ASAS J071404+7004.3 – a close, bright nova-like cataclysmic variable with gusty winds
ABSTRACT Despite being bright (V ≃ 11.8) and nearby (d = 212 pc) ASAS J071404+7004.3 has only recently been identified as a nova-like cataclysmic variable. We present time-resolved optical spectroscopy obtained at the Isaac Newton and the Hiltner and McGraw-Hill Telescopes, together with Swift X-ray...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2022-03, Vol.510 (3), p.3605-3621 |
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| creator | Inight, K Gänsicke, B T Blondel, D Boyd, D Ashley, R P Knigge, C Long, K S Marsh, T R McCleery, J Scaringi, S Steeghs, D Thorstensen, J R Vanmunster, T Wheatley, P J |
| description | ABSTRACT
Despite being bright (V ≃ 11.8) and nearby (d = 212 pc) ASAS J071404+7004.3 has only recently been identified as a nova-like cataclysmic variable. We present time-resolved optical spectroscopy obtained at the Isaac Newton and the Hiltner and McGraw-Hill Telescopes, together with Swift X-ray and ultraviolet observations. We combined these with TESS photometry and find a period of 3.28 h and a mass transfer rate of $4\!-\!9\times 10^{-9}\, {\mathrm{M_{\odot }\, yr}^{-1}}$. Historical photometry shows at least one low state establishing the system as a VY Scl star. Our high-cadence spectroscopy also revealed rapidly changing winds emanating from the accretion disc. We have modelled these using the Monte Carlo python code and shown that all the emission lines could emanate from the wind – which would explain the lack of double-peaked lines in such systems. In passing, we discuss the effect of variability on the position of cataclysmic variables in the Gaia Hertzsprung–Russell diagram. |
| doi_str_mv | 10.1093/mnras/stab3662 |
| format | Article |
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Despite being bright (V ≃ 11.8) and nearby (d = 212 pc) ASAS J071404+7004.3 has only recently been identified as a nova-like cataclysmic variable. We present time-resolved optical spectroscopy obtained at the Isaac Newton and the Hiltner and McGraw-Hill Telescopes, together with Swift X-ray and ultraviolet observations. We combined these with TESS photometry and find a period of 3.28 h and a mass transfer rate of $4\!-\!9\times 10^{-9}\, {\mathrm{M_{\odot }\, yr}^{-1}}$. Historical photometry shows at least one low state establishing the system as a VY Scl star. Our high-cadence spectroscopy also revealed rapidly changing winds emanating from the accretion disc. We have modelled these using the Monte Carlo python code and shown that all the emission lines could emanate from the wind – which would explain the lack of double-peaked lines in such systems. In passing, we discuss the effect of variability on the position of cataclysmic variables in the Gaia Hertzsprung–Russell diagram.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stab3662</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2022-03, Vol.510 (3), p.3605-3621</ispartof><rights>2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2022</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c273t-5ca231816df715643cd4515bdcd1834475249f6fc0a9e71917752b116ff4ba3f3</citedby><cites>FETCH-LOGICAL-c273t-5ca231816df715643cd4515bdcd1834475249f6fc0a9e71917752b116ff4ba3f3</cites><orcidid>0000-0002-2498-7589 ; 0000-0003-0771-4746 ; 0000-0003-1452-2240 ; 0000-0001-5387-7189 ; 0000-0002-2200-2416</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stab3662$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Inight, K</creatorcontrib><creatorcontrib>Gänsicke, B T</creatorcontrib><creatorcontrib>Blondel, D</creatorcontrib><creatorcontrib>Boyd, D</creatorcontrib><creatorcontrib>Ashley, R P</creatorcontrib><creatorcontrib>Knigge, C</creatorcontrib><creatorcontrib>Long, K S</creatorcontrib><creatorcontrib>Marsh, T R</creatorcontrib><creatorcontrib>McCleery, J</creatorcontrib><creatorcontrib>Scaringi, S</creatorcontrib><creatorcontrib>Steeghs, D</creatorcontrib><creatorcontrib>Thorstensen, J R</creatorcontrib><creatorcontrib>Vanmunster, T</creatorcontrib><creatorcontrib>Wheatley, P J</creatorcontrib><title>ASAS J071404+7004.3 – a close, bright nova-like cataclysmic variable with gusty winds</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
