本文選題：晚型恒星　切入點：密近雙星　出處：《中國科學院大學(中國科學院云南天文臺)》2017年博士論文　論文類型：學位論文

【摘要】：晚型恒星中普遍存在著類太陽磁場活動現(xiàn)象,預示著在這些晚型恒星較深的對流區(qū)內(nèi)存在與太陽類似的磁場發(fā)電機行為。我們選擇了三顆活動性較強的晚型恒星作為觀測研究對象,一方面通過對V711 Tau和UX Ari的長期高色散分光監(jiān)測,研究它們的磁場活動規(guī)模、色球活動區(qū)的結(jié)構(gòu)和遷移規(guī)律;另一方面通過對SZ Psc的密集采樣觀測,探測和研究它的冕層星珥活動事件。V711 Tau是一個周期約為2.84天的RS CVn型雙譜分光雙星系統(tǒng),它是由一顆K1型亞巨星和一顆G5型主序星組成的。我們分析了從1998年到2004年期間使用國家天文臺興隆觀測基地2.16米光學望遠鏡及其附屬的折軸階梯光柵光譜儀獲得的V711 Tau八個時段的高色散分光觀測數(shù)據(jù)。利用綜合光譜減技術(shù),對光譜覆蓋的形成于色球?qū)硬煌叨鹊幕顒又笜薈aii IRT(λ8498、λ8542和λ8662)、Hα、Nai D1D2和He i D3譜線進行了分析,得到了純色球活動發(fā)射的強度,進一步證實了V711 Tau具有非常強烈的色球活動。系統(tǒng)的色球活動發(fā)射主要是由K1型亞巨星貢獻的,同時G5型子星也具有一定活動性。我們還探測到了V711 Tau的兩次光學耀斑事件。K1型亞巨星的色球活動發(fā)射強度隨位相的變化表現(xiàn)出明顯的自轉(zhuǎn)調(diào)制現(xiàn)象,說明在其表面存在色球活動經(jīng)度帶。除了2004年2月的觀測外,其色球活動主要是由間隔180度的兩個活動經(jīng)度帶主導。V711Tau的色球活動強度還具有長期的活動變化特征。通過和相近時段的測光光變曲線相比較,我們發(fā)現(xiàn)V711 Tau色球活動區(qū)和光球?qū)雍谧踊顒訁^(qū)在空間結(jié)構(gòu)上是相互連接的。UX Ari是由一顆K0型亞巨星和一顆G5型主序星組成的RS CVn型雙星系統(tǒng),周期約為6.44天。為了探測UX Ari的光學耀斑事件和對其色球活動進行研究,我們分析了從2001年到2004年期間使用2.16米光學望遠鏡獲得的UX Ari五個時段的高色散分光觀測數(shù)據(jù)。利用綜合光譜減技術(shù)對色球活動指標Caii IRT(λ8498、λ8542和λ8662)、Hα、Na i D1D2和He i D3譜線進行了分析,研究結(jié)果進一步證實了UX Ari的色球活動是非常劇烈的,并且色球活動發(fā)射主要來自于系統(tǒng)的K0型亞巨星。在觀測中,我們探測到了UX Ari的四次光學耀斑事件。當光學耀斑發(fā)生的時候,耀斑活動的指示計Hei D3譜線是發(fā)射的,同時Hα和Caii IRT譜線也具有很強的發(fā)射,Na i D1D2譜線具有較強的填充發(fā)射或者在其線心存在明顯的反轉(zhuǎn)發(fā)射特征。通過對光學耀斑釋放能量的估算,我們發(fā)現(xiàn)這四次光學耀斑事件是非常劇烈的,尤其是2002年12月16日發(fā)生的這次耀斑事件。此外,除了2004年11月探測到的光學耀斑事件外,UX Ari的光學耀斑多發(fā)生在系統(tǒng)兩顆子星分得比較開的位相上(即0.25位相和0.75位相附近)。UX Ari色球活動強度還表現(xiàn)出明顯的自轉(zhuǎn)調(diào)制,以及長期變化特征。SZ Psc是一個三合星系統(tǒng),其兩顆主要的子星K1型亞巨星和F8型主序星構(gòu)成一個周期約為3.97天的RS CVn型雙星系統(tǒng)。為了探測SZ Psc的恒星星珥活動事件,我們于2011年10月24日和25日利用云南天文臺麗江觀測站2.4米光學望遠鏡及其附屬的麗江系外行星探測器(LiJET)在其普通光譜模式(DEM)下對它進行了時序的高色散分光觀測。利用綜合光譜減技術(shù),我們對色球活動指標Caiiλ8498、λ8542、Hα、Nai D1D2、Hei D3、Mg i b triplet和Hβ譜線進行了分析。在兩個晚上的觀測中,色球活動指標表現(xiàn)出完全不同的活動特征。在第一個晚上的觀測中,Hei D3譜線是吸收的,同時在Hα、Hβ以及其他色球活動指標的剩余光譜中有額外的吸收特征存在;吸收特征相對于系統(tǒng)K1型亞巨星的逐漸藍移和強度的逐漸增強,表明我們探測到了高度逐漸增加的恒星星珥活動事件;另外,該恒星星珥是和第二個晚上的耀斑事件有聯(lián)系的活動星珥。在第二個晚上的觀測中,Hei D3譜線是發(fā)射的,并且其他色球活動指標也具有很強的發(fā)射,表明SZ Psc發(fā)生了劇烈的光學耀斑事件;由于時間窗口限制,我們沒有觀測到完整的耀斑過程,只是觀測到了其緩變相的一部分;伴隨著光學耀斑的逐漸衰減,在色球活動指標(尤其是Hα)譜線輪廓的藍翼上出現(xiàn)了耀斑后環(huán)造成的吸收特征。因此,我們探測到SZ Psc在短時間內(nèi)發(fā)生了一系列的磁場活動現(xiàn)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.

【學位授予單位】：中國科學院大學(中國科學院云南天文臺)
【學位級別】：博士
【學位授予年份】：2017
【分類號】：P144.7

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相關期刊論文 前3條

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本文編號：1591478