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Astron. Astrophys. 339, 123-133 (1998)

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The evolution of helium white dwarfs

I. The companion of the millisecond pulsar PSR J1012+5307 *

T. Driebe 1, 2, D. Schönberner 2, T. Blöcker 1, 3 and F. Herwig 2

1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53321 Bonn, Germany (driebe@speckle.mpifr-bonn.mpg.de; bloecker@speckle.mpifr-bonn.mpg.de)
2 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany (deschoenberner@aip.de; fherwig@aip.de)
3 Institut für Theoretische Physik und Astrophysik, Universität Kiel, D-24098 Kiel, Germany

Received 6 February 1998 / Accepted 8 July 1998


We present a grid of evolutionary tracks for low-mass white dwarfs with helium cores in the mass range from 0.179 to [FORMULA]. The lower mass limit is well-suited for comparison with white dwarf companions of millisecond pulsars. The tracks are based on a [FORMULA] model sequence extending from the pre-main sequence stage up to the tip of the red-giant branch. Applying large mass loss rates at appropriate positions forced the models to move off the giant branch. The further evolution was then followed across the Hertzsprung-Russell diagram and down the cooling branch. At maximum effective temperature the envelope masses above the helium cores increase from 0.6 to [FORMULA] for decreasing mass. We carefully checked for the occurrence of thermal instabilities of the hydrogen shell by adjusting the computational time steps accordingly. Hydrogen flashes have been found to take place only in the mass interval [FORMULA].

The models show that hydrogen shell burning contributes significantly to the luminosity budget of white dwarfs with helium cores. For very low masses the hydrogen shell luminosity remains to be dominant even down to effective temperatures well below [FORMULA]. Accordingly, the corresponding cooling ages are significantly larger than those gained from model calculations which neglect nuclear burning or the white dwarf progenitor evolution.

Using the atmospheric parameters of the white dwarf in the PSR J1012+5307 system we determined a mass of [FORMULA] and a cooling age of [FORMULA], in good agreement with the spin-down age, 7 Gyr, of the pulsar.

Key words: stars: evolution – stars: interiors – white dwarfs – binaries: general – pulsars: individual: PSR J1012+5307

* Tables 5-11 are only available in electronic form at the CDS via ftp

Send offprint requests to: T. Driebe

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© European Southern Observatory (ESO) 1998

Online publication: September 30, 1998