Results 271 to 280 of about 2,510 (308)
Some of the next articles are maybe not open access.
2016
White dwarf stars are the burnt out remnants that remain after a star like the Sun has completed its nuclear evolution. In such a star there are no remaining nuclear energy sources, so the star evolves by simply radiating its stored thermal energy out into space.
openaire +1 more source
White dwarf stars are the burnt out remnants that remain after a star like the Sun has completed its nuclear evolution. In such a star there are no remaining nuclear energy sources, so the star evolves by simply radiating its stored thermal energy out into space.
openaire +1 more source
2000
I briefly review the observed properties of pulsating white dwarfs. Examples of some of the applications of seismology to these stars demonstrate how they can provide useful constraints on stellar evolution theory.
openaire +1 more source
I briefly review the observed properties of pulsating white dwarfs. Examples of some of the applications of seismology to these stars demonstrate how they can provide useful constraints on stellar evolution theory.
openaire +1 more source
Neutron Stars and White Dwarfs
1972This talk reviews the structure of neutron stars and white dwarfs, and the role of solid state physics in determining their properties. The nature of the matter in neutron stars (matter essentially in its absolute ground state), and the determination of its equation of state are first discussed; this is followed by a description of the resulting ...
openaire +1 more source
2009
White dwarfs are the most common end-product of stellarevolution, and as such contain valuable information about the evolutionof individual stars as well as about the star formation history andsubsequent evolution in our Galaxy. In this lecture, I describe the main structural and evolutive properties of white dwarfs.
openaire +1 more source
White dwarfs are the most common end-product of stellarevolution, and as such contain valuable information about the evolutionof individual stars as well as about the star formation history andsubsequent evolution in our Galaxy. In this lecture, I describe the main structural and evolutive properties of white dwarfs.
openaire +1 more source
White Dwarfs and Neutron Stars
2004This chapter on the physics of compact objects begins with a section on white dwarfs. It will be shown that the famous Chandrasekhar equation is just the relativistic Thomas–Fermi equation. For white dwarfs the Thomas–Fermi approximation is ideally justified. For neutron stars the general relativistic stellar structure equations are needed.
openaire +1 more source
1992
White dwarf stars represent the most common endpoint of stellar evolution. In fact, about 90% of all stars will end up as white dwarfs. Their high temperatures and low luminosities imply that they are small — only about the size of the Earth (R e = 0.009R⊙). The mean radius for white dwarfs is R = 0.01 R⊙ (see the first table).
openaire +1 more source
White dwarf stars represent the most common endpoint of stellar evolution. In fact, about 90% of all stars will end up as white dwarfs. Their high temperatures and low luminosities imply that they are small — only about the size of the Earth (R e = 0.009R⊙). The mean radius for white dwarfs is R = 0.01 R⊙ (see the first table).
openaire +1 more source
Brain and other central nervous system tumor statistics, 2021
Ca-A Cancer Journal for Clinicians, 2021Kimberly D Miller +2 more
exaly