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UV and X-ray observations of the neutron star LMXB EXO 0748–676 in its quiescent state
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dc.contributor.author | Parikh, A S | |
dc.contributor.author | Degenaar, N | |
dc.contributor.author | Hernández Santisteban, J V | |
dc.contributor.author | Wijnands, R | |
dc.contributor.author | Psaradaki, I | |
dc.contributor.author | Costantini, E | |
dc.contributor.author | Modiano, D | |
dc.contributor.author | Miller, J M | |
dc.date.accessioned | 2021-02-24T17:30:04Z | |
dc.date.available | 2021-02-24T17:30:04Z | |
dc.date.issued | 2021-02 | |
dc.identifier | 273020388 | |
dc.identifier | 88d09855-a560-4108-a594-a7633eef57ea | |
dc.identifier | 85100332095 | |
dc.identifier | 000608474800109 | |
dc.identifier.citation | Parikh , A S , Degenaar , N , Hernández Santisteban , J V , Wijnands , R , Psaradaki , I , Costantini , E , Modiano , D & Miller , J M 2021 , ' UV and X-ray observations of the neutron star LMXB EXO 0748–676 in its quiescent state ' , Monthly Notices of the Royal Astronomical Society , vol. 501 , no. 1 , pp. 1453-1462 . https://doi.org/10.1093/mnras/staa3734 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | Bibtex: 10.1093/mnras/staa3734 | |
dc.identifier.other | ORCID: /0000-0002-6733-5556/work/89628326 | |
dc.identifier.uri | https://hdl.handle.net/10023/21501 | |
dc.description | Funding: AP, ND, and JHS are supported by a Vidi grant awarded to ND by the Netherlands Organization for Scientific Research (NWO). IP and EC are supported by the Vidi grant 639.042.525. Further support for HST program GO-13108 was provided by NASA through a grant from the STScI. | en |
dc.description.abstract | The accretion behaviour in low-mass X-ray binaries (LMXBs) at low luminosities, especially at <1034 erg s−1, is not well known. This is an important regime to study to obtain a complete understanding of the accretion process in LMXBs, and to determine if systems that host neutron stars with accretion-heated crusts can be used probe the physics of dense matter (which requires their quiescent thermal emission to be uncontaminated by residual accretion). Here, we examine ultraviolet (UV) and X-ray data obtained when EXO 0748–676, a crust-cooling source, was in quiescence. Our Hubble Space Telescope spectroscopy observations do not detect the far-UV continuum emission, but do reveal one strong emission line, C iv. The line is relatively broad (≳3500 km s−1), which could indicate that it results from an outflow such as a pulsar wind. By studying several epochs of X-ray and near-UV data obtained with XMM–Newton, we find no clear indication that the emission in the two wavebands is connected. Moreover, the luminosity ratio of LX/LUV ≳ 100 is much higher than that observed from neutron star LMXBs that exhibit low-level accretion in quiescence. Taken together, this suggests that the UV and X-ray emission of EXO 0748–676 may have different origins, and that thermal emission from crust-cooling of the neutron star, rather than ongoing low-level accretion, may be dominating the observed quiescent X-ray flux evolution of this LMXB. | |
dc.format.extent | 10 | |
dc.format.extent | 1492272 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Accretion | en |
dc.subject | Accretion discs | en |
dc.subject | Ultraviolet: general | en |
dc.subject | X-rays: binaries | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | UV and X-ray observations of the neutron star LMXB EXO 0748–676 in its quiescent state | en |
dc.type | Journal article | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | 10.1093/mnras/staa3734 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://doi.org/10.5281/zenodo.3908291 | en |
dc.identifier.url | https://doi.org/10.1093/mnras/stab188 | en |
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