2014MNRAS.438.3587T

We aim to identify the birth place of the young pulsar PSR J0826+2637 in order to determine its kinematic age and give constraints on its radial and spatial (kick) velocity. Since the majority of neutron star (NS) progenitors are in associations or clusters, we search for a possible origin of the NS inside such stellar groups. We trace back the NS and the centres of possible birth associations and clusters to find close encounters. The kinematic age is then given by the time since the encounter. We use Monte Carlo simulations to account for observational uncertainties and the unknown radial velocity of the NS. We evaluate the outcome statistically. In order to find further indication for our findings, we also search for a runaway star that could be the former companion if it exists. We find that PSR J0826+2637 was probably born in the small young cluster Stock 7 ∼ 3Myr ago. This result is supported by the identification of the former companion candidate HIP 13962 (runaway star with spectral type G0Ia). The scenario predicts a near-zero radial velocity of the pulsar implying an inclination angle of its motion to the line of sight of 87°±11°. We also present the chemical abundances of HIP 13962. We do not find enhanced α element abundances in the highly evolved star. However, the binary supernova (SN) scenario may be supported by the overabundance of r-process elements that could have been ejected during the SN and accreted by the runaway star. Also, a high rotational velocity of vsini ∼ 29 km/s of HIP 13962 is consistent with evolution in a pre-SN binary system.