晚型恒星外层大气磁场活动的观测研究

发布时间：2018-03-10 03:08

本文选题：晚型恒星　切入点：密近双星　出处：《中国科学院大学(中国科学院云南天文台)》2017年博士论文　论文类型：学位论文

【摘要】：晚型恒星中普遍存在着类太阳磁场活动现象,预示着在这些晚型恒星较深的对流区内存在与太阳类似的磁场发电机行为。我们选择了三颗活动性较强的晚型恒星作为观测研究对象,一方面通过对V711 Tau和UX Ari的长期高色散分光监测,研究它们的磁场活动规模、色球活动区的结构和迁移规律;另一方面通过对SZ Psc的密集采样观测,探测和研究它的冕层星珥活动事件。V711 Tau是一个周期约为2.84天的RS CVn型双谱分光双星系统,它是由一颗K1型亚巨星和一颗G5型主序星组成的。我们分析了从1998年到2004年期间使用国家天文台兴隆观测基地2.16米光学望远镜及其附属的折轴阶梯光栅光谱仪获得的V711 Tau八个时段的高色散分光观测数据。利用综合光谱减技术,对光谱覆盖的形成于色球层不同高度的活动指标Caii IRT(λ8498、λ8542和λ8662)、Hα、Nai D1D2和He i D3谱线进行了分析,得到了纯色球活动发射的强度,进一步证实了V711 Tau具有非常强烈的色球活动。系统的色球活动发射主要是由K1型亚巨星贡献的,同时G5型子星也具有一定活动性。我们还探测到了V711 Tau的两次光学耀斑事件。K1型亚巨星的色球活动发射强度随位相的变化表现出明显的自转调制现象,说明在其表面存在色球活动经度带。除了2004年2月的观测外,其色球活动主要是由间隔180度的两个活动经度带主导。V711Tau的色球活动强度还具有长期的活动变化特征。通过和相近时段的测光光变曲线相比较,我们发现V711 Tau色球活动区和光球层黑子活动区在空间结构上是相互连接的。UX Ari是由一颗K0型亚巨星和一颗G5型主序星组成的RS CVn型双星系统,周期约为6.44天。为了探测UX Ari的光学耀斑事件和对其色球活动进行研究,我们分析了从2001年到2004年期间使用2.16米光学望远镜获得的UX Ari五个时段的高色散分光观测数据。利用综合光谱减技术对色球活动指标Caii IRT(λ8498、λ8542和λ8662)、Hα、Na i D1D2和He i D3谱线进行了分析,研究结果进一步证实了UX Ari的色球活动是非常剧烈的,并且色球活动发射主要来自于系统的K0型亚巨星。在观测中,我们探测到了UX Ari的四次光学耀斑事件。当光学耀斑发生的时候,耀斑活动的指示计Hei D3谱线是发射的,同时Hα和Caii IRT谱线也具有很强的发射,Na i D1D2谱线具有较强的填充发射或者在其线心存在明显的反转发射特征。通过对光学耀斑释放能量的估算,我们发现这四次光学耀斑事件是非常剧烈的,尤其是2002年12月16日发生的这次耀斑事件。此外,除了2004年11月探测到的光学耀斑事件外,UX Ari的光学耀斑多发生在系统两颗子星分得比较开的位相上(即0.25位相和0.75位相附近)。UX Ari色球活动强度还表现出明显的自转调制,以及长期变化特征。SZ Psc是一个三合星系统,其两颗主要的子星K1型亚巨星和F8型主序星构成一个周期约为3.97天的RS CVn型双星系统。为了探测SZ Psc的恒星星珥活动事件,我们于2011年10月24日和25日利用云南天文台丽江观测站2.4米光学望远镜及其附属的丽江系外行星探测器(LiJET)在其普通光谱模式(DEM)下对它进行了时序的高色散分光观测。利用综合光谱减技术,我们对色球活动指标Caiiλ8498、λ8542、Hα、Nai D1D2、Hei D3、Mg i b triplet和Hβ谱线进行了分析。在两个晚上的观测中,色球活动指标表现出完全不同的活动特征。在第一个晚上的观测中,Hei D3谱线是吸收的,同时在Hα、Hβ以及其他色球活动指标的剩余光谱中有额外的吸收特征存在;吸收特征相对于系统K1型亚巨星的逐渐蓝移和强度的逐渐增强,表明我们探测到了高度逐渐增加的恒星星珥活动事件;另外,该恒星星珥是和第二个晚上的耀斑事件有联系的活动星珥。在第二个晚上的观测中,Hei D3谱线是发射的,并且其他色球活动指标也具有很强的发射,表明SZ Psc发生了剧烈的光学耀斑事件;由于时间窗口限制,我们没有观测到完整的耀斑过程,只是观测到了其缓变相的一部分;伴随着光学耀斑的逐渐衰减,在色球活动指标(尤其是Hα)谱线轮廓的蓝翼上出现了耀斑后环造成的吸收特征。因此,我们探测到SZ Psc在短时间内发生了一系列的磁场活动现象。
[Abstract]:Common in late type stars with solar magnetic activity, indicating the presence of magnetic field generator behavior similar to that of the sun in the convection zone of these late type stars deep inside. We chose three activity of late type stars strong as the observation object of study, mainly through the V711 Tau and UX Ari of the long-term high dispersion optical monitoring, study their magnetic activity scale, structure and migration regularity of chromospheric activity area; on the other hand, through the observation of SZ Psc intensive sampling, detection and study of its crown,.V711 Tau layer star event is a period of about 2.84 days of RS type CVn double spectrum binary system and it is composed of a K1 type star and a G5 type stars. We analyzed from 1998 to 2004 by the National Astronomical Observatory of XINLUNG base during the 2.16 meter optical telescope and its subsidiary coude echelle spectrometer was High dispersion of V711 Tau eight time light observation data. By using the spectral subtraction technique, the spectral coverage is formed in the chromosphere activity index Caii IRT of different height (lambda 8498, lambda 8542 and lambda 8662), H Nai D1D2 and He I alpha, D3 spectra were analyzed, obtained solid ball emission intensity, further confirmed that V711 Tau has very strong chromospheric activity. The chromospheric activity emission is mainly contributed by the K1 type and G5 type of star, star also has a certain activity. We also detected a two V711 optical flare events Tau.K1 type subgiant ball the emission intensity with phase change activity showed obvious rotational modulation phenomenon, that exists on the surface of chromospheric activity. In addition to longitude with the February 2004 observations, the chromospheric activity is mainly composed of two active longitude at 180 degrees with.V711Tau leading