White dwarfs are a class of stars with unique physical properties. They present many
challenging problems whose solution requires advanced theories of dense matter, state-of …

We present a critical review of the determination of fundamental parameters of white dwarfs
discovered by the Gaia mission. We first reinterpret color–magnitude and color–color …

White dwarfs are stellar embers depleted of nuclear energy sources that cool over billions of
years. These stars, which are supported by electron degeneracy pressure, reach densities of …

Many stars evolve into magnetic white dwarfs (MWDs), and observations may help to
understand when the magnetic field appears at the stellar surface, if and how it evolves …

We present an overview of the sample of Northern hemisphere white dwarfs within 40 pc of
the Sun detected from Gaia Data Release 2 (DR2). We find that 521 sources are …

The magnetic white dwarfs (MWDs) are found either isolated or in interacting binaries. The
isolated MWDs divide into two groups: a high field group (10 5–10 9 G) comprising some …

White dwarfs, the extremely dense remnants left behind by most stars after their death, are
characterized by a mass comparable to that of the Sun compressed into the size of an Earth …

We present a spectrophotometric analysis of 2880 cool white dwarfs within 100 pc of the
Sun and cooler than T eff∼ 10 000 K, with grizy Pan-STARRS photometry and Gaia …

White dwarfs that accrete the debris of tidally disrupted asteroids provide the opportunity to
measure the bulk composition of the building blocks, or fragments, of exoplanets. This …

While magnetic fields have long been considered significant for the evolution of magnetic
non-degenerate stars and compact stars, it has become clear in recent years that, in fact, all …