{"title":"PSR J1755−2550: A young radio pulsar with a massive, compact companion","publication_status":"published","citation":{"mla":"Ng, C., et al. “PSR J1755−2550: A Young Radio Pulsar with a Massive, Compact Companion.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4315–26, doi:<a href=\"https://doi.org/10.1093/mnras/sty482\">10.1093/mnras/sty482</a>.","apa":"Ng, C., Kruckow, M. U., Tauris, T. M., Lyne, A. G., Freire, P. C. C., Ridolfi, A., … Stappers, B. (2018). PSR J1755−2550: A young radio pulsar with a massive, compact companion. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty482\">https://doi.org/10.1093/mnras/sty482</a>","ieee":"C. Ng <i>et al.</i>, “PSR J1755−2550: A young radio pulsar with a massive, compact companion,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4315–4326, 2018.","chicago":"Ng, C, M U Kruckow, T M Tauris, A G Lyne, P C C Freire, A Ridolfi, Ilaria Caiazzo, et al. “PSR J1755−2550: A Young Radio Pulsar with a Massive, Compact Companion.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty482\">https://doi.org/10.1093/mnras/sty482</a>.","short":"C. Ng, M.U. Kruckow, T.M. Tauris, A.G. Lyne, P.C.C. Freire, A. Ridolfi, I. Caiazzo, J. Heyl, M. Kramer, A.D. Cameron, D.J. Champion, B. Stappers, Monthly Notices of the Royal Astronomical Society 476 (2018) 4315–4326.","ista":"Ng C, Kruckow MU, Tauris TM, Lyne AG, Freire PCC, Ridolfi A, Caiazzo I, Heyl J, Kramer M, Cameron AD, Champion DJ, Stappers B. 2018. PSR J1755−2550: A young radio pulsar with a massive, compact companion. Monthly Notices of the Royal Astronomical Society. 476(4), 4315–4326.","ama":"Ng C, Kruckow MU, Tauris TM, et al. PSR J1755−2550: A young radio pulsar with a massive, compact companion. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4315-4326. doi:<a href=\"https://doi.org/10.1093/mnras/sty482\">10.1093/mnras/sty482</a>"},"page":"4315-4326","_id":"15236","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"author":[{"full_name":"Ng, C","first_name":"C","last_name":"Ng"},{"full_name":"Kruckow, M U","first_name":"M U","last_name":"Kruckow"},{"last_name":"Tauris","full_name":"Tauris, T M","first_name":"T M"},{"full_name":"Lyne, A G","first_name":"A G","last_name":"Lyne"},{"last_name":"Freire","full_name":"Freire, P C C","first_name":"P C C"},{"last_name":"Ridolfi","full_name":"Ridolfi, A","first_name":"A"},{"first_name":"Ilaria","full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","orcid":"0000-0002-4770-5388","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"last_name":"Heyl","full_name":"Heyl, J","first_name":"J"},{"full_name":"Kramer, M","first_name":"M","last_name":"Kramer"},{"full_name":"Cameron, A D","first_name":"A D","last_name":"Cameron"},{"first_name":"D J","full_name":"Champion, D J","last_name":"Champion"},{"last_name":"Stappers","first_name":"B","full_name":"Stappers, B"}],"publisher":"Oxford University Press","intvolume":"       476","volume":476,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1802.08248"}],"oa_version":"Preprint","extern":"1","publication":"Monthly Notices of the Royal Astronomical Society","language":[{"iso":"eng"}],"article_type":"original","quality_controlled":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"02","date_created":"2024-03-26T10:39:05Z","issue":"4","abstract":[{"lang":"eng","text":"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."}],"external_id":{"arxiv":["1802.08248"]},"status":"public","doi":"10.1093/mnras/sty482","type":"journal_article","oa":1,"day":"23","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_published":"2018-02-23T00:00:00Z","year":"2018","article_processing_charge":"No","date_updated":"2024-04-08T07:02:52Z"}