The spatial distribution and birth-rate of pulsars

Cosmic-ray positron measurements: on the origin of the e+ excess and limits on magnetar birthrate

“…In particular, Faucher-Giguère and Kaspi [18] show that pulsars are concentrated in the Milky Way spiral arms and present a radial distribution of these neutron stars with a maximum at 3.5 kpc from the galactic center (GC). Similar results are obtained by Guseinov and Kosumov [22]. On the basis of figure 2 in both papers, we estimate that approximately 13% of galactic pulsars are found in the region between 7.5 kpc and 9.5 kpc from the GC.…”

“…The average number density of young and middle aged pulsars within 1 kpc from the solar system results to be 33 pulsars kpc −3 . This finding follows from the work by Faucher-Giguère and Kaspi [18] and Guseinov and Kosumov [22] by considering an effective Milky Way disk volume of 32.8 kpc 3 for the region between 7.5 and 9.5 kpc from the GC by assuming an average thickness of the galactic disk of 300 pc. The volume of the Galaxy within 1 kpc from Earth is, therefore, 0.96 kpc 3 .…”

“…This finding appears in excellent agreement with the recent result of one pulsar born every 59 years following from a Monte Carlo simulation normalized to the Fermi-LAT observations of young γ-ray pulsars (WR11 in figure 2; [19]). The pulsar spatial distribution was studied in [18] and [22], among others. In particular, Faucher-Giguère and Kaspi [18] show that pulsars are concentrated in the Milky Way spiral arms and present a radial distribution of these neutron stars with a maximum at 3.5 kpc from the galactic center (GC).…”

On the galactic distributions of radio pulsars and plasma density

“…Spatial distribution of radio pulsars and its relation to the plasma density distribution were examined in some earlier works (Guseinov and Kasumov 1978, 1981, Gailly et al 1978. Later, some models on using the DM values together with some basic criteria based on empirical facts to determine locations of pulsars in different intervals of longitude and latitude were constructed, improving the pioneering work by Guseinov and Kasumov (1981) as a result of the large increase in the number and quality of the observational data (Gok et al 1996, Guseinov et al 2002, Yazgan et al 2003.…”

Supernovae. Part II: the aftermath

“…0 found by Fahlman and Gregory (1981 (Gregory, 1982 (Tuohy and Garmire, 1980;Lamb and Markert, 1981;Becker et al , 1982;Helfand, 1980Helfand, , 1981 Becker et al (1982), who found the x-ray emission (cf. also van (Large, 1971: Guseinov andKasumov, 1978;Gailly, Lequeux, and Masnou, 1978;Chevalier, 1981;Lyne, 1982), with a brief interruption (Taylor, 1977) Panagia (1978, 1980) Cas A (Chevalier, 1981) was, at least, not the product of a normally bright SN. Chevalier attributes it to a very massive star that 1ost its hydrogen-rich envelope before being disrupted, perhaps by an electron-positron pair production supernova (Sec.…”