18 research outputs found
Do Young Neutron Stars Which Show Themselves As AXPs, SGRs and Radio Pulsars Accrete?
We examined the fall-back disk models, and in general accretion, proposed to
explain the properties of anomalous X-ray pulsars (AXPs), soft gamma repeaters
(SGRs), and radio pulsars (PSRs). We checked the possibility of some gas
remaining around the neutron star after the supernova explosion. We also
compared AXPs and SGRs with the X-ray pulsars in X-ray binaries. We conclude
the existing models of accretion from a fall-back disk are insufficient to
explain the nature of AXPs/SGRs, particularly the SGR bursts. We also discussed
the proposed model of combination of magnetic dipole radiation and propeller
torques in order to explain the evolution of radio pulsars on the P-\.{P}
diagram. The predictions of this model contradict the observational data.Comment: 16 Pages, 1 Figur
Magnetospheric particle acceleration and X-ray emission of pulsars
The available data on isolated X-ray pulsars, their wind nebulae, and the
supernova remnants which are connected to some of these sources are analyzed.
It is shown that electric fields of neutron stars tear off charged particles
from the surface of neutron star and trigger the acceleration of particles. The
charged particles are accelerated mainly in the field of magneto-dipole
radiation wave. Power and energy spectra of the charged particles depend on the
strength of the magneto-dipole radiation. Therefore, the X-ray radiation is
strongly dependent on the rate of rotational energy loss and weakly dependent
on the electric field intensity. Coulomb interaction between the charged
particles is the main factor for the energy loss and the X-ray spectra of the
charged particles.Comment: minor correction on table format, 20 pages (4 figures, 1 table),
submitted to International Journal of Modern Physics
Influences of neutron star parameters on evolutions of different types of pulsar; evolutions of anomalous X-ray pulsars, soft gamma repeaters and dim isolated thermal neutron stars on the P-\.{P} diagram
Influences of the mass, moment of inertia, rotation, absence of stability in
the atmosphere and some other parameters of neutron stars on the evolution of
pulsars are examined. It is shown that the locations and evolutions of soft
gamma repeaters, anomalous X-ray pulsars and other types of pulsar on the
period versus period derivative diagram can be explained adopting values of
B G for these objects. This approach gives the possibility to explain
many properties of different types of pulsar.Comment: 18 pages, 1 figur
The Relation Between the Surface Brightness and the Diameter for Galactic Supernova Remnants
In this work, we have constructed a relation between the surface brightness
() and diameter (D) of Galactic C- and S-type supernova remnants
(SNRs). In order to calibrate the -D dependence, we have carefully
examined some intrinsic (e.g. explosion energy) and extrinsic (e.g. density of
the ambient medium) properties of the remnants and, taking into account also
the distance values given in the literature, we have adopted distances for some
of the SNRs which have relatively more reliable distance values. These
calibrator SNRs are all C- and S-type SNRs, i.e. F-type SNRs (and S-type SNR
Cas A which has an exceptionally high surface brightness) are excluded. The
Sigma-D relation has 2 slopes with a turning point at D=36.5 pc: (at 1
GHz)=8.4 D
WmHzster (for
WmHzster and D36.5 pc) and (at 1
GHz)=2.7 10 D
WmHzster (for
WmHzster and D36.5 pc). We discussed the theoretical
basis for the -D dependence and particularly the reasons for the change
in slope of the relation were stated. Added to this, we have shown the
dependence between the radio luminosity and the diameter which seems to have a
slope close to zero up to about D=36.5 pc. We have also adopted distance and
diameter values for all of the observed Galactic SNRs by examining all the
available distance values presented in the literature together with the
distances found from our -D relation.Comment: 45 pages, 2 figures, accepted for publication in Astronomical and
Astrophysical Transaction