Further X-ray observations of EXO 0748−676 in quiescence: evidence for a cooling neutron star crust
In late 2008, the quasi-persistent neutron star X-ray transient and eclipsing binary EXO 0748−676 started a transition from outburst to quiescence, after it actively accreted for more than 24 yr. In a previous work, we discussed Chandra and Swift observations obtained during the first 5 months of th...
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| creator | Degenaar, N. Wolff, M. T. Ray, P. S. Wood, K. S. Homan, J. Lewin, W. H. G. Jonker, P. G. Cackett, E. M. Miller, J. M. Brown, E. F. Wijnands, R. |
| description | In late 2008, the quasi-persistent neutron star X-ray transient and eclipsing binary EXO 0748−676 started a transition from outburst to quiescence, after it actively accreted for more than 24 yr. In a previous work, we discussed Chandra and Swift observations obtained during the first 5 months of this transition. Here, we report on further X-ray observations of EXO 0748−676, extending the quiescent monitoring to 1.6 yr. Chandra and XMM-Newton data reveal quiescent X-ray spectra composed of a soft, thermal component that is well fitted by a neutron star atmosphere model. An additional hard power-law tail is detected that changes non-monotonically over time, contributing between 4 and 20 per cent to the total unabsorbed 0.5-10 keV flux. The combined set of Chandra, XMM-Newton and Swift data reveals that the thermal bolometric luminosity fades from ∼ 1 × 1034 to 6 × 1033 (D/7.4 kpc)2 erg s −1, whereas the inferred neutron star effective temperature decreases from ∼124 to 109 eV. We interpret the observed decay as cooling of the neutron star crust and show that the fractional quiescent temperature change of EXO 0748−676 is markedly smaller than observed for three other neutron star X-ray binaries that underwent prolonged accretion outbursts. |
| doi_str_mv | 10.1111/j.1365-2966.2010.17562.x |
| format | Article |
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T. ; Ray, P. S. ; Wood, K. S. ; Homan, J. ; Lewin, W. H. G. ; Jonker, P. G. ; Cackett, E. M. ; Miller, J. M. ; Brown, E. F. ; Wijnands, R.</creator><creatorcontrib>Degenaar, N. ; Wolff, M. T. ; Ray, P. S. ; Wood, K. S. ; Homan, J. ; Lewin, W. H. G. ; Jonker, P. G. ; Cackett, E. M. ; Miller, J. M. ; Brown, E. F. ; Wijnands, R.</creatorcontrib><description>In late 2008, the quasi-persistent neutron star X-ray transient and eclipsing binary EXO 0748−676 started a transition from outburst to quiescence, after it actively accreted for more than 24 yr. In a previous work, we discussed Chandra and Swift observations obtained during the first 5 months of this transition. Here, we report on further X-ray observations of EXO 0748−676, extending the quiescent monitoring to 1.6 yr. Chandra and XMM-Newton data reveal quiescent X-ray spectra composed of a soft, thermal component that is well fitted by a neutron star atmosphere model. An additional hard power-law tail is detected that changes non-monotonically over time, contributing between 4 and 20 per cent to the total unabsorbed 0.5-10 keV flux. The combined set of Chandra, XMM-Newton and Swift data reveals that the thermal bolometric luminosity fades from ∼ 1 × 1034 to 6 × 1033 (D/7.4 kpc)2 erg s −1, whereas the inferred neutron star effective temperature decreases from ∼124 to 109 eV. 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We interpret the observed decay as cooling of the neutron star crust and show that the fractional quiescent temperature change of EXO 0748−676 is markedly smaller than observed for three other neutron star X-ray binaries that underwent prolonged accretion outbursts.</description><subject>accretion</subject><subject>accretion discs</subject><subject>accretion, accretion discs</subject><subject>Astronomy</subject><subject>binaries: eclipsing</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Luminosity</subject><subject>Spectrum analysis</subject><subject>Stars & galaxies</subject><subject>stars: individual: EXO 0748−676</subject><subject>stars: neutron</subject><subject>X-ray astronomy</subject><subject>X-rays: binaries</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><recordid>eNp1kMtqGzEUhkVoIW6adxCBLsc9us90UShpbuAmEFoSshGyLq1cd-RIM6n9Bl3nEfMknYmDN6Xa6KDzf7_gQwgTmJLhvF9MCZOioo2UUwrjqxKSTtd7aLJbvEITACaqWhGyj96UsgAAzqicIH_a5-6Hz_i2ymaD07z4_GC6mNqCU8Ant1cYFK-f_jxKJXFs8X0ffbG-tf4D9g_RjRMOKWODbUrL2H7Hre-7nFpcOpOxzX3p3qLXwSyLP3y5D9C305Ovx-fV7Ors4vjTrLIcOK0aZ4hnToGHBjhnjITA58xZX899ICyIWkrGpRN-Hih1nDvhrCBOkUaBCuwAHW17Vznd9750epH63A5f6loCCCBUDaF3LyFTrFmGbFobi17l-MvkjaYcKK95PeQ-bnO_49JvdnsCehSvF3r0q0e_ehSvn8Xrtf5yef08DgVsW5D61X_w6h98oKotFUvn1zvO5J9aKqaEvrk8G9hZc_f5mmjF_gJNR5aB</recordid><startdate>201104</startdate><enddate>201104</enddate><creator>Degenaar, N.