Helioseismic Study of Solar Internal Rotation

太阳内自转的日震研究

• 批准号: 08454048
• 负责人: SHIBAHASHI Hiromoto
• 金额: $ 4.48万
• 依托单位: The University of Tokyo
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (B)
• 财政年份: 1996
• 资助国家: 日本
• 起止时间: 1996 至 1997
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-08454048/
• 关键词: Sun : Interior; Stars : Interior; Helioseismology; Sun : Oscillation; Inverse problem; 太陽:内部構造; 恒星:内部構造

Dwarf novae are eruptive variables showing repetitive outbursts of amplitudes of 2-6 magnitude once every a few weeks to months. It is now widelyu accepted that outbursts of dwarf novae may be caused by the instability in accretion disks in cataclysmic variable stars : i.e., the disk instability model which was first proposed by the present author (Osaki, 1974) in 1974. There is a rich variety in outburst behaviors of non-magnetic cataclysmic variable stars, starting from non-outbursting nova-like stars to various sub-classes of dwarf novae (i.e., U Gem-type, Z Cam-type, and SU UMa-type). Furthermore, two extreme cases of SU UMa-type dw arf novaehave recently been recognized : WZ Sge-type and ER UMa-type.A unification model for dwarf nova outbursts is proposed within the basic framework of the disk instability model in which two different intrinsic instabilities (i.e., the thermal instability and the tidal instability) within accretion disks play an essential role. Non-magnetic cataclysmic variables are classified into four regions in orbital-period versus mass-transfer rate diagram in different combination of stability behavior for the two intrinsic instabilities in accretion disks, and their different outburst behaviors are basically understood in this diagram. In particular, outbursts in SU UMa-type dwarf novae are understood by the thermal-tidal instability model in which the coupling of the two intrinsic instabailities in accretion disks plays a unique role. A rich variety of outburst behavior of cataclysmic variables below the period gap (i.e., starting from "parmanent superhumpers", to Z Cam-like SU UMa stars, "ER UMa stars", to ordinary SU UMa stars, finally to WZ Sge stars) is understood by the thermal-tidal instability model.

矮新星是一种爆发性变星，每隔几周到几个月就会重复爆发一次，振幅为2-6级。现在大家普遍认为，矮新星的爆发可能是由激变变星吸积盘的不稳定性引起的：即，本文作者（大崎，1974）于1974年首次提出的盘不稳定性模型。非磁性激变变星的爆发行为有着丰富的多样性，从非爆发的类新星恒星到矮新星的各种子类（即，U Gem-type、Z Cam-type和SU UMa-type）。此外，最近还发现了SU UMa型矮新星的两种极端情况：WZ Sge型和ER UMa型。在盘不稳定性模型的基本框架内，提出了矮新星爆发的统一模型，其中两种不同的内禀不稳定性（即，热不稳定性和潮汐不稳定性）在吸积盘中起着至关重要的作用。在吸积盘中两种内禀不稳定性稳定性行为的不同组合下，非磁性激变变星在轨道周期与质量传递率图中被分为四个区域，它们的不同爆发行为在该图中得到了基本理解。特别是，爆发在SU UMA型矮新星的热潮汐不稳定性模型中，两个内在的不稳定性吸积盘的耦合起着独特的作用。周期间隙以下的激变变量的丰富多样的爆发行为（即，从“paramentalsuperhumpers”开始，到类Z Cam的SU Uma星，“ER Uma星”，到普通SU Uma星，最后到WZ Sge星）。

项目成果

Shibahashi, H., &Takata, M.: "Making a Seismic Solar Model and an Estimate of the Neutrino Fluxes" Sounding Solar and Stellar Interiors,IAU Symp.No.181,eds.J.Provost et al.(Kluwer Academic Publ.,Dordrecht). 167-174 (1997)

芝桥，H.，

Shibahashi, H., & Takata, M.: "Making a Seismic Solar Model and an Estimate of the Neutrino Fluxes" in Sounding Solar and Stellar Interiors, " IAU Symp.No.181, eds.J.Provost et al.(Kluwer Academic Publ., Dordrecht). 167-174 (1997)

芝桥，H.，

Shibahashi, H.: "Theoretical Aspects of the Rapidly Oscillating Ap Stars" in "Highlights of Astronomy, " (Kluwer Academic Publ., Dordrecht). (in press). (1998)

Shibahashi, H.：“天文学亮点”中的“快速振荡 Ap 星的理论方面”（Kluwer 学术出版社，多德雷赫特）。

H.Shibahashi: "Implication of Long-ferm Frequency Variation of Low and Intermediate Degree Modes" Proc.IAU Symp.181,Sounding Solar and Stellar Interiors. (印刷中).

H. Shibahashi：“低度和中度模式的长期频率变化的含义”Proc.IAU Symp.181，探测太阳和恒星内部（正在出版）。

Shibahashi, H., & Takata, M.: "An Estimate of the Solar Fluxes Based on the Hilioseismic Data" Bull.Astron.Soc.India. 24. 301-304 (1996)

芝桥，H.，