Doppler tomography and photometry of the cataclysmic variable 1RXS J064434.5+334451
We have obtained simultaneous photometric and spectroscopic observations of the cataclysmic variable 1RXS J064434.5+334451. We have calibrated the spectra for slit losses using simultaneous photometry, allowing us to construct reliable Doppler images from H... and He ii 4686-A emission lines. We hav...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2017-01, Vol.464 (1), p.104-104 |
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| creator | Santisteban, J V Hernandez Echevarria, J Michel, R Costero, R |
| description | We have obtained simultaneous photometric and spectroscopic observations of the cataclysmic variable 1RXS J064434.5+334451. We have calibrated the spectra for slit losses using simultaneous photometry, allowing us to construct reliable Doppler images from H... and He ii 4686-A emission lines. We have improved the ephemeris of the object based on new photometric eclipse timings, obtaining HJD = 245 3403.759 533 + 0.269 374 46E. Some eclipses present a clear internal structure, which we attribute to a central He ii emission region surrounding the white dwarf, a finding supported by Doppler tomography. This indicates that the system has a large inclination angle i = 78 plus or minus 2... We have also analysed the radial velocity curve from the emission lines to measure its semi-amplitude, K sub( 1), from H... and He ii 4686 and derive the masses of the components M sub( 1) = 0.82 plus or minus 0.06 M..., M sub( 2) = 0.78 plus or minus 0.04 M... and their separation a = 2.01 plus or minus 0.06 R... The Doppler tomography and other observed features in this nova-like system strongly suggest that this is a SW Sex type system. (ProQuest: ... denotes formulae/symbols omitted.) |
| doi_str_mv | 10.1093/mnras/stw2282 |
| format | Article |
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We have calibrated the spectra for slit losses using simultaneous photometry, allowing us to construct reliable Doppler images from H... and He ii 4686-A emission lines. We have improved the ephemeris of the object based on new photometric eclipse timings, obtaining HJD = 245 3403.759 533 + 0.269 374 46E. Some eclipses present a clear internal structure, which we attribute to a central He ii emission region surrounding the white dwarf, a finding supported by Doppler tomography. This indicates that the system has a large inclination angle i = 78 plus or minus 2... We have also analysed the radial velocity curve from the emission lines to measure its semi-amplitude, K sub( 1), from H... and He ii 4686 and derive the masses of the components M sub( 1) = 0.82 plus or minus 0.06 M..., M sub( 2) = 0.78 plus or minus 0.04 M... and their separation a = 2.01 plus or minus 0.06 R... The Doppler tomography and other observed features in this nova-like system strongly suggest that this is a SW Sex type system. 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We have calibrated the spectra for slit losses using simultaneous photometry, allowing us to construct reliable Doppler images from H... and He ii 4686-A emission lines. We have improved the ephemeris of the object based on new photometric eclipse timings, obtaining HJD = 245 3403.759 533 + 0.269 374 46E. Some eclipses present a clear internal structure, which we attribute to a central He ii emission region surrounding the white dwarf, a finding supported by Doppler tomography. This indicates that the system has a large inclination angle i = 78 plus or minus 2... We have also analysed the radial velocity curve from the emission lines to measure its semi-amplitude, K sub( 1), from H... and He ii 4686 and derive the masses of the components M sub( 1) = 0.82 plus or minus 0.06 M..., M sub( 2) = 0.78 plus or minus 0.04 M... and their separation a = 2.01 plus or minus 0.06 R... The Doppler tomography and other observed features in this nova-like system strongly suggest that this is a SW Sex type system. (ProQuest: ... denotes formulae/symbols omitted.)