晚型恒星磁活动与恒星自转相关性研究
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摘要
我们在第一章中系统地总结了前人对晚型恒星的磁活动与恒星自转向的相关性研究方面的成果，在第二章中对两种不同的发电机理论进行了简要的叙述和分析，同时在第三章中从理论和观测方面简要地描述了晚型恒星的角动量演化方面的研究。由于前人采用的恒星样本、磁活动和自转参量的不同，以及观测资料的限制，晚型恒星的磁活动与恒星自转间的关系在很大程度上是不确定的。因此，我们收集了晚型恒星的色球和冕球活动的指数以及恒星自转方面研究发表的大量的观测资料并结合Hipparcos卫星的观测结果，对晚型恒星的磁活动与恒星自转间的相关性进行细致的研究。在第四章我们给出了晚型恒星的磁活动指数和自转参量的计算及样本的总体信息。
在第五章中，我们采用不同的磁活动指数研究了晚型恒星磁活动与恒星自转参量(自转周期、Rossby数)、磁活动与恒星色指数以及恒星磁活动指数之间的相关性。大样本分析显示晚型主序恒星的色球活动与恒星自转参量的研究晚型主序恒星的色球活动与恒星自转参量间的关系表现出对恒星光谱型的依赖。对于A—早F型主序恒星的色球活动水平也随自转周期呈线性下降趋势，随Rossby数却呈上升趋势。A—早F型主序恒星的自转周期和恒星对流区的随色指数的分布明显地影响着这些恒星的色球活动行为。而M型主序星的色球活动水平基本上随自转参量的增大呈上升趋势，并且M型主序星的色球活动水平在色指数较大时趋于饱和。从M型主序星的自转周期的和恒星内部对流区随色指数的分布来看，M型主序星的色球活动行为与αΩ发电机理论的预期有明显的差异。从主序星的角动量与以色球活动指数为指标的磁动量间的相关性分析表明α~2Ω发电机可能是M型主序星磁场产生的主要机制。对于介于早F型和M型之间的主序星，色球活动的水平基本上随恒星自转参量的增大而下降。通过主序星的色球活动对恒星色指数不同依赖关系的研究，我们分析了Vaughan—Preston间隙产生的原因，分析结果显示恒星的年龄在这一间隙的形成中扮演了重要的角色。演化恒星的色球活动与恒星自转周期间存在很好的相关性。但是细致分析显示演化恒星色球活动水平随恒星自转周期间的分布对恒星光谱型和恒星表面有效温度有很强的依赖，并对这些现象提出了几种可能的解释。
晚型主序星的冕球活动也表现出对恒星光谱型的依赖性。分析结果显示F型主序星的冕球活动在光谱型F5附近存在拐点。这一拐点的出现可能是F型主序星的对流区的变化影响形成的，也可能是F型主序星在F5附近存在较差自转的上限形成的。对不同光谱型的主序星的统计研究显示G、K、M型主序星的冕球活动基本上随色指数的增大而下降。但是M型主序星的冕球活动是随色指数的增大而下降，这与M型主序星色球活动的行为相反。这种现象可能是由于主序星的色球与冕球间存在的能量平衡和转移以及加热机制不同产生的。此外，统计结果也显示，M型主序星中强冕球活动的样本占总的M型主序星样本比率明显地高于G、K型主序星。主序星的角动量与以冕球活动指数为指标的磁动量间的相关性分析表明M型主序星的角动量与磁动量间的关系偏离了其它类型的主序星的总体线性关系。与主序星色球活动的研究相比，尽管数据点的弥散使这种偏离不是十分的明显，仍然能够对主序星色球研究中的结论提供了一定程度的支持。由于样本的不完备对演化恒星冕球活动与恒星自转间的分析，没有
新男
得到二者间十分可靠的相关性。演化恒星的磁冕球活动在色指数和自转周期的
分布上都显示出冕球磁活动存在上限的现象，并且对冕球磁活动上限的拟合表
明在色指数B一V为1.0附近和自转周期!og尸为1.75附近出现拐点。这些拐点
的出现可能是演化恒星的色球、冕球的能量平衡和加热机制引起的。
我们通过对大样本恒星的统计分析分别得到了晚型主序星磁活动与恒星自
转参量间以及磁活动与恒星色指数之间更广泛意义的数值关系。
在第六章中，我们对晚型主序星和演化恒星的色球、冕球磁活动指数的相
关性进行分析。我们发现主序星的色球与冕球磁活动指数存在着很好的线性相
关性，而演化恒星的则表现出较弱的相关性。晚型主序星和演化恒星色球与冕
球磁活动指数相关性差异进一步支持了对演化恒星的冕球磁活动研究中得到的
结论，即演化恒星的冕球活动与色球活动行为的差异是恒星色球、冕球的能量
平衡和加热机制不同产生的。M型主序星在演化恒星的冕球活动与色球活动行
为的差异则是由于M型主序星的色球与冕球间存在的能量平衡和转移过程产生
的。
在第七章中，我们讨论了晚型恒星的自转周期的分布、恒星年龄对晚型恒
星磁活动的影响以及晚型恒星的角动量演化。晚型主序恒星的自转周期、磁活
动与恒星年龄之间存在很好的线性相关性。而晚型演化恒星不论是演化恒星的
磁活动还是自转周期以恒星年龄10”年为分界点表现出随年龄不同的规律。这
种现象在很大程度上反映了不同质量的恒星的不同的演化历程和演化状态。对
晚型恒星角动量演化的分析显示晚型恒星的角动量演化基本上是守恒演化。但
处于演化晚期的巨星和超巨星，由于星风的增大，恒星角动量的演化会不守恒。
We have collected a mass of stellar activity and rotation data of late-type stars. Combining with the results of Hipparcos satellite, we reserch the relation between stellar activity and rotation(include rotation period and Rossby number), and discuss the distribution of stellar rotation period and the evolution of angle momentum of late-type stars. Furthermore, we also reserch the influence of setllar age to stellar activity of late-type stars.
