Structure and Evolution of White Dwarfs and their Interaction with the Local Interstellar Medium

Abstract

Abstract:The development of far-UV astronomy has been particularly important for the study of hot white dwarf stars. A significant fraction of their emergent flux appears in the far-UV and traces of elements heavier than hydrogen or helium are, in general, only detected in this waveband or at shorter wavelengths that are also only accessible from space. Although white dwarfs have been studied in the far-UV throughout the past ~25 years, since the launch of IUE, only a few tens of objects have been studied in great detail and a much larger sample is required to gain a detailed understanding of the evolution of hot white dwarfs and the physical processes that determine their appearance. We review here the current knowledge regarding hot white dwarfs and outline what work needs to be carried out by future far-UV observatories.

A population synthesis fitting of the Gaia resolved white dwarf binary population within 100 pc

“…★ E-mail: santiago.torres@upc.es Barstow & Werner 2006), and the central objects in the generation of type Ia supernovae through the different possible scenarios (e.g. Livio & Mazzali 2018).…”

A finite temperature chandrasekhar model: Determining the parameters and calculation of the characteristics of degenerate dwarfs

“…The very rich observational data available have been applied to analyses of the mass-radius relation for a wide range of photosphere temperatures [1][2][3][4][5]; the empirical discovery of interesting peculiarities in the mass and radius distributions of dwarfs [6][7][8][9][10][11][12] has enabled evolutionary approach to the theory of degenerate dwarfs [13][14][15][16][17], and led to attempts to include the effects of magnetic fields and Coulomb interactions in the theory of relativistic stars [5,18,19].…”

“…In the model, μ e varies within a fairly narrow range close to μ e = 2.0. Using the calculated masses and radii of the dwarfs and eliminating x 0 , the mass-radius relation can be found in the form of a family of curves, each corresponding to a specified value of μ e in the above range [1][2][3][4]. The mass-radius relation is considered to be one of the main tests of the theory.…”

Stellar And Galactic Environment survey (SAGE)

“…Production of white dwarfs in the disk substantially enriches the content of the local ISM, contributing significantly to the total cosmic abundance of metals, particularly CNO (e.g. Barstow and Werner [22]), and these stars also make good background sources against which interstellar material can be detected. There is compelling evidence that some white dwarfs are surrounded by circumstellar material [23], which may be a remnant of earlier mass loss phases.…”