The rate of iPTF 14gqr like ultra-stripped supernovae and binary evolution leading to double neutron star formation

Abstract

Double neutron star (DNS) systems are produced from massive binaries. A supernova (SN) explosion of an extremely stripped star is expected to occur at the final stage of DNS formation. This type of SN is called ultra-stripped SN (USSN). A recent research reveals that a type Ic SN, iPTF 14gqr (SN 2014ft) has low ejecta mass ($\approx 0.2{\mathrm{M}}_{\odot }$) and its progenitor has a helium envelope with its mass $\sim 0.01{\mathrm{M}}_{\odot }$. Then this SN is interpreted as an USSN, and this is the first discovery of the USSN. Furthermore, the observation of iPTF 14gqr provides us with some information about its formation history. Here, we perform population synthesis calculations so as to estimate the detection rate of iPTF 14gqr like USSNe by optical transient surveys, intermediate Palomar Transient Factory (iPTF), Zwicky Transient Facility (ZTF), and Large Synoptic Survey Telescope (LSST). We find that iPTF, ZTF, and LSST can observe iPTF 14gqr like USSNe at the rates of 1, 40, and 5 ${\mathrm{yr}}^{-1}$, respectively. The iPTF may detect 4 iPTF 14gqr like USSNe during four years observation. Additionally, we investigate effects of some binary physics on the orbital parameters of DNS systems and formation channels.

arXiv comment12 pages, 5 figures, published in ApJ

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