Formation of the Double Neutron Star System PSR J1930$-$1852

Abstract

The spin period (185 ms) and period derivative ($1.8\times 10^{-17}\mathrm{s}{\mathrm{s}}^{-1}$) of the double neutron star (DNS) system PSR J1930$-$1852 recently discovered indicate that the pulsar was mildly recycled through the process of Roche-lobe overflow. This system has the longest orbital period (45 days) of the known DNS systems, and can be formed from a helium star-NS binary if the initial mass of the helium star was $\lesssim 4.0M_{\odot }$; otherwise the helium star would never fill its Roche-lobe \citep{t15}. At the moment of the supernova explosion, the mass of the helium star was $\lesssim 3.0M_{\odot }$. We find that the probability distribution of the velocity kick imparted to the new-born neutron star has a maximum at about $30\mathrm{km}{\mathrm{s}}^{-1}$ (and a tail up to $260\mathrm{km}{\mathrm{s}}^{-1}$), indicating that this NS most probably received a low kick velocity at birth.

9 pages, 4 figures, accepted for publication in ApJ

References in corpus (1)

• PSR J1930-1852: a pulsar in the widest known orbit around another neutron star

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• A strange dwarf scenario for the formation of the peculiar double white dwarf binary SDSS J125733.63+542850.5