• Publications
  • Influence
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 in
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. The
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 from
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 interesting
Cobalt-56 γ-ray emission lines from the type Ia supernova 2014J
The observed γ-ray properties are in broad agreement with the canonical model of an explosion of a white dwarf just massive enough to be unstable to gravitational collapse, but do not exclude merger scenarios that fuse comparable amounts of 56Ni.
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 dwarfs
s-Process nucleosynthesis in carbon stars
We present the first detailed and homogeneous analysis of the s-element content in Galactic carbon stars of N type. Abundances of Sr, Y, Zr (low-mass s-elements, or ls), Ba, La, Nd, Sm, and Ce
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 dwarf
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 we
The initial-final mass relationship from white dwarfs in common proper motion pairs
Context. The initial-final mass relationship of white dwarfs, which is poorly constrained, is of paramount importance for different aspects of modern astrophysics. From an observational perspective,