The relation of stellar chromospheric activity and rotation of late-type main sequence stars depend on stellar spectral type. For A-early F type MS stars, stellar chromospheric activity decrease with stellar rotation period, but increase with Rossby number; For M type MS stars, stellar chromospheric activity increase with stellar rotation period and Rossby number, and stellar chromospheric activity reach saturation at large color index; For the MS stars between mid-F to M type, stellar chromospheric activity decrease with stellar rotation period and Rossby number. From the distribution of rotation period and convection parameter of M type stars, stellar chromospheric activity of M type stars depart from the anticipation of a. dynamo theory obviously. According to the analysis of the relation of between angle momentum and magnetic
momentum, we find that a2 dynamo is main mechanism for the stars with
deep interior convection zone similarly late-M type stars. By the reserching the relation between stellar chromospheric activity and color index, we find that stellar ages play a pivotal role for producing Vaughan-Preston gap of MS stars. The relation between stellar chromospheric activity and rotation of evolution stars have a good relativity. But meticulous analysis show chromospheric activity of evolution stars depend on stellar spectral type and effective temperature strongly. We provide several possible explain for those phenomena.
The corona activity of late-type main sequence stars also depend on the stellar spectral type. The corona activity of late-type MS stars exist a inflexion nearby F5. There have two fold reason. One reason is the change of interior convection zone with spectral type produce the phenomena; Another reason is the differential rotation of F type stars exist a upper limit. The corona activity of G, K, M type stars decrease with color index increasing as a whole. The result of statistics show the ratio of strong activity samples in M type MS stars is larger than that in other G, K type MS stars, the relation of between angle momentum and magnetic momentum of M type stars also depart from the whole relation of MS stars. Though this departure is not obvious, the result still support the conclusion in the analysis of stellar chromospheric activity. For evolution stars,
wo don't, obtain significative result because the deficient samples. But the statistics analysis show the distrbution of corona activity of late type with color index and rotation period exist upper limit. And those
limit have inflexion nearby B-V=1.0 and log P=1.75 respectively. Those
inflexion are brought by the energy balance and heating mechanism in stellar chromosphere and corona.
Using large samples, we gain several credible numeric relation between different magnetic activity index and rotational parameters.
