No period change in two long-period AM CVn binaries
文献类型：期刊论文
| 作者 | Green, Matthew J1,2; Marsh, Thomas R3; Roestel, Jan van4,5; Wong, Tin Long Sunny6; Belloni Diogo7; Kilic, Mukremin1; Breedt, Elmé8; Brown, Alex9; Copperwheat, Chris M10; Chakpor, Anurak11 |
| 刊名 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
 |
| 出版日期 | 2026-05 |
| 卷号 | 548期号:3 |
| 关键词 | binaries: close stars: dwarf novae novae, cataclysmic variables white dwarfs |
| ISSN号 | 0035-8711 |
| DOI | 10.1093/mnras/stag673 |
| 产权排序 | 第7完成单位 |
| 文献子类 | Article |
| 英文摘要 | Ultracompact binary systems, consisting of two compact objects in an orbit less than or similar to 0.5R(circle dot), should exhibit measurable rates of orbital period change (P-center dot not equal 0) due to the emission of gravitational waves (GWs). Measurements of P-center dot have so far been limited to the shortest-period ultracompact binaries ( less than or similar to 20 min). Among the AM CVn-type subclass, several works have proposed the presence of extra angular momentum loss beyond GW emission, with magnetic braking being a widely discussed mechanism. If present, this magnetic braking would dominate the angular momentum loss of AM CVn-type binaries with orbital periods less than or similar to 30 min. In this work, we present a long-term eclipse timing study of two AM CVn-type binaries, YZ LMi and Gaia14aae, with respective orbital periods of 28.3 min and 49.7 min and continuous observations since 2006 and 2015. Both systems show P-center dot consistent with zero within 2 Q. Their 3cr upper limits are 1 . 1 & times; 10(-13) s s(-1) and 9 . 7 & times; 10(-14) s s(-1), respectively. These non-detections are most simply explained by a scenario in which secular angular momentum loss is not substantially stronger than GW emission at all orbital periods, but is combined with deviations from the secular P-center dot whose time-scales span decades but whose amplitude is < 10(-13) s s(-1). Our non-detections of P-center dot represent a limit on the strength of any enhanced angular momentum loss beyond pure GW emission. |
| 学科主题 | 天文学 ; 恒星与银河系 |
| URL标识 | 查看原文 |
| 出版地 | GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND |
| WOS关键词 | MINUTE ORBITAL PERIOD ; ECLIPSING DWARF NOVA ; MASS-TRANSFER ; CATACLYSMIC VARIABLES ; STELLAR EVOLUTION ; GALACTIC BINARIES ; WHITE ; SYSTEMS ; DECAY ; STAR |
| 资助项目 | United States National Science Foundation (NSF)[AST-2508429]; European Research Council under the European Union's Horizon 2020 research and innovation programme[101002408-MOS100PC]; United States National Aeronautics and Space Administration (NASA)[80NSSC24K0436]; United States National Aeronautics and Space Administration (NASA)[80NSSC22K0479]; United States National Aeronautics and Space Administration (NASA)[80NSSC24K0380]; Science and Technology Facilities Council[ST/Z000033/1]; Royal Society[URF\R1\231496]; United Kingdom Research and Innovation[ST/W001934/1]; United Kingdom Research and Innovation[ST/X005933/1] |
| WOS研究方向 | Astronomy & Astrophysics |
| 语种 | 英语 |
| WOS记录号 | WOS:001754360400001 |
| 出版者 | OXFORD UNIV PRESS |
| 资助机构 | United States National Science Foundation (NSF)[AST-2508429] ; European Research Council under the European Union's Horizon 2020 research and innovation programme[101002408-MOS100PC] ; United States National Aeronautics and Space Administration (NASA)[80NSSC24K0436, 80NSSC22K0479, 80NSSC24K0380] ; Science and Technology Facilities Council[ST/Z000033/1] ; Royal Society[URF\R1\231496] ; United Kingdom Research and Innovation[ST/W001934/1, ST/X005933/1] |
| 版本 | 出版稿 |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/29202]  |
| 专题 | 云南天文台_大样本恒星演化研究组 |
| 通讯作者 | Green, Matthew J |
| 作者单位 | 1.Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks Street, Norman, OK 73019, USA; 2.JILA, University of Colorado and National Institute of Standards and Technology, 440 UCB, Boulder, CO 80309-0440, USA; 3.Astronomy and Astrophysics Group, Department of Physics, University of Warwick, Coventry CV4 7AL, UK; 4.Institute of Science and Technology Austria, Am Campus 1, Klosterneuburg A-3400, Austria; 5.Anton Pannekoek Institute for Astronomy, University of Amsterdam, NL-1090 GE Amsterdam, the Netherlands; 6.The Observatories of the Carnegie Institution for Science, Pasadena, CA 91101, USA; 7.International Centre of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research, Yunnan Observatories, CAS, Kunming 650216, China; 8.Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK; 9.Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany; 10.Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK; |
| 推荐引用方式 GB/T 7714 | Green, Matthew J,Marsh, Thomas R,Roestel, Jan van,et al. No period change in two long-period AM CVn binaries[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2026,548(3). |
| APA | Green, Matthew J.,Marsh, Thomas R.,Roestel, Jan van.,Wong, Tin Long Sunny.,Belloni Diogo.,...&Yates, Amalie.(2026).No period change in two long-period AM CVn binaries.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,548(3). |
| MLA | Green, Matthew J,et al."No period change in two long-period AM CVn binaries".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 548.3(2026). |
入库方式： OAI收割
来源：云南天文台
浏览0
下载0
收藏0
其他版本
除非特别说明，本系统中所有内容都受版权保护，并保留所有权利。