Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/29643
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Simone Dall'Osso | en_US |
dc.contributor.author | Rosalba Perna | en_US |
dc.contributor.author | STELLA, Luigi | en_US |
dc.date.accessioned | 2021-01-11T14:41:56Z | - |
dc.date.available | 2021-01-11T14:41:56Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/29643 | - |
dc.description.abstract | The identification of the Ultraluminous X-ray source (ULX) X-2 in M82 as an accreting pulsar has shed new light on the nature of a subset of ULXs, while rising new questions on the nature of the super-Eddington accretion. Here, by numerically solving the torque equation of the accreting pulsar within the framework of the magnetically threaded-disk scenario, we show that three classes of solutions, corresponding to different values of the magnetic field, are mathematically allowed. We argue that the highest magnetic field one, corresponding to B $\sim 10^{13}$ G, is favoured based on physical considerations and the observed properties of the source. In particular, that is the only solution which can account for the observed variations in $\dot{P}$ (over four time intervals) without requiring major changes in $\dot{M}$, which would be at odds with the approximately constant X-ray emission of the source during the same time. For this solution, we find that the source can only accomodate a moderate amount of beaming, 0.5 $\lesssim b < 1$. Last, we show that the upper limit on the luminosity, L$_X < 2.5 \times 10^{38}$ erg s$^{-1}$ from archival observations, is consistent with a highly-magnetized neutron star being in the propeller phase at that time. | en_US |
dc.language.iso | eng | en_US |
dc.title | NuSTAR J095551+6940.8: a highly magnetised neutron star with super-Eddington mass accretion | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stv170 | en_US |
dc.identifier.scopus | 2-s2.0-84954493926 | en_US |
dc.identifier.isi | 000355337500079 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/449/2/2144/1064867 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 449 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 2144 | en_US |
dc.relation.lastpage | 2150 | en_US |
dc.relation.numberofpages | 7 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | 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 | 2015MNRAS.449.2144D | 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::PE9_10 High energy and particle astronomy – X-rays, cosmic rays, gamma rays, neutrinos | 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.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0002-0018-1687 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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stv170.pdf | PDF editoriale | 472.23 kB | Adobe PDF | View/Open |
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