Physics of Compact Objects
Different models for the composition and equation
of state of neutron-star matter produce neutron star models with different
properties which might then be detected in observations. Particularly important
in this context is the possibility of constraining the form of particle
interactions in high density matter or of finding evidence for the occurrence
of phase transitions in the stellar interior or of exotic states of matter
("strange stars" being an extreme example).
Electrodynamics of Neutron Stars:
Static Configurations General relativistic
corrections have been computed for the electromagnetic fields of a slowly
rotating relativistic star with misaligned magnetic moment. The analytic
formalism developed has been used to study the relativistic Ohmic decay
of the magnetic field of such a star.
Electrodynamics of Neutron Stars:
Perturbed Configurations Stellar Oscillations
will generate GWs together with electromagnetic (EM) radiation. The general
relativistic corrections for the EM waves produced in a vacuum spacetime
have been derived analytically. EM radiation, together with GW radiation,
could be used to determine physical parameters of the star such as its
mass and radius.
Electrodynamics of
Proto Neutron Stars: During the initial
few seconds after their birth, newly-formed neutron stars are extremely
hot and potentially subject to a number of convective
instabilities. These instabilities can easily couple with the intense and
turbulent magnetic fields which have been amplified during the collapse
and lead to dynamo processes. A first investigation in this direction has
been reported in this paper.
Non-standard
models for compact stars:Study of
models for which a scalar field plays an important role together with ordinary
matter, investigatingparticularly their behaviour when subject to perturbations
in order to see if they might show distinctive characteristic properties
which could be observed.
People involved:
Staff Members: J.C.
Miller, L. Rezzolla
Post-Docs:
Ph.D. students:
Main Collaborators:
B. Ahmedov (Tashkent), A. Bonanno
(Catania), J. Rikovska-Stone (Oxford), V. Urpin (St. Petersburg),
O. Zanotti (Valencia)
Page created by:
Luciano Rezzolla
Last change made: April 15,
2004