Between chromospheric activity index and corona activity index of MS stars, there exist good linear relativity. But for evolution stars, this relation show a large dispersion. This phenomenon farther surport our conclusion in the analysis of evolution stars, i.e. the difference of stellar chromosphere and corona activity of evolution stars is bred by the energy balance and heating mechanism in stellar chromosphere and corona.
There have good linear relativity between stellar magnetic activity, rotational period and stellar age of MS stars, but this relativity of evolution stars has different action. For the evolution stars with age less than 109 years, stellar magnetic activity and rotational period decrease with stellar age; For the stars with age larger
在第五章中，我们采用不同的磁活动指数研究了晚型恒星磁活动与恒星自转参量(自转周期、Rossby数)、磁活动与恒星色指数以及恒星磁活动指数之间的相关性。大样本分析显示晚型主序恒星的色球活动与恒星自转参量的研究晚型主序恒星的色球活动与恒星自转参量间的关系表现出对恒星光谱型的依赖。对于A—早F型主序恒星的色球活动水平也随自转周期呈线性下降趋势，随Rossby数却呈上升趋势。A—早F型主序恒星的自转周期和恒星对流区的随色指数的分布明显地影响着这些恒星的色球活动行为。而M型主序星的色球活动水平基本上随自转参量的增大呈上升趋势，并且M型主序星的色球活动水平在色指数较大时趋于饱和。从M型主序星的自转周期的和恒星内部对流区随色指数的分布来看，M型主序星的色球活动行为与αΩ发电机理论的预期有明显的差异。从主序星的角动量与以色球活动指数为指标的磁动量间的相关性分析表明α~2Ω发电机可能是M型主序星磁场产生的主要机制。对于介于早F型和M型之间的主序星，色球活动的水平基本上随恒星自转参量的增大而下降。通过主序星的色球活动对恒星色指数不同依赖关系的研究，我们分析了Vaughan—Preston间隙产生的原因，分析结果显示恒星的年龄在这一间隙的形成中扮演了重要的角色。演化恒星的色球活动与恒星自转周期间存在很好的相关性。但是细致分析显示演化恒星色球活动水平随恒星自转周期间的分布对恒星光谱型和恒星表面有效温度有很强的依赖，并对这些现象提出了几种可能的解释。
晚型主序星的冕球活动也表现出对恒星光谱型的依赖性。分析结果显示F型主序星的冕球活动在光谱型F5附近存在拐点。这一拐点的出现可能是F型主序星的对流区的变化影响形成的，也可能是F型主序星在F5附近存在较差自转的上限形成的。对不同光谱型的主序星的统计研究显示G、K、M型主序星的冕球活动基本上随色指数的增大而下降。但是M型主序星的冕球活动是随色指数的增大而下降，这与M型主序星色球活动的行为相反。这种现象可能是由于主序星的色球与冕球间存在的能量平衡和转移以及加热机制不同产生的。此外，统计结果也显示，M型主序星中强冕球活动的样本占总的M型主序星样本比率明显地高于G、K型主序星。主序星的角动量与以冕球活动指数为指标的磁动量间的相关性分析表明M型主序星的角动量与磁动量间的关系偏离了其它类型的主序星的总体线性关系。与主序星色球活动的研究相比，尽管数据点的弥散使这种偏离不是十分的明显，仍然能够对主序星色球研究中的结论提供了一定程度的支持。由于样本的不完备对演化恒星冕球活动与恒星自转间的分析，没有
新男
得到二者间十分可靠的相关性。演化恒星的磁冕球活动在色指数和自转周期的
分布上都显示出冕球磁活动存在上限的现象，并且对冕球磁活动上限的拟合表
明在色指数B一V为1.0附近和自转周期!og尸为1.75附近出现拐点。这些拐点
的出现可能是演化恒星的色球、冕球的能量平衡和加热机制引起的。
我们通过对大样本恒星的统计分析分别得到了晚型主序星磁活动与恒星自
转参量间以及磁活动与恒星色指数之间更广泛意义的数值关系。
在第六章中，我们对晚型主序星和演化恒星的色球、冕球磁活动指数的相
关性进行分析。我们发现主序星的色球与冕球磁活动指数存在着很好的线性相
关性，而演化恒星的则表现出较弱的相关性。晚型主序星和演化恒星色球与冕
球磁活动指数相关性差异进一步支持了对演化恒星的冕球磁活动研究中得到的
结论，即演化恒星的冕球活动与色球活动行为的差异是恒星色球、冕球的能量
平衡和加热机制不同产生的。M型主序星在演化恒星的冕球活动与色球活动行
为的差异则是由于M型主序星的色球与冕球间存在的能量平衡和转移过程产生
的。
在第七章中，我们讨论了晚型恒星的自转周期的分布、恒星年龄对晚型恒
星磁活动的影响以及晚型恒星的角动量演化。晚型主序恒星的自转周期、磁活
动与恒星年龄之间存在很好的线性相关性。而晚型演化恒星不论是演化恒星的
磁活动还是自转周期以恒星年龄10”年为分界点表现出随年龄不同的规律。这
种现象在很大程度上反映了不同质量的恒星的不同的演化历程和演化状态。对
晚型恒星角动量演化的分析显示晚型恒星的角动量演化基本上是守恒演化。但
处于演化晚期的巨星和超巨星，由于星风的增大，恒星角动量的演化会不守恒。
We have collected a mass of stellar activity and rotation data of late-type stars. Combining with the results of Hipparcos satellite, we reserch the relation between stellar activity and rotation(include rotation period and Rossby number), and discuss the distribution of stellar rotation period and the evolution of angle momentum of late-type stars. Furthermore, we also reserch the influence of setllar age to stellar activity of late-type stars.
