@article{DriebeBloeckerHerwigetal.1998,
  author    = {Driebe, Thomas and Bl{\"o}cker, Thomas and Herwig, Falk and Sch{\"o}nberner, Detlef},
  title     = {Diffusive overshooting in hot bottom burning AGB models},
  year      = {1998},
  language  = {en}
}
@article{DriebeSchoenbernerBloeckeretal.1998,
  author    = {Driebe, Thomas and Sch{\"o}nberner, Detlef and Bl{\"o}cker, Thomas and Herwig, Falk},
  title     = {The evolution of helium white dwarfs : I. the companion of the millisecond pular PSR J1012+5307},
  year      = {1998},
  language  = {en}
}
@article{HerwigSchoenbernerBloecker1998,
  author    = {Herwig, Falk and Sch{\"o}nberner, Detlef and Bl{\"o}cker, Thomas},
  title     = {On the validity of the core-mass luminosity relation for TP-AGB stars with efficient dredge-up},
  year      = {1998},
  language  = {en}
}
@article{HerwigBloecker1999,
  author    = {Herwig, Falk and Bl{\"o}cker, Thomas},
  title     = {Overshoot in giant stars},
  year      = {1999},
  language  = {en}
}
@article{DriebeBloeckerSchoenberneretal.1999,
  author    = {Driebe, Thomas and Bl{\"o}cker, Thomas and Sch{\"o}nberner, Detlef and Herwig, Falk},
  title     = {The evolution of helium white dwarfs : II. Thermal instabilities},
  year      = {1999},
  abstract  = {We calculated a grid of evolutionary models for white dwarfs with helium cores (He-WDs) and investigated the occurrence of hydrogen-shell flashes due to unstable hydrogen burning via CNO cycling. Our calculations show that such thermal instabilities are restricted to a certain mass range (M approx 0.21 ... 0.30 Msun), consistent with earlier studies. Models within this mass range undergo the more hydrogen shell flashes the less massive they are. This is caused by the strong dependence of the envelope mass on the white dwarf core mass. The maximum luminosities from hydrogen burning during the flashes are of the order of 105 Lsun. Because of the development of a pulse-driven convection zone whose upper boundary temporarily reaches the surface layers, the envelope's hydrogen content decreases by Delta X approx 0.06 per flash. Our study further shows that an additional high mass-loss episode during a flash-driven Roche lobe overflow to the white dwarf's companion does not affect the final cooling behaviour of the models. Independent of hydrogen shell flashes the evolution along the final white dwarf cooling branch is determined by hydrogen burning via pp-reactions down to effective temperatures as low as approx 8000 K.},
  language  = {en}
}
@article{HerwigBloeckerSchoenberner1999,
  author    = {Herwig, Falk and Bl{\"o}cker, Thomas and Sch{\"o}nberner, Detlef},
  title     = {The role of convective boundaries},
  year      = {1999},
  language  = {en}
}
@article{HerwigSchoenbernerBloecker1999,
  author    = {Herwig, Falk and Sch{\"o}nberner, Detlef and Bl{\"o}cker, Thomas},
  title     = {Violation of the Core Mass - Luminosity relation for AGB models wich experience the thord dredge-up},
  year      = {1999},
  language  = {en}
}
@article{BloeckerDriebeHerwig1999,
  author    = {Bl{\"o}cker, Thomas and Driebe, Thomas and Herwig, Falk},
  title     = {AGB evolution with overshoot : hot bootom burning vs. dredge-up},
  year      = {1999},
  language  = {en}
}
@article{HerwigBloeckerLangeretal.1999,
  author    = {Herwig, Falk and Bl{\"o}cker, Thomas and Langer, Norbert and Driebe, Thomas},
  title     = {On the formation of hydrogen-deficient post-AGB stars},
  year      = {1999},
  abstract  = {We present an evolutionary sequence of a low mass star from the Asymtotic Giant Branch (AGB) through its post- AGB stage, during which its surface chemical composition changes from hydrogen-rich to strongly hydrogen-deficient as consequence of a very late thermal pulse, following the so-called born-again scenario. The internal structure and abundance changes during this pulse are computed with a \%newly developed numerical method which allows the physically consistent calculation of stellar layers where thermonuclear and mixing time scale are comparable --- a situation which occurs when the helium flash driven convection zone extends to the hydrogen-rich surface layers during the pulse peak. The final surface mass fractions are [He/C/O]=[0.38/0.36/0.22], where the high oxygen abundance is due to diffusive overshoot employed during the AGB evolution. These models are the first to achieve general agreement with the surface abundance pattern observed in hydrogen-deficient post-AGB stars --- e.g. the PG 1159 stars or the WR-type central stars of planetary nebulae ---, confirming the born-again scenario with a physically consistent calculation and supporting the occurrence of convective overshooting in thermally pulsing AGB stars.},
  language  = {en}
}