Microscopic vortex velocity in the inner crust and outer core of
... 4 VO RT E X V E L O C I T Y I N T H E I N N E R C RU S T The physical state of the inner crust with its neutron rich nuclei and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is fou ...
... 4 VO RT E X V E L O C I T Y I N T H E I N N E R C RU S T The physical state of the inner crust with its neutron rich nuclei and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is fou ...
Turning Points in the Evolution of Isolated Neutron Stars` Magnetic
... Showdowns in the Life of Neutron Star Magnetic Fields ...
... Showdowns in the Life of Neutron Star Magnetic Fields ...
Magnetic fields and mass loss in massive stars
... At all scales the magnetic fields are thought to be either generated by dynamo processes, or to be of a fossil origin. The origin of the magnetic fields on the largest scales, scales of galaxies and larger, is a fundamental cosmological question (see, e.g., Vallée 2004; Giovannini 2004). The magnet ...
... At all scales the magnetic fields are thought to be either generated by dynamo processes, or to be of a fossil origin. The origin of the magnetic fields on the largest scales, scales of galaxies and larger, is a fundamental cosmological question (see, e.g., Vallée 2004; Giovannini 2004). The magnet ...
Galactic Winds Sylvain Veilleux
... through telescopes. This has become clear from the most comprehensive numerical simulations involving up to 1010 particles, which purport to track the evolution of individual galaxies to the present day. Although Cold Dark Matter (CDM) simulations account well for the observed large-scale structure, ...
... through telescopes. This has become clear from the most comprehensive numerical simulations involving up to 1010 particles, which purport to track the evolution of individual galaxies to the present day. Although Cold Dark Matter (CDM) simulations account well for the observed large-scale structure, ...
White dwarfs, black holes and neutron stars in close binaries
... nuclear burning time-scale) or because of angular momentum loss from the orbit (e.g. by gravitational wave radiation); in that case the mass transfer proceeds on the typical time-scale of this angular momentum loss. Because the mass-transfer rates are generally low, most transferred matter can proba ...
... nuclear burning time-scale) or because of angular momentum loss from the orbit (e.g. by gravitational wave radiation); in that case the mass transfer proceeds on the typical time-scale of this angular momentum loss. Because the mass-transfer rates are generally low, most transferred matter can proba ...
