六个色球活动双星的H_a观测和研究

１９９０年８月至１９９１年８月期间，利用云南天文台１ｍ望远镜折轴摄谱仪附加厚片ＣＣＤ探测器进行了观测，得到二十余颗色球活动双星的大色散、高分辨率，高信噪比的光谱，本文发表其中ηＡｎｄ、３Ｃａｍ、４ＵＭｉ、ｖ２Ｓｇｒ、Ｓｇｒ、ＨＲ７３３３六个双星系统的Ｈａ附近区域光谱观测和研究结果。这六个系统在ＣＡＢＳ表中有关Ｈａ线的资料还是空白。我们给出了它们高分辨率的Ｈａ线轮廓图，计算了它们的等值宽度、半宽、Ｈａ线心的视向速度以及３条金属线视向速度．由观测结果表明，ηＡｎｄ双星的Ｈａ线在不同位相变化不大，没有观测到它的色球活动．３Ｃａｍ由于受色球活动的影响，在０．１５４位相时Ｈａ轮廓发生了突变，其等值宽度明显小于其它位相的等值宽度．４ＵＭｉ的Ｈａ线也是吸收线，但由于受色球活动的影响，致使Ｈａ线心部分受到发射的填充．Ｓｇｒ和ｖ２Ｓｇｒ的光谱Ｈａ线都属于吸收线，没有发现色球活动的影响，很可能不是色球活动星．ＨＲ７３３３是个色球活动比较剧烈的双星，Ｈａ吸收线受到了色球活动引起的发射填充，而且填充量较大．     

活动色球双星HR1099近红外分光光度观测

本文发表了强活动色球双星ＨＲ１０９９（＝Ｖ７１１Ｔａｕ）在１９８９年１２月特大能量白光耀发前后的近红外分光光度观测结果，给出该星从２．３－４．１μｍ首次ＣＶＦ低色散光谱，以及耀发前后的变化；计算了同期观测到的子星表面黑子的影响，给出双星黑体近似辐射能谱，并与多波段测光以及ＩＲＡＳ观测作了对比，揭示了该双星有很强的星周物质的２．３μｍ发射带和３．１μｍ波段吸收带特征，本文对可能的星周物质成分和分布亦作了初步讨论。     

晚型矮星的色球活动

晚型矮星色球ＣａⅡＨ和Ｋ级及Ｈα线发射的波动的时序分析，能提供我们关于恒星活动的许多信息。在晚型矮星上都观测到类似太阳色球活动行为的所有时标变化。在类太阳恒星上找到了类太阳的＂Ｍａｕｎｄｅｒ极小”长期宁静统计意义上的证据；在晚型矮星上完全肯定地观测到十年左右周期的；已用几天到几星期时标的色球活动区的自转调制来测量晚型星的自转周期；在若干晚型星上也已发现几分钟到几小时时标的类耀发现象。     

晚型双星UX Ari的多频射电观测研究

用美国甚大阵（ＶＬＡ）对色球活动性双星系统ＵＸＡｒｉ进行了从１．４ＧＨｚ到１５ＧＨｚ范围内五个频段的观测，观测期间ＵＸＡｒｉ处于活动性比较低的阶段，射电光度为（６．６－１２．６）×１０１６ｅｒｇｓ－１Ｈｚ－１．射电频谱低频部分比较平坦，高频呈幂律形式，低频的圆偏振度很低，趋于零，高频辐射有中等圆偏振度（１５％）．射电发射机制可能是回旋同步加速机制，由此我们估计出发射区的磁场强度为几至几十高斯，相对论电子密度为～１０４－１０２ｃｍ－３量级，热电子数密度～１０８ｃｍ－３。     

耀斑色球压缩区的传播与谱线的不对称性

色球压缩区是耀斑大气动力学过程的一个基本特征，是产生色球谱线红不对称性的基础。本文基于压缩区从大气高层向低层传播的理论公式，在二种不同情况下，计算得到了压缩区内物质运动速度随高度和时间的变化．结果表明，色球蒸发区压力增量Δｐ为常数时压缩区之寿命比压缩区波阵面后的压力ｐ２为常数时要长得多，这就大大缓解了以往谱线不对称性的延续时间的理论值比观测值小的矛盾。形成高度不同的谱线具有不同程度的不对称性这一观测现象也同色球压缩区的传播特性相一致。     

1959年太阳耀斑观测报告

下面发表的是紫金山天文台1959年全年和北京天文台1959年5—12月的耀斑观测结果.北京天文台使用的是苏联 AΦP-2型色球望远镜,紫金山天文台使用的是法国里约(Lyot)型的色球望远镜,这二仪器均约透过 H_a 的带宽为0.65(?).法国里约型色球望远镜的拍摄过程是自动化的,最快每分钟可拍4次,露光时间可维持恒定,使胶卷上太阳象的浓度不会变化,仪器上并附有八级强度标,用以研究耀斑强度的变化.观测结果见下表:     

