PSR J1755-2550: a young radio pulsar with a massive, compact companion
Date Issued
2018
Author(s)
Ng, C.
•
Kruckow, M. U.
•
Tauris, T. M.
•
Lyne, A. G.
•
Freire, P. C. C.
•
•
Caiazzo, I.
•
Heyl, J.
•
Kramer, M.
•
Cameron, A. D.
•
Champion, D. J.
•
Stappers, B.
Abstract
Radio pulsars found in binary systems with short orbital periods are usually fast spinning as a consequence of recycling via mass transfer from their companion stars; this process is also thought to decrease the magnetic field of the neutron star being recycled. Here, we report on timing observations of the recently discovered binary PSR J1755-2550 and find that this pulsar is an exception: with a characteristic age of 2.1 Myr, it is relatively young; furthermore, with a spin period of 315 ms and a surface magnetic field strength at its poles of 0.88 × 1012 G, the pulsar shows no sign of having been recycled. Based on its timing and orbital characteristics, the pulsar either has a massive white dwarf (WD) or a neutron star (NS) companion. To distinguish between these two cases, we searched radio observations for a potential recycled pulsar companion and analysed archival optical data for a potential WD companion. Neither work returned conclusive detections. We apply population synthesis modelling and find that both solutions are roughly equally probable. Our population synthesis also predicts a minimum mass of 0.90 M☉ for the companion star to PSR J1755-2550 and we simulate the systemic runaway velocities for the resulting WDNS systems which may merge and possibly produce Ca-rich supernovae. Whether PSR J1755-2550 hosts a WD or a NS companion star, it is certainly a member of a rare subpopulation of binary radio pulsars.
Volume
476
Issue
4
Start page
4315
Issn Identifier
0035-8711
Ads BibCode
2018MNRAS.476.4315N
Rights
open.access
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