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From Planetary Nebula nuclei to white dwarfs: The impact of evolutionary envelope masses

Published online by Cambridge University Press:  25 May 2016

T. Blöcker ,
F. Herwig ,
T. Driebe ,
H. Bramkamp  and
D. Schönberner
T. Blöcker
Affiliation:
1Institut für Astronomie und Astrophysik, 24098 Kiel, Germany
F. Herwig
Affiliation:
2Astrophysikalisches Institut Potsdam, 14473 Potsdam, Germany
T. Driebe
Affiliation:
2Astrophysikalisches Institut Potsdam, 14473 Potsdam, Germany
H. Bramkamp
Affiliation:
2Astrophysikalisches Institut Potsdam, 14473 Potsdam, Germany
D. Schönberner
Affiliation:
2Astrophysikalisches Institut Potsdam, 14473 Potsdam, Germany

Extract

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It is well known that the evolution of white dwarfs (WDs) depends sensitively on the question whether they have “thin” or “thick” envelopes of H and He (see Wood 1995). Standard evolutionary caluclations (e.g. Paczynksi 1971) show that at the tip of the Asymptotic Giant Branch the envelope masses are tightly correlated with the mass of the hydrogen exhausted core (≈ total mass). Accordingly, the masses of hydrogen, M H, and helium, M He, on top of the degenerate C/O interiors decrease by orders of magnitudes with increasing stellar mass. In contrast, many applications of WD calculations consider only single values of q H,He = log(M H,He/M ∗) asuming either “thick” or “thin” envelopes.

Type
VI. From Planetary Nebulae to White Dwarfs
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 389
Copyright
Copyright © Kluwer 1997 

References

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