young neutron stars and their wind nebulae YOUNGNEUTRON STARS WINDNEBULAE Patrick Slane Harvard-Smithsonian Center Astrophysicsslane@cfa.harvard.edu Abstract Teragaussmagnetic fields, surface gravity sufficiently strong signifi-cantly modify light paths, central densities higher than standardnu- ...
This predicts a simple evolution of the surface-field of such stars as they spin down or, less commonly, are spun up. Consequences and comparisons with observations are given for properties of solitary spinning down pulsars, including their glitches and spin-down ages, X-ray pulsars, and the ...
The life of a star, no matter its size, is a balancing act between the inward "push" of gravity and the outward push provided by photons generated as they conductnuclear fusion, the forging of heavy atomic nuclei from light nuclei, at their cores. When stars run out of hydrogen to fuse...
Like other neutron stars, pulsars form when massive stars die in supernova explosions and their remnants collapse into compact objects made only of neutrons. When a mass as great as our sun's is packed into a space about the size of a city, the conserved angular momentum causes the resultin...
Neutron stars are not only the most dense objects in the Universe, but they rotate very fast and regularly. Until they don't. Occasionally these neutronstarsstart to spin faster, caused by portions of the inside of the star moving outwards. It's called a "glitch" and it provides astronomer...
Neutron stars are the smallest, densest stars in the universe, born out of the gravitational collapse of extremely massive stars. True to their name, neutron stars are composed almost entirely of neutrons—neutral subatomic particles that have been compr
Since neutron stars contain magnetic fields, while black holes don't, the researchers knew that the ULX was the former and not the latter. The immense gravitational pull of a neutron star draws in material from companion stars, which causes the matter to heat up and glow with X-rays. ...
We show that PHSs with a mass M < Mcr could survive the early stages of their evolution without decaying to QSs. Finally, we discuss the possible evolutionary paths of PHSs. Keywords: Neutron stars; equations of state of neutron-star matter; quark deconfine- ment. 1. Introduction Neutron ...
Neutron stars are born when massive stars reach the end of their fuel for nuclear fusion at their cores. This causes that core to collapse rapidly while the outer layers of the star are slewed away, leaving behind a body with a mass of between one and two times that of the sun squashed...
Mass, temperature, and magnetic fields can all be used to characterize neutron stars; a unique equation can also describe their internal structure. The way these stars act is determined by this formula. One has to research neutron stars to learn about the most unusual material ...