铀宝石的新光谱

IF 1.1 4区物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS

Revista Mexicana de Astronomia y Astrofisica Pub Date : 2023-10-01 DOI:10.22201/ia.01851101p.2023.59.02.04

J. Echevarría, S. H. Ramírez, M. Fuentes, L. J. Sánchez, V. Patiño, V. Chavushyan

{"title":"铀宝石的新光谱","authors":"J. Echevarría, S. H. Ramírez, M. Fuentes, L. J. Sánchez, V. Patiño, V. Chavushyan","doi":"10.22201/ia.01851101p.2023.59.02.04","DOIUrl":null,"url":null,"abstract":"We present new optical spectroscopic observations of U Geminorum obtained during a quiescent stage. We perform a radial velocity analysis of three Balmer emission lines yielding inconsistent results. Assuming that the radial velocity semi amplitude accurately reflects the motion of the white dwarf, we arrive at masses for the primary which are in the range of Mwd = 1.21−1.37M☉. Based on the internal radial velocity inconsistencies and results produced from the Doppler tomography - wherein we do not detect emission from the hot spot, but rather an intense asymmetric emission overlaying the disc, reminiscent of spiral arms - we discuss the possibility that the overestimation of the masses may be due to variations of gas opacities and a partial truncation of the disc.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":null,"pages":null},"PeriodicalIF":1.1000,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"NEW SPECTROSCOPY OF U GEM\",\"authors\":\"J. Echevarría, S. H. Ramírez, M. Fuentes, L. J. Sánchez, V. Patiño, V. Chavushyan\",\"doi\":\"10.22201/ia.01851101p.2023.59.02.04\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We present new optical spectroscopic observations of U Geminorum obtained during a quiescent stage. We perform a radial velocity analysis of three Balmer emission lines yielding inconsistent results. Assuming that the radial velocity semi amplitude accurately reflects the motion of the white dwarf, we arrive at masses for the primary which are in the range of Mwd = 1.21−1.37M☉. Based on the internal radial velocity inconsistencies and results produced from the Doppler tomography - wherein we do not detect emission from the hot spot, but rather an intense asymmetric emission overlaying the disc, reminiscent of spiral arms - we discuss the possibility that the overestimation of the masses may be due to variations of gas opacities and a partial truncation of the disc.\",\"PeriodicalId\":49602,\"journal\":{\"name\":\"Revista Mexicana de Astronomia y Astrofisica\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":1.1000,\"publicationDate\":\"2023-10-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Revista Mexicana de Astronomia y Astrofisica\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.22201/ia.01851101p.2023.59.02.04\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q3\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Revista Mexicana de Astronomia y Astrofisica","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.22201/ia.01851101p.2023.59.02.04","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}

引用次数: 0

摘要

我们提出了在静止阶段获得的新的双子星光谱观测。我们执行径向速度分析三个巴尔默发射线产生不一致的结果。假设径向速度半振幅准确地反映了白矮星的运动，我们得到的主恒星的质量范围是Mwd = 1.21−1.37M☉。基于内部径向速度的不一致和多普勒断层扫描产生的结果-其中我们没有检测到热点的发射，而是强烈的不对称发射覆盖在圆盘上，让人想起螺旋臂-我们讨论了质量高估的可能性，可能是由于气体不透明度的变化和圆盘的部分截断。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

查看原文本刊更多论文

NEW SPECTROSCOPY OF U GEM

We present new optical spectroscopic observations of U Geminorum obtained during a quiescent stage. We perform a radial velocity analysis of three Balmer emission lines yielding inconsistent results. Assuming that the radial velocity semi amplitude accurately reflects the motion of the white dwarf, we arrive at masses for the primary which are in the range of Mwd = 1.21−1.37M☉. Based on the internal radial velocity inconsistencies and results produced from the Doppler tomography - wherein we do not detect emission from the hot spot, but rather an intense asymmetric emission overlaying the disc, reminiscent of spiral arms - we discuss the possibility that the overestimation of the masses may be due to variations of gas opacities and a partial truncation of the disc.

求助全文

通过发布文献求助，成功后即可免费获取论文全文。去求助

来源期刊

Revista Mexicana de Astronomia y Astrofisica 地学天文-天文与天体物理

CiteScore

1.30

自引率

10.00%

发文量

审稿时长

>12 weeks

期刊介绍： The Revista Mexicana de Astronomía y Astrofísica, founded in 1974, publishes original research papers in all branches of astronomy, astrophysics and closely related fields. Two numbers per year are issued and are distributed free of charge to all institutions engaged in the fields covered by the RMxAA.