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We aim to identify the birth place of the young pulsar PSR J0826+2637 inorder to determine its kinematic age and give constraints on its radial andspatial (kick) velocity. Since the majority of neutron star (NS) progenitorsare in associations or clusters, we search for a possible origin of the NSinside such stellar groups. We trace back the NS and the centres of possiblebirth associations and clusters to find close encounters. The kinematic age isthen given by the time since the encounter. We use Monte Carlo simulations toaccount for observational uncertainties and the unknown radial velocity of theNS. We evaluate the outcome statistically. In order to find further indicationfor our findings, we also search for a runaway star that could be the formercompanion if it exists. We find that PSR J0826+2637 was probably born in thesmall young cluster Stock 7 ~3 Myr ago. This result is supported by theidentification of the former companion candidate HIP 13962 (runaway star withspectral type G0Ia). The scenario predicts a near-zero radial velocity of thepulsar implying an inclination angle of its motion to the line-of-sight of87+/-11 deg. We also present the chemical abundances of HIP 13962. We do notfind enhanced alpha element abundances in the highly evolved star. However, thebinary supernova scenario may be supported by the overabundance of r-processelements that could have been ejected during the supernova and accreted by therunaway star. Also, a high rotational velocity of v sin i ~29 km/s of HIP 13962is consistent with evolution in a pre-SN binary system.

The Origin of the Young Pulsar PSR J0826+2637 and Its Possible Former Companion HIP 13962