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S. Tagieva

Publications and source records attributed to S. Tagieva.

3 recordsLinked to original sources
arXiv2003

Origin of PSRs with 0.1 < P < 0.3 s and 5 x 1E5 < Tau < 1E7 yr after the second Supernova explosion in HMXBs

The origin of a part of the single pulsars with relatively low magnetic fields B < 1E12 G and with characteristic times Tau < 1E7 yr is established. Such pulsars occur as a result of the disruption of High Mass X-ray Binary Systems after a second Supernova explosion. In these binaries mass accretion onto the surface of X-ray pulsars leads to the decrease of the magnetic field from its initial value B ~ 1E12-1E13 G down to B < 1E12 G similar to the processes in Low Mass X-ray Binaries.

astro-ph↗
arXiv2002

Pulsar Luminosity Function

We construct and investigate the pulsar luminosity function using the new catalogue which includes data for 1315 radio pulsars. The luminosity functions are constructed for 400 and 1400 MHz separately, and they are compared. Also, the luminosity functions excluding the binary millisecond pulsars and other pulsars with low magnetic fields are constructed. The 1400 MHz luminosities as a function of characteristic age and as a function of magnetic field for radio pulsars, anomalous X-ray pulsars and dim radio quiet neutron stars are presented and the implications of the pulsar luminosity function on these new kind of neutron stars are discussed.

astro-ph↗
arXiv2002

Statistical Investigations of 1315 Radio Pulsars

In this paper we have used the data of 1315 pulsars (Guseinov et al. 2002) for statistical analysis and showed the changes in pulsar parameters since the appearance of Taylor et al. (1996) catalog. Here we present the space distribution of pulsars, dispersion measures, distances from the galactic plane and from the Sun, electron density, luminosity distributions at 400 and 1400 MHz, the relations between luminosities of pulsars at 400 and 1400 MHz and the dependence of luminosity on age and on magnetic field. We also present the updated P-Pdot diagram.

astro-ph↗