Abstract The redshift distribution of fast radio bursts (FRBs) is not well constrained. association the Galactic FRB 200428 with young magnetar SGR 1935+2154 raises working hypothesis that sources track star formation history universe. discovery 20200120E in a globular cluster nearby galaxy M81, however, casts doubts on such an assumption. We apply Monte Carlo method developed previous work to ...

We report on the first ten weeks of Rossi X-ray Timing Explorer observations of the X-ray transient XTE J1701–462. Large count rate variations were accompanied by changes in the source’s spectral and variability properties. Based on comparisons with other sources we conclude that XTE J1701–462 had all the characteristics of the neutron star Z sources, i.e., the class of the brightest persistent...

One of the most important factors influencing the track maintenance is the transitions between parts of the track with different vertical stiffness. The dynamic...

this paper deals with the threshold radius that warrants the use of single restraining rail for transit and railroads. different railways use different threshold radius from 91m to 365m to provide restraining rail. these threshold figures are probably experience driven choices. the need for restraining rail may be related to a so-called derailment alarm coefficient of 1.2 sustained over 2m leng...

The cosmic γ-ray burst (GRB) formation rate, as derived from the variabilityluminosity relation for long-duration GRBs, is compared with the cosmic star formation rate. If GRBs are related to the collapse of massive stars, one expects the GRB rate to be approximately proportional to the star formation rate. We found that these two rates have similar slopes at low redshift. This suggests that GR...

We characterize the local (2-kpc sized) environments of Type Ia, II, and Ib/c supernovae (SNe) that have recently occurred in nearby ($d\lesssim50$ Mpc) galaxies. Using ultraviolet (UV, from GALEX) infrared (IR, WISE) maps 359 galaxies a sample 472 SNe, we measure star formation rate surface density ($\Sigma_{\rm SFR}$) stellar mass ($\Sigma_\star$) 2-kpc beam centered on each SN site. show cor...

In the present work, we have obtained the equation of state for neutron star matter considering the in uence of the ferromagnetic and antiferromagnetic spin state. We have also investigated the structure of neutron stars. According to our results, the spin asymmetry stiens the equation of state and leads to high mass for the neutron star.