Precise parameters for both white dwarfs in the eclipsing binary CSS 41177
We present ULTRACAM photometry and X-Shooter spectroscopy of the eclipsing double white dwarf binary CSS 41177, the only such system that is also a double-lined spectroscopic binary. Combined modelling of the light curves and radial velocities yield masses and radii for both white dwarfs without the...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2014-03, Vol.438 (4), p.3399-3408 |
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| creator | Bours, M. C. P. Marsh, T. R. Parsons, S. G. Copperwheat, C. M. Dhillon, V. S. Littlefair, S. P. Gänsicke, B. T. Gianninas, A. Tremblay, P.-E. |
| description | We present ULTRACAM photometry and X-Shooter spectroscopy of the eclipsing double white dwarf binary CSS 41177, the only such system that is also a double-lined spectroscopic binary. Combined modelling of the light curves and radial velocities yield masses and radii for both white dwarfs without the need to assume mass-radius relations. We find that the primary white dwarf has a mass of M
1 = 0.38 ± 0.02 M and a radius of R
1 = 0.0222 ± 0.0004 R. The secondary white dwarf's mass and radius are M
2 = 0.32 ± 0.01 M and R
2 = 0.0207 ± 0.0004 R, and its temperature and surface gravity (T
2 = 11678 ± 313 K, log(g
2) = 7.32 ± 0.02) put it close to the white dwarf instability strip. However, we find no evidence for pulsations to roughly 0.5 per cent relative amplitude. Both masses and radii are consistent with helium white dwarf models with thin hydrogen envelopes of ≤10−4
M
*. The two stars will merge in 1.14 ± 0.07 Gyr due to angular momentum loss via gravitational wave emission. |
| doi_str_mv | 10.1093/mnras/stt2453 |
| format | Article |
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1 = 0.38 ± 0.02 M and a radius of R
1 = 0.0222 ± 0.0004 R. The secondary white dwarf's mass and radius are M
2 = 0.32 ± 0.01 M and R
2 = 0.0207 ± 0.0004 R, and its temperature and surface gravity (T
2 = 11678 ± 313 K, log(g
2) = 7.32 ± 0.02) put it close to the white dwarf instability strip. However, we find no evidence for pulsations to roughly 0.5 per cent relative amplitude. Both masses and radii are consistent with helium white dwarf models with thin hydrogen envelopes of ≤10−4
M
*. The two stars will merge in 1.14 ± 0.07 Gyr due to angular momentum loss via gravitational wave emission.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stt2453</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Gravity ; Hydrogen ; Pulsars ; Star & galaxy formation ; White dwarfs</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2014-03, Vol.438 (4), p.3399-3408</ispartof><rights>2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2014</rights><rights>Copyright Oxford University Press, UK Mar 11, 2014</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c337t-14ae38cf843b365630e5541898242f23df62c60a374c265830a54f9e8cb0ad8e3</citedby><cites>FETCH-LOGICAL-c337t-14ae38cf843b365630e5541898242f23df62c60a374c265830a54f9e8cb0ad8e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stt2453$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Bours, M. C. P.</creatorcontrib><creatorcontrib>Marsh, T. R.</creatorcontrib><creatorcontrib>Parsons, S. G.</creatorcontrib><creatorcontrib>Copperwheat, C. M.</creatorcontrib><creatorcontrib>Dhillon, V. S.</creatorcontrib><creatorcontrib>Littlefair, S. P.</creatorcontrib><creatorcontrib>Gänsicke, B. T.</creatorcontrib><creatorcontrib>Gianninas, A.</creatorcontrib><creatorcontrib>Tremblay, P.-E.</creatorcontrib><title>Precise parameters for both white dwarfs in the eclipsing binary CSS 41177</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Mon. Not. R. Astron. Soc</addtitle><description>We present ULTRACAM photometry and X-Shooter spectroscopy of the eclipsing double white dwarf binary CSS 41177, the only such system that is also a double-lined spectroscopic binary. Combined modelling of the light curves and radial velocities yield masses and radii for both white dwarfs without the need to assume mass-radius relations. We find that the primary white dwarf has a mass of M
1 = 0.38 ± 0.02 M and a radius of R
1 = 0.0222 ± 0.0004 R. The secondary white dwarf's mass and radius are M
2 = 0.32 ± 0.01 M and R
2 = 0.0207 ± 0.0004 R, and its temperature and surface gravity (T
2 = 11678 ± 313 K, log(g
