most citedThe initial-final mass relationship from white dwarfs in common proper motion pairs

86 citations · 184 across the 4 of their papers we have counts for

collaborators

8 papers

astro-ph200758 cited

Gravitational settling of 22Ne and white dwarf evolution

E. García--Berro, L. G. Althaus, A. H. Córsico +1

We study the effects of the sedimentation of the trace element 22Ne in the cooling of white dwarfs. In contrast with previous studies, which adopted a simplified treatment of the e…

astro-ph200718 cited

WD0433+270: an old Hyades stream member or an Fe-core white dwarf?

S. Catalan, I. Ribas, J. Isern +1

G39-27/289 is a common proper motion pair formed by a white dwarf (WD0433+270) and a main-sequence star (BD+26 730) that apparently has been classified as a member of the Hyades op…

astro-ph200786 cited

The initial-final mass relationship from white dwarfs in common proper motion pairs

S. Catalan, J. Isern, E. Garcia-Berro +3

The initial-final mass relationship of white dwarfs, which is poorly constrained, is of paramount importance for different aspects in modern astrophysics. From an observational per…

astro-ph200722 cited

Evidence for a merger of binary white dwarfs: the case of GD 362

E. Garcia-Berro, P. Loren-Aguilar, A. G. Pedemonte +4

GD 362 is a massive white dwarf with a spectrum suggesting a H-rich atmosphere which also shows very high abundances of Ca, Mg, Fe and other metals. However, for pure H-atmospheres…

gr-qc2005

The variation of the gravitational constant inferred from the Hubble diagram of Type Ia supernovae

E. Garcia-Berro, Yu. A. Kubyshin, P. Loren-Aguilar +1

We consider a cosmological model with a variable gravitational constant, G, based on a scalar-tensor theory. Using the recent observational data for the Hubble diagram of type Ia s…

astro-ph2004

Pulsations of massive ZZ Ceti stars with carbon/oxygen and oxygen/neon cores

A. H. Corsico, E. Garcia-Berro, L. G. Althaus +1

We explore the adiabatic pulsational properties of massive white dwarf stars with hydrogen-rich envelopes and oxygen/neon and carbon/oxygen cores. To this end, we compute the cooli…