a live ball The dynamic strength also has the characteristics of long term change activities. By the time of the light and similar light curve comparison, we found that V711 and Tau active chromosphere region photospheric sunspots in the space structure is connected.UX Ari RS CVn is composed of a K0 type star and a G5 type stars binary system, a period of about 6.44 days. In order to detect UX Ari optical flare events and the chromospheric activity research, we analyzed the high dispersion from 2004 to 2001 during the use of 2.16 meter optical telescope obtained UX Ari five time light observation data reduction technique. The chromospheric activity indicators using IRT spectrum Caii (lambda 8498, lambda 8542 and lambda 8662), H Na I and He D1D2 alpha, I D3 spectrum was analyzed, the results further confirmed that the UX Ari of the chromospheric activity is very violent, and chromospheric activity emissions mainly come from the system of K0 Asian superstar. In observation, we detected four UX Ari optical flare events. When the optical flare and flare activity indicator Hei D3 spectral line is emitted, while H alpha and Caii IRT line also has a strong launch, Na I D1D2 spectra of strong filling emission or in the heart line has obvious reverse emission characteristics with. By estimating the release energy of optical flares, we found the four optical flare events is very severe, especially in December 16, 2002 occurred in this event. In addition, in addition to optical flare events detected in November 2004, optical flares occurred in Ari UX the two planet system share on the phase (i.e., near the 0.25 phase and 0.75 phase).UX Ari chromospheric activity also showed obvious modulation intensity of rotation, and the long term variation of.SZ Psc is a three star system, the The two main sub star type K1 sub star and F8 type stars constitute a period of about 3.97 days of RS CVn type binary system. In order to detect SZ Psc stars and events, we in October 24, 2011 and 25, by the Yunnan Observatory 2.4 meter optical telescope and Lijiang Department of foreign subsidiaries Lijiang Observatory starprobe (LiJET) in the normal mode spectra (DEM) of it were high dispersion timing spectroscopic observations. Using the spectral subtraction technique, the chromospheric activity indicators Caii lambda 8498, lambda 8542, H alpha, Nai D1D2, Hei D3, Mg I B triplet and H beta spectra were analyzed. In the observation of two nights, chromospheric activity indicators show the characteristics of completely different. In the observation of the first night, Hei D3 spectrum is absorbed at the same time, H alpha, H beta and residual spectrum of other chromospheric activity indicators in additional absorption characteristics; absorption Compared with the characteristics of gradually increased K1 type subgiant shifted and intensity, that we detected the height increasing of stars and events; in addition, the stars, and there is a relationship between the night of the second flare events. In second, the star observation at night, Hei D3 spectrum the line is launched, and the other chromospheric activity indicators also has strong emission, indicating the occurrence of intense optical flare events SZ Psc; because of the time window constraints, we have not observed the flare process complete, only observed the slow part in disguise; accompanied by a gradual attenuation of optical flares in the chromospheric activity the index (especially H alpha) appeared flare line profiles on the posterior ring of blue wing caused by absorption characteristics. Therefore, we detected SZ Psc has undergone a series of phenomena of magnetic activity in a short period of time.

【学位授予单位】：中国科学院大学(中国科学院云南天文台)
【学位级别】：博士
【学位授予年份】：2017
【分类号】：P144.7

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