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The initial–final mass relationship of white dwarfs revisited: effect on the luminosity function and mass distribution
The initial-final mass relationship connects the mass of a white dwarf with the mass of its progenitor in the main-sequence. Although this function is of fundamental importance to several fields inExpand
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The Cooling of CO White Dwarfs: Influence of the Internal Chemical Distribution
White dwarfs are the remnants of stars of low and intermediate masses on the main sequence. Since they have exhausted all of their nuclear fuel, their evolution is just a gravothermal process. TheExpand
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New cooling sequences for old white dwarfs
We present full evolutionary calculations appropriate for the study of hydrogen-rich DA white dwarfs. This is done by evolving white dwarf progenitors from the zero-age main sequence, through theExpand
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High-resolution smoothed particle hydrodynamics simulations of the merger of binary white dwarfs
Context. The coalescence of two white dwarfs is the final outcome of a sizeable fraction of binary stellar systems. Moreover, this process has been proposed to explain several interestingExpand
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The age and colors of massive white dwarf stars
We present evolutionary calculations and colors for massive white dwarfs with oxygen-neon cores for masses between 1.06 and 1.28 Mo. The evolutionary stages computed cover the luminosity range fromExpand
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Evolutionary and pulsational properties of white dwarf stars
White dwarf stars are the final evolutionary stage of the vast majority of stars, including our Sun. Since the coolest white dwarfs are very old objects, the present population of white dwarfsExpand
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Mass-radius relations for massive white dwarf stars
We present detailed theoretical mass-radius relations for massive white dwarf stars with oxygen-neon cores. This work is motivated by recent observational evidence about the existence of white dwarfExpand
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The Ages of Very Cool Hydrogen-rich White Dwarfs
The evolution of white dwarfs is essentially a cooling process that depends primarily on the energy stored in their degenerate cores and on the transparency of their envelopes. In this paper weExpand
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On the Evolution of Stars that Form Electron-Degenerate Cores Processed by Carbon Burning. III. The Inward Propagation of a Carbon-Burning Flame and Other Properties of a 9 M☉ Model Star
A 9 M☉ stellar model of Population I composition is evolved from the hydrogen-burning main sequence to the thermally pulsing "super" asymptotic giant branch stage, where it has an electron-degenerateExpand
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