Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32441
DC Field | Value | Language |
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dc.contributor.author | Ng, C. | en_US |
dc.contributor.author | Kruckow, M. U. | en_US |
dc.contributor.author | Tauris, T. M. | en_US |
dc.contributor.author | Lyne, A. G. | en_US |
dc.contributor.author | Freire, P. C. C. | en_US |
dc.contributor.author | RIDOLFI, ALESSANDRO | en_US |
dc.contributor.author | Caiazzo, I. | en_US |
dc.contributor.author | Heyl, J. | en_US |
dc.contributor.author | Kramer, M. | en_US |
dc.contributor.author | Cameron, A. D. | en_US |
dc.contributor.author | Champion, D. J. | en_US |
dc.contributor.author | Stappers, B. | en_US |
dc.date.accessioned | 2022-06-21T14:50:17Z | - |
dc.date.available | 2022-06-21T14:50:17Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32441 | - |
dc.description.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 × 10<SUP>12</SUP> 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<SUB>☉</SUB> 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. | en_US |
dc.language.iso | eng | en_US |
dc.title | PSR J1755-2550: a young radio pulsar with a massive, compact companion | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty482 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/476/4/4315/4904135 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 476 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 4315 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018MNRAS.476.4315N | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
item.fulltext | With Fulltext | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
crisitem.author.dept | O.A. Cagliari | - |
crisitem.author.orcid | 0000-0001-6762-2638 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Ng_2018.pdf | Pdf editoriale | 2.41 MB | Adobe PDF | View/Open |
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