</description><subject>Astronomy</subject><subject>Cataclysmic variables</subject><subject>Doppler</subject><subject>Doppler effect</subject><subject>Eclipses</subject><subject>Photometry</subject><subject>Spectrum analysis</subject><subject>Symbols</subject><subject>Tomography</subject><subject>White dwarf stars</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNqFkU1Lw0AQhhdRsFaP3he8CJJ2dmez2RylflMQrIK3MEk2tiXpxt1Uyb83Wk9ePA0Mzzsw78PYqYCJgBSnzcZTmIbuU0oj99hIoI4jmWq9z0YAGEcmEeKQHYWwBgCFUo_Y4sq1bW0971zj3jy1y57TpuTt0g0b2_meu4p3S8sL6qio-9CsCv5BfkV5bbl4el3wB9BKoZrEF4hKxeKYHVRUB3vyO8fs5eb6eXYXzR9v72eX86hAFF1ElawoKSsgiSolJVNTGrC5rUAlpTG6KHMgQwiGFIqEwGgLiDpP07yAHMfsfHe39e59a0OXNatQ2LqmjXXbkAmjVYxaDJn_0RgSYwSYAT37g67d1m-GRwZqKC2ROHQ3ZtGOKrwLwdsqa_2qId9nArJvG9mPjezXBn4BN_p78g</recordid><startdate>20170101</startdate><enddate>20170101</enddate><creator>Santisteban, J V Hernandez</creator><creator>Echevarria, J</creator><creator>Michel, R</creator><creator>Costero, R</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20170101</creationdate><title>Doppler tomography and photometry of the cataclysmic variable 1RXS J064434.5+334451</title><author>Santisteban, J V Hernandez ; Echevarria, J ; Michel, R ; Costero, R</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c331t-af2fa7df0a2349a4298d80ebef047d886cdb0a8a308a4317a086e0336b99bc0b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Astronomy</topic><topic>Cataclysmic variables</topic><topic>Doppler</topic><topic>Doppler effect</topic><topic>Eclipses</topic><topic>Photometry</topic><topic>Spectrum analysis</topic><topic>Symbols</topic><topic>Tomography</topic><topic>White dwarf stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Santisteban, J V Hernandez</creatorcontrib><creatorcontrib>Echevarria, J</creatorcontrib><creatorcontrib>Michel, R</creatorcontrib><creatorcontrib>Costero, R</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Santisteban, J V Hernandez</au><au>Echevarria, J</au><au>Michel, R</au><au>Costero, R</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Doppler tomography and photometry of the cataclysmic variable 1RXS J064434.5+334451</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2017-01-01</date><risdate>2017</risdate><volume>464</volume><issue>1</issue><spage>104</spage><epage>104</epage><pages>104-104</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We have obtained simultaneous photometric and spectroscopic observations of the cataclysmic variable 1RXS J064434.5+334451. We have calibrated the spectra for slit losses using simultaneous photometry, allowing us to construct reliable Doppler images from H... and He ii 4686-A emission lines. We have improved the ephemeris of the object based on new photometric eclipse timings, obtaining HJD = 245 3403.759 533 + 0.269 374 46E. Some eclipses present a clear internal structure, which we attribute to a central He ii emission region surrounding the white dwarf, a finding supported by Doppler tomography. This indicates that the system has a large inclination angle i = 78 plus or minus 2... We have also analysed the radial velocity curve from the emission lines to measure its semi-amplitude, K sub( 1), from H... and He ii 4686 and derive the masses of the components M sub( 1) = 0.82 plus or minus 0.06 M..., M sub( 2) = 0.78 plus or minus 0.04 M... and their separation a = 2.01 plus or minus 0.06 R... The Doppler tomography and other observed features in this nova-like system strongly suggest that this is a SW Sex type system. (ProQuest: ... denotes formulae/symbols omitted.)</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stw2282</doi><tpages>1</tpages></addata></record> |
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| language | eng |
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| source | Oxford Journals Open Access Collection |
| subjects | Astronomy Cataclysmic variables Doppler Doppler effect Eclipses Photometry Spectrum analysis Symbols Tomography White dwarf stars |
| title | Doppler tomography and photometry of the cataclysmic variable 1RXS J064434.5+334451 |
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