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Dynamical Masses of the Primary Be Star and Secondary sdB Star in the Single-lined Binary kappa Dra (B6 IIIe)
Klement, Robert1; Baade, Dietrich2; Rivinius, Thomas3; Gies, Douglas R.4; Wang LQ(王璐茜)4,5; Labadie-Bartz, Jonathan6; Santos, Pedro Ticiani dos7; Monnier, John D.8; Carciofi, Alex C.7; Mérand, Antoine2; Anugu, Narsireddy1; Schaefer, Gail H.1; Bouquin, Jean-Baptiste Le9; Davies, Claire L.10; Ennis, Jacob8; Gardner, Tyler8; Kraus, Stefan11; Setterholm, Benjamin R.8; Labdon, Aaron3
发表期刊ASTROPHYSICAL JOURNAL
2022-11-01
卷号940期号:1
DOI10.3847/1538-4357/ac98b8
产权排序第5完成单位
收录类别SCI
摘要

Because many classical Be stars may owe their nature to mass and angular-momentum transfer in a close binary, the present masses, temperatures, and radii of their components are of high interest for comparison to stellar evolution models. Object kappa Dra is a 61.5 day single-lined binary with a B6 IIIe primary. With the CHARA Array instruments MIRC/MIRC-X and MYSTIC, we detected the secondary at (approximately photospheric) flux ratios of 1.49% +/- 0.10% and 1.63% +/- 0.09% in the H and K band, respectively. From a large and diverse optical spectroscopic database, only the radial velocity curve of the Be star could be extracted. However, employing the parallaxes from Hipparcos and Gaia, which agree within their nominal 1 sigma errors, we could derive the total mass and found component masses of 3.65 +/- 0.48 and 0.426 +/- 0.043 M (circle dot) for the Be star and the companion, respectively. Previous cross-correlation of the observed FUV spectrum with O-type subdwarf (sdO) spectral model templates had not detected a companion belonging to the hot sdO population known from similar to 20 earlier-type Be stars. Guided by our full 3D orbital solution, we found a strong cross-correlation signal for a stripped subdwarf B-type companion (FUV flux ratio of 2.3% +/- 0.5%), enabling the first firm characterization of such a star and making kappa Dra the first mid- to late-type Be star with a directly observed subdwarf companion.

资助项目National Science Foundation[AST-1636624] ; National Science Foundation[AST-2034336] ; National Science Foundation[AST-1908026] ; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program[639889] ; Provost's Office of Georgia State University ; CNPq[311446/2019-1] ; FAPESP[2018/04055-8] ; FAPESP[2019/13354-1] ; ERC Consolidator Grant[101003096] ; STFC Consolidated Grant[ST/V000721/1] ; NASA-XRP[NNX16AD43G] ; NSF-AST[1909165] ; NSF-ATI[1506540] ; CAPES[88887.604774/2021-00]
项目资助者National Science Foundation[AST-1636624, AST-2034336, AST-1908026] ; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program[639889] ; Provost's Office of Georgia State University ; CNPq[311446/2019-1] ; FAPESP[2018/04055-8, 2019/13354-1] ; ERC Consolidator Grant[101003096] ; STFC Consolidated Grant[ST/V000721/1] ; NASA-XRP[NNX16AD43G] ; NSF-AST[1909165] ; NSF-ATI[1506540] ; CAPES[88887.604774/2021-00]
语种英语
学科领域天文学 ; 恒星与银河系
学科门类理学 ; 理学::天文学
文章类型Article
出版者IOP Publishing Ltd
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS记录号WOS:000889847500001
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]EVOLUTIONARY STATUS ; GALACTIC PLANE ; VARIABILITY ; KINEMATICS ; HIPPARCOS ; OB ; SPECTROGRAPH ; PARALLAXES ; VALIDATION ; EMISSION
引用统计
被引频次:7[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
版本出版稿
条目标识符http://ir.ynao.ac.cn/handle/114a53/25671
专题大样本恒星演化研究组
通讯作者Klement, Robert
作者单位1.The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, CA 91023, USA; robertklement@gmail.com;
2.European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany;
3.European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Casilla 19001, Santiago 19, Chile;
4.Center for High Angular Resolution Astronomy, Department of Physics and Astronomy, Georgia State University, P.O. Box 5060, Atlanta, GA 30302-5060, USA;
5.Yunnan Observatories, CAS, P.O. Box 110, Kunming 650011, Yunnan, People's Republic of China;
6.Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA;
7.Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900 São Paulo, SP, Brazil;
8.Department of Astronomy, University of Michigan, 1085 S. University Ave., Ann Arbor, MI 48109, USA;
9.Université Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France;
10.Astrophysics Group, Department of Physics & Astronomy, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK;
11.Astrophysics Group, School of Physics and Astronomy, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK
推荐引用方式
GB/T 7714
Klement, Robert,Baade, Dietrich,Rivinius, Thomas,et al. Dynamical Masses of the Primary Be Star and Secondary sdB Star in the Single-lined Binary kappa Dra (B6 IIIe)[J]. ASTROPHYSICAL JOURNAL,2022,940(1).
APA Klement, Robert.,Baade, Dietrich.,Rivinius, Thomas.,Gies, Douglas R..,Wang LQ.,...&Labdon, Aaron.(2022).Dynamical Masses of the Primary Be Star and Secondary sdB Star in the Single-lined Binary kappa Dra (B6 IIIe).ASTROPHYSICAL JOURNAL,940(1).
MLA Klement, Robert,et al."Dynamical Masses of the Primary Be Star and Secondary sdB Star in the Single-lined Binary kappa Dra (B6 IIIe)".ASTROPHYSICAL JOURNAL 940.1(2022).
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