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http://hdl.handle.net/20.500.12386/26772
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | MEREGHETTI, Sandro | en_US |
dc.contributor.author | LA PALOMBARA, NICOLA | en_US |
dc.contributor.author | TIENGO, ANDREA | en_US |
dc.contributor.author | ESPOSITO, PAOLO | en_US |
dc.date.accessioned | 2020-08-24T11:42:18Z | - |
dc.date.available | 2020-08-24T11:42:18Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26772 | - |
dc.description.abstract | We report the results of a new XMM-Newton observation of the helium-rich hot subdwarf BD+37°442 carried out in 2016 February. The possible periodicity at 19 s seen in a 2011 shorter observation is not confirmed, thus dismissing the evidence for a binary nature. This implies that the observed soft X-ray emission, with a luminosity of a few 10<SUP>31</SUP> erg s<SUP>-1</SUP>, originates in BD+37°442 itself, rather than in an accreting neutron star companion. The X-ray spectrum is well fit by thermal plasma emission with a temperature of 0.22 keV and non-solar element abundances. Besides the overabundance of He, C and N already known from optical/UV studies, the X-ray spectra indicate also a significant excess of Ne. The soft X-ray spectrum and the ratio of X-ray to bolometric luminosity, L<SUB>X</SUB>/L<SUB>BOL</SUB> ∼ 2 × 10<SUP>-7</SUP>, are similar to those observed in massive early-type stars. This indicates that the mechanisms responsible for plasma shock-heating can work also in the weak stellar winds (mass-loss rates dot{M}_W≤ 10^{-8} M<SUB>☉</SUB> yr<SUP>-1</SUP>) of low-mass hot stars. | en_US |
dc.language.iso | eng | en_US |
dc.title | The lack of X-ray pulsations in the extreme helium star BD+37°442 and its possible stellar wind X-ray emission | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw3335 | en_US |
dc.identifier.scopus | 2-s2.0-85018338423 | en_US |
dc.identifier.isi | 000398418600030 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/466/3/2918/2736293 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 466 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 2918 | en_US |
dc.type.referee | REF_1 | 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 | 2017MNRAS.466.2918M | 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.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.orcid | 0000-0003-3259-7801 | - |
crisitem.author.orcid | 0000-0001-7015-6359 | - |
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