SMM观测到的白光耀斑

本文收集了ＳＭＭ运行期间（１９８０．２－１９８９．１１）与地面观测相对应的太阳白光耀斑ＨＸＲＢＳ和ＧＲＳ观测资料，就白光耀斑与硬Ｘ－射线发射及伽玛射线发射之产的关系进行了初步的统计研究，结果表明：白光耀斑与伽玛射线发射之间不存在对应关系；白光耀斑也并非全具有强硬Ｘ－射线发射，对那些只具有对较弱的硬Ｘ－射线发射的白光耀斑，我们发现低能粒子具有足够的能量驱动连续发射，因而它们可能起源于色球，而对那些具     

太阳宁静区磁元的空间结构

利用怀柔太阳磁场望远镜,我们对太阳宁静区光球和色球磁场进行了观测。日面中心到边缘的观测表明,太阳宁静区中的小尺度磁结构在从光球到色球的扩展过程中变化不大。日面边缘的观测表明,小尺度磁结构的水平分量在光球和色球都不大。对极区和赤道边缘纵向磁场的比较发现,极区磁场与赤道边缘磁场有着不同的磁结构特性     

大角星的Hell0830A的短时标活动

１９８８－１９９２年间，我们用云南天文台１ｍ望远镜的Ｃｏｕｄｅ－ＣＣＤ摄谱仪系统，对大角星的Ｈｅｉ１０８３０Ａ谱线进行了高分辨率光谱观测。从１９９１年６月２日的观测资料中发现谱线中出现明显的发射特征。该谱线显出类似于天鹅座Ｐ型星的轮廓，有发射射 和吸收谷，发射峰的蓝移有相当于６ｋｍ／ｓ的向外速度。分析认为我们观测到的是大角星的一次以天计的短时标色球剧烈活动，它伴随着物质的向外抛射，也引起星周物质的     

色球和日冕的MHD加热机制

扼要地介绍了色球和日冕加热问题的研究历史。随着空间太阳观测技术的进步，人们认识到色球和日冕加热机制主要与MHD过程有关。因此，在本文中着重介绍四种MHD色球和日冕加热机制：（1）阿尔芬波；（2）MHD湍动；（3）场向电流；（4）磁重联。由于这四种加热机制的有效性都需要通过高分辨率观测来判定，所以空间太阳观测对于研究色球和日冕加热问题具有重大意义。     

On some flare-sensitive high photospheric and low chromospheric lines

During a stay at the Kitt Peak National Observatory the writer has tried to find an influence of flare radiation on the high photospheric and low chromospheric lines of the area occupied by the flare. Observations have been made in the H region and in the region of the H and K lines. When flare emission is present in sunspots some of the faint (molecular) lines seem to be weakened. When a flare appears near the solar limb some of the Evershed-type (chromospheric) lines are strongly influenced.Kitt Peak National Observatory Contribution No. 481.Visiting Astronomer to the Solar Division, Kitt Peak National Observatory, operated by the Association of Universities for Research in Astronomy, Inc. under contract with the National Science Foundation.     

Variations of Flaring Kernel Sizes in Various Parts of the H⍺ Line Profile

We analyze the temporal variations of the sizes and emission intensities of 31 flaring kernels in various parts of the H? line profile. We have found that the areas of all kernels decrease systematically when observed in consecutive wavelengths toward the wings of the H? line, but their areas and emission intensity vary in time. Our results are in agreement with the commonly accepted model of the wine-glass-shaped lower parts of the magnetic flaring loops channelling high-energy variable particle beams toward the chromospheric plasma. High time-resolution spectral-imaging data used in our work were collected using the Large Coronagraph and Horizontal Telescope equipped with the Multi-channel Subtractive Double Pass Spectrograph and the Solar Eclipse Coronal Imaging System (MSDP-SECIS) at the Bia?ków Observatory of the University of Wroc?aw, Poland.     

On a difference of the chromospheric background intensity between the equatorial and polar regions of the sun

Small chromospheric emission centres (here defined as flocculi) were studied photometrically on K _{2, 3, 2} spectroheliograms taken at the Arcetri Observatory. The intensity ratio between I _fl, the flocculus brightness, and I _chr, the brightness of the chromospheric background, was determined. A difference was found between the polar and the equatorial limb values of the ratio I _fl/I _chr.     