</creator><creator>Wolff, M. T.</creator><creator>Ray, P. S.</creator><creator>Wood, K. S.</creator><creator>Homan, J.</creator><creator>Lewin, W. H. G.</creator><creator>Jonker, P. G.</creator><creator>Cackett, E. M.</creator><creator>Miller, J. M.</creator><creator>Brown, E. F.</creator><creator>Wijnands, R.</creator><general>Blackwell Publishing Ltd</general><general>Wiley-Blackwell</general><general>Oxford University Press</general><scope>BSCLL</scope><scope>IQODW</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>201104</creationdate><title>Further X-ray observations of EXO 0748−676 in quiescence: evidence for a cooling neutron star crust</title><author>Degenaar, N. ; Wolff, M. T. ; Ray, P. S. ; Wood, K. S. ; Homan, J. ; Lewin, W. H. G. ; Jonker, P. G. ; Cackett, E. M. ; Miller, J. M. ; Brown, E. 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S.</creatorcontrib><creatorcontrib>Homan, J.</creatorcontrib><creatorcontrib>Lewin, W. H. G.</creatorcontrib><creatorcontrib>Jonker, P. G.</creatorcontrib><creatorcontrib>Cackett, E. M.</creatorcontrib><creatorcontrib>Miller, J. M.</creatorcontrib><creatorcontrib>Brown, E. F.</creatorcontrib><creatorcontrib>Wijnands, R.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Degenaar, N.</au><au>Wolff, M. T.</au><au>Ray, P. S.</au><au>Wood, K. S.</au><au>Homan, J.</au><au>Lewin, W. H. G.</au><au>Jonker, P. G.</au><au>Cackett, E. M.</au><au>Miller, J. M.</au><au>Brown, E. F.</au><au>Wijnands, R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Further X-ray observations of EXO 0748−676 in quiescence: evidence for a cooling neutron star crust</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Monthly Notices of the Royal Astronomical Society</stitle><date>2011-04</date><risdate>2011</risdate><volume>412</volume><issue>3</issue><spage>1409</spage><epage>1418</epage><pages>1409-1418</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><coden>MNRAA4</coden><abstract>In late 2008, the quasi-persistent neutron star X-ray transient and eclipsing binary EXO 0748−676 started a transition from outburst to quiescence, after it actively accreted for more than 24 yr. In a previous work, we discussed Chandra and Swift observations obtained during the first 5 months of this transition. Here, we report on further X-ray observations of EXO 0748−676, extending the quiescent monitoring to 1.6 yr. Chandra and XMM-Newton data reveal quiescent X-ray spectra composed of a soft, thermal component that is well fitted by a neutron star atmosphere model. An additional hard power-law tail is detected that changes non-monotonically over time, contributing between 4 and 20 per cent to the total unabsorbed 0.5-10 keV flux. The combined set of Chandra, XMM-Newton and Swift data reveals that the thermal bolometric luminosity fades from ∼ 1 × 1034 to 6 × 1033 (D/7.4 kpc)2 erg s −1, whereas the inferred neutron star effective temperature decreases from ∼124 to 109 eV. We interpret the observed decay as cooling of the neutron star crust and show that the fractional quiescent temperature change of EXO 0748−676 is markedly smaller than observed for three other neutron star X-ray binaries that underwent prolonged accretion outbursts.</abstract><cop>Oxford, UK</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1111/j.1365-2966.2010.17562.x</doi><tpages>10</tpages></addata></record> |
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| subjects | accretion accretion discs accretion, accretion discs Astronomy binaries: eclipsing Earth, ocean, space Exact sciences and technology Luminosity Spectrum analysis Stars & galaxies stars: individual: EXO 0748−676 stars: neutron X-ray astronomy X-rays: binaries |
| title | Further X-ray observations of EXO 0748−676 in quiescence: evidence for a cooling neutron star crust |
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