HD 42477: coupled r modes, g modes, and a p mode in an A0Vnne star
ABSTRACT Several studies have shown that a number of stars pulsating in p modes lie between the β Cep and δ Sct instability strips in the Hertzsprung–Russell (HR) Diagram. At present, there is no certain understanding of how p modes can be excited in this Teff range. The goal of this work is to disp...
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creator | Kurtz, D W Jayaraman, R Sowicka, P Handler, G Saio, H Labadie-Bartz, J Lee, U |
description | ABSTRACT
Several studies have shown that a number of stars pulsating in p modes lie between the β Cep and δ Sct instability strips in the Hertzsprung–Russell (HR) Diagram. At present, there is no certain understanding of how p modes can be excited in this Teff range. The goal of this work is to disprove the conjecture that all stars pulsating in p modes and lying in this Teff range are the result of incorrect measurements of Teff, contamination, or the presence of unseen cooler companions lying in the δ Sct instability strip (given the high binary fraction of stars in this region of the HR Diagram). Using TESS data, we show that the A0Vnne star HD 42477 has a single p mode coupled to several r modes and/or g modes. We rule out a contaminating background star with a pixel-by-pixel examination, and we essentially rule out the possibility of a companion δ Sct star in a binary. We model the pulsations in HD 42477, and suggest that the g modes are excited by overstable convective core modes. We also conjecture that the single p mode is driven by coupling with the g modes, or that the oblateness of this rapidly-rotating star permits driving by He ii ionization in the equatorial region. |
doi_str_mv | 10.1093/mnras/stad858 |
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Several studies have shown that a number of stars pulsating in p modes lie between the β Cep and δ Sct instability strips in the Hertzsprung–Russell (HR) Diagram. At present, there is no certain understanding of how p modes can be excited in this Teff range. The goal of this work is to disprove the conjecture that all stars pulsating in p modes and lying in this Teff range are the result of incorrect measurements of Teff, contamination, or the presence of unseen cooler companions lying in the δ Sct instability strip (given the high binary fraction of stars in this region of the HR Diagram). Using TESS data, we show that the A0Vnne star HD 42477 has a single p mode coupled to several r modes and/or g modes. We rule out a contaminating background star with a pixel-by-pixel examination, and we essentially rule out the possibility of a companion δ Sct star in a binary. We model the pulsations in HD 42477, and suggest that the g modes are excited by overstable convective core modes. We also conjecture that the single p mode is driven by coupling with the g modes, or that the oblateness of this rapidly-rotating star permits driving by He ii ionization in the equatorial region.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stad858</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2023-05, Vol.521 (3), p.4765-4774</ispartof><rights>2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2023</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c270t-52996a9c220f90d8ee872c316b8eecd61729e277dd66aca304e944090ab4793c3</citedby><cites>FETCH-LOGICAL-c270t-52996a9c220f90d8ee872c316b8eecd61729e277dd66aca304e944090ab4793c3</cites><orcidid>0000-0002-6605-0268 ; 0000-0002-1015-3268 ; 0000-0002-2919-6786</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,777,781,1599,27905,27906</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stad858$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Kurtz, D W</creatorcontrib><creatorcontrib>Jayaraman, R</creatorcontrib><creatorcontrib>Sowicka, P</creatorcontrib><creatorcontrib>Handler, G</creatorcontrib><creatorcontrib>Saio, H</creatorcontrib><creatorcontrib>Labadie-Bartz, J</creatorcontrib><creatorcontrib>Lee, U</creatorcontrib><title>HD 42477: coupled r modes, g modes, and a p mode in an A0Vnne star</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