Morphology of H-alpha filaments and filament channel systems

Ring-like filaments have been detected on the spectroheliograms in the H-alpha line. Inside these filaments the magnetic field flux has a predominant polarity. Some of the dark filaments are connected by filament channels which can be seen at the limb either as (a) weak prominences or (b) dense low chromospheric features or (c) multi-channel system of matter flow between two prominences or (d) common quiescent prominences. The filament and the filament channel together form a continuous closed contour and outline the region of thef polarity particularly at the beginning of the solar cycle. The change in sign of the polar field of the Sun is associated with the drift of the filament band to high latitudes.     

Are plasma satellites present among chromospheric lines?

From a study of the chromospheric lines listed by Pierce (1968, 1973) indications have been found that first-order plasma satellites appear sometimes as a pair of faint chromospheric emission lines in such places where forbidden lines, mainly of metals, should be located. Second-order satellites are indicated sometimes by an asymmetry in the emission wings of stronger lines, either with respect to intensity or with respect to distance from the line centre and, if so, with the remote wing of diffuse shape. Finally diffuse faint lines, appearing in somewhat greater distances from strong chromospheric lines, suggest the appearance sometimes of fourth-order plasma satellites. All the three types of satellites give electron densities of the order of 10¹² cm^?3. Traces of possible absorption satellites are found also for some of the lines in the solar spectrum. In this connection special attention is drawn to a few faint solar lines located near the wavelengths of corona emission lines. The observational evidence is discussed on the bases of recent theoretical research by Drawin and Truong-Bach (1982a, b).     

Kinematics of a twisted surge

Using the H-alpha solar filtergrams taken at Kandilli Observatory, we have studied the motion of a twisted surge, from the kinematic point of view. We applied the Palu (1972) method to two knots of the twisted surge occurred at 10 November, 1967. The results are discussed.     

XPer的新发射相：光谱与红外观测

ＸＰｅｒ的新发射相：光谱与红外观测杭恒荣，夏剑萍中国科学院紫金山天文台，南京２１０００８中国科学院光学天文联合实验室关键词Ｂｅ星／Ｘ射线双星，发射线，ＪＨＫ测光１引言ＸＰｅｒ是一颗Ｂｅ／Ｘ射线双星（４Ｕ０３５２＋３０）的光学对应体［１－３］，中子星的...     

Chromospheric rotation during 1972–73, years of declining activity

The rotational behaviour of the chromosphere, observed in the Ca ii K₃ line, is studied during 1972–1973, years of decreasing solar activity. Daily chromospheric filtergrams, detected at the Anacapri Observatory, are digitized by means of a flying-spot photometer, controlled by computer. The time series of the daily chromospheric data detected at central meridian, relative to 30 consecutive latitude zones, are analyzed to determine the recurrence tendency due to the rotation of long-lived chromospheric features. The computed rotation rate is independent of latitude, in agreement with the results obtained for the green corona during the years before sunspot minimum. Namely both chromospheric and coronal features, with lifetime exceeding one solar rotation, are almost not affected by differential rotation before sunspot minimum.     

Stellar Active Region Evolution – II. Identification and Evolution of Variance Morphologies in Ca II H+K Time Series

The relative distribution of pooled variance computed at various time scales for records of chromospheric activity has been calculated for approximately 100 stars observed at Mount Wilson Observatory. As shown in Paper I, analysis of the pooled variance provides a technique for estimating the lifetimes of stellar active regions and their influence on chromospheric time series used for determining rotation and activity cycle periods. Pooled variance diagrams may be divided into three morphological types which depend to a large extent on a star's mean level of chromospheric activity (i.e., age) and B-V color (i.e., mass), and possibly depend on star's evolutionary state.     

Spectroscopic observations of zeta Aurigae during the 1971–72 eclipse

The chromospheric phases in the 1971–72 eclipse were observed at wavelength regions containing the K-line of ionized calcium on six nights at ingress and on eight nights at egress at the Okayama Astrophysical Observatory. The linear dispersion of the spectrograms is about 10 Å mm^?1. The spectrograms were measured for line intensities of the K-line and for radial velocities of metallic and hydrogen lines. The results are compared with those obtained in the earlier eclipses. The intensities of the chromospheric K-line during this eclipse were relatively ‘weak’ at both ingress and egress and were similar to those in the 1939–40 eclipse. It seems that the chromospheric activity of ζ Aurigae increased after 1939, reached a maximum at 1950–56, and then decreased again until 1971. The radial velocities of the chromospheric lines of hydrogen atoms, ionized calcium, and some other atoms and ions varied with phase showing almost the same characteristic features as in most earlier eclipses. Intensities and velocities were also measured for satellite lines of the K-line.