rate which is
greatest immediately prior to a helium-shell flash. The calculations
are compared with the large observational database that has developed
over recent years for the Large Magellanic Cloud. These calculations
will be useful for determining the planetary nebula luminosity function,
and for the study of the ultraviolet excess observed in elliptical
galaxies.
Addresses:
Vassiliadis E.
Mount Stromlo and Siding Spring Observatories, Institute of Advanced
Studies, The Australian National Observatory, Private Bag,
Weston Creek P.O., A.C.T. 2611, Australia
Wood P.R.
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore,
MD 21218
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table.tex 87 1014 LaTeX version of the tables
table3.dat 41 720 H-Burning PNN Evolutionary Models
table4.dat 41 401 He-Burning PNN Evolutionary Models
table5.dat 41 45 H-Like He-Burning PNN Evolutionary Model
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat table4.dat table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.2 solMass M Initial, main-sequence mass
6- 9 F4.2 solMass Y Y index (always 25)
11- 15 F5.3 solMass Z Metallicity
17- 26 F10.1 yr Time Time. Taken to be zero at log Teff = 4.
29- 33 F5.3 K log(Teff) Effective temperature
36- 41 F6.3 solLum log(L) Luminosity
--------------------------------------------------------------------------------
Origin: AAS CD-ROM series, Volume 2, 1994
================================================================================
(End) Lee Brotzman [ADS] 12-May-94, Patricia Bauer [CDS] 03-Nov-1994