Several studies have shown that a number of stars pulsating in p modes lie between the β Cep and δ Sct instability strips in the Hertzsprung–Russell (HR) Diagram. At present, there is no certain understanding of how p modes can be excited in this Teff range. The goal of this work is to disprove the conjecture that all stars pulsating in p modes and lying in this Teff range are the result of incorrect measurements of Teff, contamination, or the presence of unseen cooler companions lying in the δ Sct instability strip (given the high binary fraction of stars in this region of the HR Diagram). Using TESS data, we show that the A0Vnne star HD 42477 has a single p mode coupled to several r modes and/or g modes. We rule out a contaminating background star with a pixel-by-pixel examination, and we essentially rule out the possibility of a companion δ Sct star in a binary. We model the pulsations in HD 42477, and suggest that the g modes are excited by overstable convective core modes. We also conjecture that the single p mode is driven by coupling with the g modes, or that the oblateness of this rapidly-rotating star permits driving by He ii ionization in the equatorial region.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><recordid>eNqFkLtOAzEQRS0EEkugpHdJgcn4sX7QhfAIUiQaoLUc24uCst6VHQr-HpOEmmrulY5mNAehSwo3FAyf9im7Mi1bF3Srj1BDuWwJM1IeowaAt0QrSk_RWSmfACA4kw26W9xjwYRSt9gPX-MmBpxxP4RYrvHHX3ApYIfHXcXrVDuewXtKEddj-RyddG5T4sVhTtDb48PrfEGWL0_P89mSeKZgS1pmjHTGMwadgaBj1Ip5TuWqRh8kVcxEplQIUjrvOIhohAADbiWU4Z5PENnv9XkoJcfOjnndu_xtKdhfAXYnwB4EVP5qz9e__kF_ABa3WwM</recordid><startdate>20230501</startdate><enddate>20230501</enddate><creator>Kurtz, D W</creator><creator>Jayaraman, R</creator><creator>Sowicka, P</creator><creator>Handler, G</creator><creator>Saio, H</creator><creator>Labadie-Bartz, J</creator><creator>Lee, U</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-6605-0268</orcidid><orcidid>https://orcid.org/0000-0002-1015-3268</orcidid><orcidid>https://orcid.org/0000-0002-2919-6786</orcidid></search><sort><creationdate>20230501</creationdate><title>HD 42477: coupled r modes, g modes, and a p mode in an A0Vnne star</title><author>Kurtz, D W ; Jayaraman, R ; Sowicka, P ; Handler, G ; Saio, H ; Labadie-Bartz, J ; Lee, U</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c270t-52996a9c220f90d8ee872c316b8eecd61729e277dd66aca304e944090ab4793c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kurtz, D W</creatorcontrib><creatorcontrib>Jayaraman, R</creatorcontrib><creatorcontrib>Sowicka, P</creatorcontrib><creatorcontrib>Handler, G</creatorcontrib><creatorcontrib>Saio, H</creatorcontrib><creatorcontrib>Labadie-Bartz, J</creatorcontrib><creatorcontrib>Lee, U</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>Kurtz, D W</au><au>Jayaraman, R</au><au>Sowicka, P</au><au>Handler, G</au><au>Saio, H</au><au>Labadie-Bartz, J</au><au>Lee, U</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>HD 42477: coupled r modes, g modes, and a p mode in an A0Vnne star</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2023-05-01</date><risdate>2023</risdate><volume>521</volume><issue>3</issue><spage>4765</spage><epage>4774</epage><pages>4765-4774</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Several studies have shown that a number of stars pulsating in p modes lie between the β Cep and δ Sct instability strips in the Hertzsprung–Russell (HR) Diagram. At present, there is no certain understanding of how p modes can be excited in this Teff range. The goal of this work is to disprove the conjecture that all stars pulsating in p modes and lying in this Teff range are the result of incorrect measurements of Teff, contamination, or the presence of unseen cooler companions lying in the δ Sct instability strip (given the high binary fraction of stars in this region of the HR Diagram). Using TESS data, we show that the A0Vnne star HD 42477 has a single p mode coupled to several r modes and/or g modes. We rule out a contaminating background star with a pixel-by-pixel examination, and we essentially rule out the possibility of a companion δ Sct star in a binary. We model the pulsations in HD 42477, and suggest that the g modes are excited by overstable convective core modes. We also conjecture that the single p mode is driven by coupling with the g modes, or that the oblateness of this rapidly-rotating star permits driving by He ii ionization in the equatorial region.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stad858</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0002-6605-0268</orcidid><orcidid>https://orcid.org/0000-0002-1015-3268</orcidid><orcidid>https://orcid.org/0000-0002-2919-6786</orcidid></addata></record> |
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title | HD 42477: coupled r modes, g modes, and a p mode in an A0Vnne star |
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