Theoretical mass-radius relations for massive white dwarfs with oxygen-neon cores and stellar masses from 1.06 to 1.30 Msun, and described in Althaus, García-Berro , Isern at al. 2005, A&A, 441, 689, are provided. Our cooling sequences are based on evolutionary calculations that take into account the chemical composition expected from massive white dwarf progenitors that burned carbon in partially degenerate conditions. Thus, an oxygen-neon composition is expected in the core of our massive white dwarfs. Each cooling track file lists from left to right:
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The logarithm of the surface luminosity in solar unit |
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The logarithm of the effective temperature (K) |
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The logarithm of stellar radius (cm) |
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The logarithm of surface gravity (cm/s2) |
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Stellar mass (solar unit) |
All the evolutionary sequences have the same core composition and shell profile. In particular, the chemical abundance distribution is displayed in the figure below