The relation of stellar chromospheric activity and rotation of late-type main sequence stars depend on stellar spectral type. For A-early F type MS stars, stellar chromospheric activity decrease with stellar rotation period, but increase with Rossby number; For M type MS stars, stellar chromospheric activity increase with stellar rotation period and Rossby number, and stellar chromospheric activity reach saturation at large color index; For the MS stars between mid-F to M type, stellar chromospheric activity decrease with stellar rotation period and Rossby number. From the distribution of rotation period and convection parameter of M type stars, stellar chromospheric activity of M type stars depart from the anticipation of a. dynamo theory obviously. According to the analysis of the relation of between angle momentum and magnetic
momentum, we find that a2 dynamo is main mechanism for the stars with
deep interior convection zone similarly late-M type stars. By the reserching the relation between stellar chromospheric activity and color index, we find that stellar ages play a pivotal role for producing Vaughan-Preston gap of MS stars. The relation between stellar chromospheric activity and rotation of evolution stars have a good relativity. But meticulous analysis show chromospheric activity of evolution stars depend on stellar spectral type and effective temperature strongly. We provide several possible explain for those phenomena.
The corona activity of late-type main sequence stars also depend on the stellar spectral type. The corona activity of late-type MS stars exist a inflexion nearby F5. There have two fold reason. One reason is the change of interior convection zone with spectral type produce the phenomena; Another reason is the differential rotation of F type stars exist a upper limit. The corona activity of G, K, M type stars decrease with color index increasing as a whole. The result of statistics show the ratio of strong activity samples in M type MS stars is larger than that in other G, K type MS stars, the relation of between angle momentum and magnetic momentum of M type stars also depart from the whole relation of MS stars. Though this departure is not obvious, the result still support the conclusion in the analysis of stellar chromospheric activity. For evolution stars,
wo don't, obtain significative result because the deficient samples. But the statistics analysis show the distrbution of corona activity of late type with color index and rotation period exist upper limit. And those
limit have inflexion nearby B-V=1.0 and log P=1.75 respectively. Those
inflexion are brought by the energy balance and heating mechanism in stellar chromosphere and corona.
Using large samples, we gain several credible numeric relation between different magnetic activity index and rotational parameters.
Between chromospheric activity index and corona activity index of MS stars, there exist good linear relativity. But for evolution stars, this relation show a large dispersion. This phenomenon farther surport our conclusion in the analysis of evolution stars, i.e. the difference of stellar chromosphere and corona activity of evolution stars is bred by the energy balance and heating mechanism in stellar chromosphere and corona.
There have good linear relativity between stellar magnetic activity, rotational period and stellar age of MS stars, but this relativity of evolution stars has different action. For the evolution stars with age less than 109 years, stellar magnetic activity and rotational period decrease with stellar age; For the stars with age larger
引文
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