2) = 7.32 ± 0.02) put it close to the white dwarf instability strip. However, we find no evidence for pulsations to roughly 0.5 per cent relative amplitude. Both masses and radii are consistent with helium white dwarf models with thin hydrogen envelopes of ≤10−4
M
*. The two stars will merge in 1.14 ± 0.07 Gyr due to angular momentum loss via gravitational wave emission.</description><subject>Gravity</subject><subject>Hydrogen</subject><subject>Pulsars</subject><subject>Star & galaxy formation</subject><subject>White dwarfs</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><recordid>eNqFkEFLAzEUhIMoWKtH7wEvXta-5CXZ7FGKVqWgUD2HbJrYLe3umqQU_72r7d3TXD5mho-QawZ3DCqcbNto0yTlzIXEEzJiqGTBK6VOyQgAZaFLxs7JRUprABDI1Yi8vEXvmuRpb6Pd-uxjoqGLtO7yiu5XTfZ0ubcxJNq0NK889W7T9KlpP2ndtDZ-0-liQQVjZXlJzoLdJH91zDH5eHx4nz4V89fZ8_R-XjjEMhdMWI_aBS2wHg4qBC-lYLrSXPDAcRkUdwoslsJxJTWClSJUXrsa7FJ7HJObQ28fu6-dT9msu11sh0nDJHAQsgI9UMWBcrFLKfpg-thsh8OGgfnVZf50maOugb898N2u_wf9AWOQayg</recordid><startdate>20140311</startdate><enddate>20140311</enddate><creator>Bours, M. C. P.</creator><creator>Marsh, T. R.</creator><creator>Parsons, S. G.</creator><creator>Copperwheat, C. M.</creator><creator>Dhillon, V. S.</creator><creator>Littlefair, S. P.</creator><creator>Gänsicke, B. T.</creator><creator>Gianninas, A.</creator><creator>Tremblay, P.-E.</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20140311</creationdate><title>Precise parameters for both white dwarfs in the eclipsing binary CSS 41177</title><author>Bours, M. C. P. ; Marsh, T. R. ; Parsons, S. G. ; Copperwheat, C. M. ; Dhillon, V. S. ; Littlefair, S. P. ; Gänsicke, B. T. ; Gianninas, A. ; Tremblay, P.-E.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c337t-14ae38cf843b365630e5541898242f23df62c60a374c265830a54f9e8cb0ad8e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Gravity</topic><topic>Hydrogen</topic><topic>Pulsars</topic><topic>Star & galaxy formation</topic><topic>White dwarfs</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bours, M. C. P.</creatorcontrib><creatorcontrib>Marsh, T. R.</creatorcontrib><creatorcontrib>Parsons, S. G.</creatorcontrib><creatorcontrib>Copperwheat, C. M.</creatorcontrib><creatorcontrib>Dhillon, V. S.</creatorcontrib><creatorcontrib>Littlefair, S. P.</creatorcontrib><creatorcontrib>Gänsicke, B. T.</creatorcontrib><creatorcontrib>Gianninas, A.</creatorcontrib><creatorcontrib>Tremblay, P.-E.</creatorcontrib><collection>CrossRef</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_linktorsrc</fulltext></delivery><addata><au>Bours, M. C. P.</au><au>Marsh, T. R.</au><au>Parsons, S. G.</au><au>Copperwheat, C. M.</au><au>Dhillon, V. S.</au><au>Littlefair, S. P.</au><au>Gänsicke, B. T.</au><au>Gianninas, A.</au><au>Tremblay, P.-E.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Precise parameters for both white dwarfs in the eclipsing binary CSS 41177</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Mon. Not. R. Astron. Soc</stitle><date>2014-03-11</date><risdate>2014</risdate><volume>438</volume><issue>4</issue><spage>3399</spage><epage>3408</epage><pages>3399-3408</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We present ULTRACAM photometry and X-Shooter spectroscopy of the eclipsing double white dwarf binary CSS 41177, the only such system that is also a double-lined spectroscopic binary. Combined modelling of the light curves and radial velocities yield masses and radii for both white dwarfs without the need to assume mass-radius relations. We find that the primary white dwarf has a mass of M
1 = 0.38 ± 0.02 M and a radius of R
1 = 0.0222 ± 0.0004 R. The secondary white dwarf's mass and radius are M
2 = 0.32 ± 0.01 M and R
2 = 0.0207 ± 0.0004 R, and its temperature and surface gravity (T
2 = 11678 ± 313 K, log(g
2) = 7.32 ± 0.02) put it close to the white dwarf instability strip. However, we find no evidence for pulsations to roughly 0.5 per cent relative amplitude. Both masses and radii are consistent with helium white dwarf models with thin hydrogen envelopes of ≤10−4
M
*. The two stars will merge in 1.14 ± 0.07 Gyr due to angular momentum loss via gravitational wave emission.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stt2453</doi><tpages>10</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Gravity Hydrogen Pulsars Star & galaxy formation White dwarfs |
| title | Precise parameters for both white dwarfs in the eclipsing binary CSS 41177 |
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