Richard J. Rudy, Ray W. Russell, Michael L. Sitko, David K. Lynch, Charles E. Woodward
{"title":"The Coronal Lines of the High-excitation, Fe ii-type Nova V2467 Cygni","authors":"Richard J. Rudy, Ray W. Russell, Michael L. Sitko, David K. Lynch, Charles E. Woodward","doi":"10.3847/2515-5172/ad6e78","DOIUrl":null,"url":null,"abstract":"Optical and infrared spectra are presented for the nova V2467 Cygni from the period of its maximum excitation. The spectra indicate exceptionally high excitation for a Fe <sc>ii</sc>-type nova, exhibiting [Si <sc>x</sc>] 1.4305 <italic toggle=\"yes\">μ</italic>m and several emission lines that we associate with C <sc>vi</sc>. Along with numerous coronal features, V2467 Cygni also displayed low-excitation nebular lines. A CLOUDY analysis indicates a temperature of 5.5 × 10<sup>5</sup> for its exciting source, a very heterogeneous emission line region, and an ejected mass ≥1.5 × 10<sup>−4</sup> <italic toggle=\"yes\">L</italic>\n<sub>☉</sub>.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"14 1","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-08-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Research notes of the AAS","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/2515-5172/ad6e78","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
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Abstract
Optical and infrared spectra are presented for the nova V2467 Cygni from the period of its maximum excitation. The spectra indicate exceptionally high excitation for a Fe ii-type nova, exhibiting [Si x] 1.4305 μm and several emission lines that we associate with C vi. Along with numerous coronal features, V2467 Cygni also displayed low-excitation nebular lines. A CLOUDY analysis indicates a temperature of 5.5 × 105 for its exciting source, a very heterogeneous emission line region, and an ejected mass ≥1.5 × 10−4L☉.
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