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<article xsi:noNamespaceSchemaLocation="http://jats.nlm.nih.gov/publishing/1.1/xsd/JATS-journalpublishing1-mathml3.xsd" dtd-version="1.1" xmlns:xlink="http://www.w3.org/1999/xlink" xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance"><front><journal-meta><journal-id journal-id-type="publisher-id">SSSD</journal-id><journal-title-group><journal-title>Scientific and Social Sustainable Development</journal-title></journal-title-group><issn>3066-8964</issn><eissn>3066-8980</eissn><publisher><publisher-name>Art and Technology</publisher-name></publisher></journal-meta><article-meta><article-id pub-id-type="doi">10.61369/SSSD.2026050044</article-id><article-categories><subj-group subj-group-type="heading"><subject>Article</subject></subj-group></article-categories><title>双星的形成与演化</title><url>https://artdesignp.com/journal/SSSD/2/5/10.61369/SSSD.2026050044</url><author>钟萃相</author><pub-date pub-type="publication-year"><year>2026</year></pub-date><volume>2</volume><issue>5</issue><history><date date-type="pub"><published-time>2026-03-14</published-time></date></history><abstract>双星的形成与演化是恒星形成与演化的关键步骤，因此其研究成为了现代天文学研究的核心内容。尽管早在1976年玻丹&amp;middot;帕琴斯基提出了双星共有包层演化理论, 但一直没有得到确认，直到2022年中国科学院云南天文台与澳大利亚团队首次观测到了双星共有包层抛射现象，为玻丹. 帕琴斯基的理论提供了支持，但对于双星的真正形成机制与演化过程尚未确定。为此本文作者根据双星共有包层演化理论和潮汐瓦解理论提出了双星的形成与演化理论，为确立完整的恒星形成与演化理论奠定了基础。</abstract><keywords>双星共有包层演化理论,双星共有包层抛射现象,潮汐瓦解,双星的形成与演化</keywords></article-meta></front><body/><back><ref-list><ref id="B1" content-type="article"><label>1</label><element-citation publication-type="journal"><p>[1]Han Zhanwen. Binary Population Synthesis[J]. Research in Astronomy and Astrophsics,2020, 20(10):161.[2]Jia-jia Li,Jian-ping Xiong, Zhi-jia Tian, Chao-Liu, Zhanwen Han, Xue-fei Chen. Identify Main-sequence Binaries from the Chinese Space Station Telescope Survey withMachine Learning. II. Based on Gaia and GALEX [J]. The Astronomical Journal (2025).[3]Li Zhenwei, Chen Xuefei,Ge Hongwei, Chen Hai-liang and Han Zhanwen. Influence of a mass transfer stability criterion on double white dwarf populations [J]. A&amp;amp;A 669, A(82) (2023).[4]Jarrod R. Hurley, Christopher A. Tout and Onner R. Pols. Evolution of Binary Stars and the Effect of Tides on Binary Populations [J]. Mon. Not. R. Astron. Soc. 000,1,36(2000).[5]Pollack J B, et al. Formation of the giant planets by concurrent accretion of solids and gas[J]. Icarus,1996,124:62-85.[6]Laughlin, G.; Bodenheimer, P.; Adams, F. C. The End of the Main Sequence [J]. The Astrophysical Journal,1997, 482: 420.[7]Dixon D, Tayar J, Stassun K G. Rotationally Driven Ultraviolet Emission of Red Giant Stars[J]. The Astronomical Journal, 2020, 160(1):12.[8]Sollerman J, et al. Late-time observations of the extraordinary Type II supernova iPTF14hls [J]. Astronomy and Astrophysics, 2019, 621.[9]T Tauris. Neutron Star Formation and Evolution - Singles, Binaries and Triples [C]. 40th COSPAR Scientific Assembly, held 2-10 August 2014, in Moscow, Russia.[10]MG Haehnelt,G Kauffmann. The Formation and Evolution of Supermassive Black Holes and their Host Galaxies. Springer Berlin Heidelberg , 2001:364-374.[11]Wu, XB, et al. An ultra luminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30 [J]. Nature, 2015,518(7540): 512-515.[12]Cuixiang Zhong.The Formation and Evolution Law of Stars and Quasars[J]. Journal of Physical Science and Application 15 (1) (2025) 1-15.</p><pub-id pub-id-type="doi"/></element-citation></ref></ref-list></back></article>
