Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/28829
DC Field | Value | Language |
---|---|---|
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.contributor.author | Belfiore, Andrea | en_US |
dc.contributor.author | STELLA, Luigi | en_US |
dc.contributor.author | ESPOSITO, PAOLO | en_US |
dc.contributor.author | CASELLA, Piergiorgio | en_US |
dc.contributor.author | DE LUCA, Andrea | en_US |
dc.contributor.author | MARELLI, MARTINO | en_US |
dc.contributor.author | PAPITTO, ALESSANDRO | en_US |
dc.contributor.author | PERRI, Matteo | en_US |
dc.contributor.author | Puccetti, Simonetta | en_US |
dc.contributor.author | RODRIGUEZ CASTILLO, Guillermo Andres | en_US |
dc.contributor.author | Salvetti, David | en_US |
dc.contributor.author | TIENGO, ANDREA | en_US |
dc.contributor.author | ZAMPIERI, Luca | en_US |
dc.contributor.author | D'Agostino, Daniele | en_US |
dc.contributor.author | Greiner, Jochen | en_US |
dc.contributor.author | Haberl, Frank | en_US |
dc.contributor.author | Novara, Giovanni | en_US |
dc.contributor.author | SALVATERRA, Ruben | en_US |
dc.contributor.author | Turolla, Roberto | en_US |
dc.contributor.author | Watson, Mike | en_US |
dc.contributor.author | Wilms, Joern | en_US |
dc.contributor.author | WOLTER, Anna Luisa Maria | en_US |
dc.date.accessioned | 2020-12-14T14:14:22Z | - |
dc.date.available | 2020-12-14T14:14:22Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0036-8075 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28829 | - |
dc.description.abstract | Ultraluminous x-ray sources (ULXs) in nearby galaxies shine brighter than any x-ray source in our Galaxy. ULXs are usually modeled as stellar-mass black holes (BHs) accreting at very high rates or intermediate-mass BHs. We present observations showing that NGC 5907 ULX is instead an x-ray accreting neutron star (NS) with a spin period evolving from 1.43 seconds in 2003 to 1.13 seconds in 2014. It has an isotropic peak luminosity of ~1000 times the Eddington limit for a NS at 17.1 megaparsec. Standard accretion models fail to explain its luminosity, even assuming beamed emission, but a strong multipolar magnetic field can describe its properties. These findings suggest that other extreme ULXs (x-ray luminosity ≥ 10<SUP>41</SUP> erg second<SUP>-1</SUP>) might harbor NSs. | en_US |
dc.language.iso | eng | en_US |
dc.title | An accreting pulsar with extreme properties drives an ultraluminous x-ray source in NGC 5907 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1126/science.aai8635 | en_US |
dc.identifier.scopus | 2-s2.0-85013993738 | en_US |
dc.identifier.isi | 000395127600036 | en_US |
dc.identifier.url | https://science.sciencemag.org/content/355/6327/817 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 355 | en_US |
dc.relation.issue | 6327 | en_US |
dc.relation.firstpage | 817 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | DEU | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | SCIENCE | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017Sci...355..817I | en_US |
dc.relation.fund | FP7 | 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 | mixedopen | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0036-8075 | - |
crisitem.journal.ance | E151981 | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.author.orcid | 0000-0002-0752-3301 | - |
crisitem.author.orcid | 0000-0001-6739-687X | - |
crisitem.author.orcid | 0000-0001-6289-7413 | - |
crisitem.author.orcid | 0000-0003-3613-4409 | - |
crisitem.author.orcid | 0000-0003-3952-7291 | - |
crisitem.author.orcid | 0000-0002-6516-1329 | - |
crisitem.author.orcid | 0000-0002-9393-8078 | - |
crisitem.author.orcid | 0000-0001-5840-9835 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | Existing users please |
---|---|---|---|---|
ScienceMain_Final.pdf | [Administrators only] | 586.7 kB | Adobe PDF | |
ScienceSM_Final.pdf | Supplementary Material | 890.78 kB | Adobe PDF | View/Open |
preprint1609.07375.pdf | preprint | 10.53 MB | Adobe PDF | View/Open |
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