Despite being bright (V ≃ 11.8) and nearby (d = 212 pc) ASAS J071404+7004.3 has only recently been identified as a nova-like cataclysmic variable. We present time-resolved optical spectroscopy obtained at the Isaac Newton and the Hiltner and McGraw-Hill Telescopes, together with Swift X-ray and ultraviolet observations. We combined these with TESS photometry and find a period of 3.28 h and a mass transfer rate of $4\!-\!9\times 10^{-9}\, {\mathrm{M_{\odot }\, yr}^{-1}}$. Historical photometry shows at least one low state establishing the system as a VY Scl star. Our high-cadence spectroscopy also revealed rapidly changing winds emanating from the accretion disc. We have modelled these using the Monte Carlo python code and shown that all the emission lines could emanate from the wind – which would explain the lack of double-peaked lines in such systems. In passing, we discuss the effect of variability on the position of cataclysmic variables in the Gaia Hertzsprung–Russell diagram.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><recordid>eNqFkLtOw0AQRVcIJEygpd4WgZMd78suo4inIlEEKgprvPYmBieOdp2gdGmp-YF8Sz4lX4IhUFPNaO49UxxCzoF1gSW8N5059D3fYMaVig5IAFzJMEqUOiQBY1yGsQY4JifevzLGBI9UQF76o_5ot_54YBoEE5e6Dbp8u9mtP7cbpKaqfXFFM1eOJw2d1UsMq_KtoAYbNNXKT0tDl-hKzKqCvpfNhI4Xvlm16yz3p-TIYuWLs9_ZIc8310-Du3D4eHs_6A9DE2nehNJgxCEGlVsNUgluciFBZrnJIeZCaBmJxCprGCaFhgR0e8kAlLUiQ255h3T3f42rvXeFTeeunKJbpcDSbzXpj5r0T00LXOyBejH_r_sF3p1opw</recordid><startdate>20220301</startdate><enddate>20220301</enddate><creator>Inight, K</creator><creator>Gänsicke, B T</creator><creator>Blondel, D</creator><creator>Boyd, D</creator><creator>Ashley, R P</creator><creator>Knigge, C</creator><creator>Long, K S</creator><creator>Marsh, T R</creator><creator>McCleery, J</creator><creator>Scaringi, S</creator><creator>Steeghs, D</creator><creator>Thorstensen, J R</creator><creator>Vanmunster, T</creator><creator>Wheatley, P J</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-2498-7589</orcidid><orcidid>https://orcid.org/0000-0003-0771-4746</orcidid><orcidid>https://orcid.org/0000-0003-1452-2240</orcidid><orcidid>https://orcid.org/0000-0001-5387-7189</orcidid><orcidid>https://orcid.org/0000-0002-2200-2416</orcidid></search><sort><creationdate>20220301</creationdate><title>ASAS J071404+7004.3 – a close, bright nova-like cataclysmic variable with gusty winds</title><author>Inight, K ; Gänsicke, B T ; Blondel, D ; Boyd, D ; Ashley, R P ; Knigge, C ; Long, K S ; Marsh, T R ; McCleery, J ; Scaringi, S ; Steeghs, D ; Thorstensen, J R ; Vanmunster, T ; Wheatley, P J</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c273t-5ca231816df715643cd4515bdcd1834475249f6fc0a9e71917752b116ff4ba3f3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Inight, K</creatorcontrib><creatorcontrib>Gänsicke, B T</creatorcontrib><creatorcontrib>Blondel, D</creatorcontrib><creatorcontrib>Boyd, D</creatorcontrib><creatorcontrib>Ashley, R P</creatorcontrib><creatorcontrib>Knigge, C</creatorcontrib><creatorcontrib>Long, K S</creatorcontrib><creatorcontrib>Marsh, T R</creatorcontrib><creatorcontrib>McCleery, J</creatorcontrib><creatorcontrib>Scaringi, S</creatorcontrib><creatorcontrib>Steeghs, D</creatorcontrib><creatorcontrib>Thorstensen, J R</creatorcontrib><creatorcontrib>Vanmunster, T</creatorcontrib><creatorcontrib>Wheatley, P J</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Inight, K</au><au>Gänsicke, B T</au><au>Blondel, D</au><au>Boyd, D</au><au>Ashley, R P</au><au>Knigge, C</au><au>Long, K S</au><au>Marsh, T R</au><au>McCleery, J</au><au>Scaringi, S</au><au>Steeghs, D</au><au>Thorstensen, J R</au><au>Vanmunster, T</au><au>Wheatley, P J</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>ASAS J071404+7004.3 – a close, bright nova-like cataclysmic variable with gusty winds</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2022-03-01</date><risdate>2022</risdate><volume>510</volume><issue>3</issue><spage>3605</spage><epage>3621</epage><pages>3605-3621</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Despite being bright (V ≃ 11.8) and nearby (d = 212 pc) ASAS J071404+7004.3 has only recently been identified as a nova-like cataclysmic variable. We present time-resolved optical spectroscopy obtained at the Isaac Newton and the Hiltner and McGraw-Hill Telescopes, together with Swift X-ray and ultraviolet observations. We combined these with TESS photometry and find a period of 3.28 h and a mass transfer rate of $4\!-\!9\times 10^{-9}\, {\mathrm{M_{\odot }\, yr}^{-1}}$. Historical photometry shows at least one low state establishing the system as a VY Scl star. Our high-cadence spectroscopy also revealed rapidly changing winds emanating from the accretion disc. We have modelled these using the Monte Carlo python code and shown that all the emission lines could emanate from the wind – which would explain the lack of double-peaked lines in such systems. In passing, we discuss the effect of variability on the position of cataclysmic variables in the Gaia Hertzsprung–Russell diagram.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stab3662</doi><tpages>17</tpages><orcidid>https://orcid.org/0000-0002-2498-7589</orcidid><orcidid>https://orcid.org/0000-0003-0771-4746</orcidid><orcidid>https://orcid.org/0000-0003-1452-2240</orcidid><orcidid>https://orcid.org/0000-0001-5387-7189</orcidid><orcidid>https://orcid.org/0000-0002-2200-2416</orcidid><oa>free_for_read</oa></addata></record> |
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| title | ASAS J071404+7004.3 – a close, bright nova-like cataclysmic variable with gusty winds |
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