1997年3月9日日全食8.6mm波段射电观测

１９９７年３月９日日全食８．６ｍｍ波段射电观测资料的分析表明,８．６ｍｍ波段射电太阳的半径为１．０１２Ｒ,总流量为２５４０ｓｆｕ（１ｓｆｕ＝１０＾－２２Ｗ／ｍ＾２Ｈｚ）,日面平均亮温度为９６３２Ｋ,径向亮温度分布,在日面光学边缘内侧０．９３６－０．９９２Ｒ处,存在临边增亮,平均增亮幅度相对于日面中心为９．７％。     

1997年3月9日日全食(英)

1997年3月9日的日全食是本世纪中国可见的最后一次日全食．对这次日食概况和中国、特别是漠河地区见食的情况作一介绍．这次观测结果基本上与预报一致,文中所列各表供观测者处理资料时参考．     

1997年3月9日的日冕偏振CCD观测

给出１９９７年３月９日日全食时所作的日冕偏振ＣＣＤ观测资料的处理结果,包括太阳赤道东西和两极等十二个方向的中冕（１．６－３．２Ｒ）绝对亮度分布和偏振度分布。     

8.6毫米波段太阳射电亮温度分布的日环食测定

本文根据１９８７年９月２３日的８．６毫米波段射电日食观测资料，计算了太阳射电的径向亮温度分布，计算结果表明：８．６毫米波段太阳径向亮温度分布呈临边增亮；增亮幅度相对于日面中心部分为５．１％，中国部分也存在着增亮的征兆；日食当天８．６毫米波段太阳射电辐射的剖流量为２３４６Ｓ、ｆ、Ｕ；食甚时的剩余流量约为１２．５％，掩食半径为１．０１４光学太阳半径。     

1997年3月9日漠河日全食外冕观测方案

目前太阳活动处于极小期，太阳表面的活动区磁场处于相对不活动状态。但暗条和冕洞等活动形式仍有存在。特别是极区冕洞，其性质仍有许多疑团不被人所知。例如磁场对冕洞的影响。在中低太阳纬度，冕洞出现在大块的磁场单极区。然而在高纬区情况如何呢？冕洞在极区经常存在（极区冕洞），但并不总是存在。我们曾看到美国高山天文台（ＨＡＯ）于１９７３观测的一幅日全食照片，其南极有明显的极区冕洞，而北极区存在有纤细而美丽的冕羽。我国１９６８年和１９８０年两次日全食所观测的资料只有中内冕（Ｒ⊙—１．５Ｒ⊙以内），Ｒ⊙大于１．５Ｒ⊙的外日冕平时还只有在空间才能得到。１９９７年３月９日日全食是本世纪我国国土上观测日冕的良好机会，但条件限制我们不能携带专门用于日全食观测的大型设备，本文提出了一种用普通摄像机拍摄日冕像而再进行图像采集处理的方法，以获得Ｒ⊙大于等于２范围的日冕观测方案。另外在日全食观测前后，需要用同一台摄像机在同盘磁带上对黑暗进行拍摄以备暗场处理之用。再用同台摄像机和ＧＧ１１滤光片在同盘磁带上对均匀天空进行拍摄以作黄光，白光平场背景之用。根据不同研究的需要，在资料处理时，应作相应的绝对定标，大气消光及位移的改正。     

1997年3月9日全食

１９９７年３月９日的日全食是本世纪中国可见的最后一次日全食,对这次日食概况和中国,特别是漠河地区见食的情况作一介绍。这次观测结果基本上与预报一致,文中所列各表供观测者处理资料时参考。     

1997年3月9日漠河日全食外冕观测方案

目前太阳活动处于极小期，太阳表面的活动区磁场处于相对不活动状态，但暗条和冕洞等活动形式仍有存在，特别是极区冕洞，其性质仍多疑团不被人所知，例旭磁场对冕洞的影响，在中低太阳纬度，冕洞出现大块的磁场单极区，然而在高纬区情况如何呢？冕洞在极区经常存在（极区冕洞），但并不总是存在。我们曾看到美国高山天文台（ＨＡＯ）于１９７３观测一幅日全食照片，其南极有明显的极区冕洞，而北极区存在有纤细而美丽的冕羽，我国１     

1997年3月9日3.2cm射电日食观测

本文介绍了1997年3月9日,紫金山天文台在3.2cm波段上日偏食观测概况及所得到的结果。     

8.6毫米波段太阳射电亮度温度分布

本文根据１９８０年２月１６日的８．６毫米波长射电日食观测资料，计算了太阳射电辐射的亮度温度的径向分布，由日食过程的第一，第二和第三接触的计算结果表明，在日面光学边缘内侧的二角分范围内，均存在明显的单峰状增亮结构。三个接触的平均增亮峰值约为１８％，增亮区的射电辐射占日面总辐射的４％。日食当天在８．６毫米波段上测得的日面平均亮度温度为９７２７Ｋ。     

1997年3月9日漠河日全食外日冕结构及相对强度分布

利用简单的视频图像采集系统 ,对 1 997年 3月 9日用PanasonicNV -S880EN型摄像机拍摄的黑龙江漠河日全食黄光 (加GG1 1滤光片 )和白光日冕观测资料进行计算处理 ,得到大于 1 .5R⊙ 的太阳活动低年外日冕结构及其相对强度分布。     

Observation of the 1997-03-09 total eclipse at 8.6 mm

COPY THE ORIGINAL Analysis of the total eclipse observation of 1997 March 9 at wavelength 8.6 mm, shows that, at this wavelength, the solar radius is 1.012 R_⊙, the total flux density is 2540 sfu, the mean brightness temperature of the solar disk is 9632 K, and the brightness temperature distribution shows limb brightening at the inner edge of the solar disk, the average brightness at 0.936−0.992 R_⊙ being 9.7% above the central brightness.     

Observations of the 21 June 2001 Total Solar Eclipse

Total solar eclipses are rare events, but the publicity surrounding them is generating a lot of interest. These events can be used to popularize astronomy and promote science awareness. The internet is gaining popularity as a medium to view eclipses remotely as is evidenced by the number of websites devoted to the 2001 solar eclipse. More internet webcasts are needed to meet the demand that these events generate. The attempt by a team from the Astronomy Department at the University of South Africa to broadcast a streaming video of the 21 June 2001 total eclipse from Lusaka on the internet are described. All the necessary equipment is commercially available. Lessons learnt from this eclipse can be used to prepare for future events. This revised version was published online in July 2006 with corrections to the Cover Date.     

Properties of the noise storm source at wavelength 1 m from observations of the solar eclipse on March 29, 2006

Observations of the solar eclipse on March 29, 2006, at the Laboratory of Radio Astronomy of the CrAO showed that the radio radius of the Sun at a wavelength of 1 m in the direction of the first contact was R _d = 1.12 R _⊙ during solar activity minimum between cycles 23 and 24. The brightness temperature of the undisturbed Sun was T _d = (0.6 ± 0.06) × 10⁶ K. There was a noise storm source above the sunspot group NOAA 0865 whose bright nucleus had a size of 1′.3 and a brightness temperature T _b = 16 × 10⁶ K. The noise storm bursts were emitted from the region of the bright nucleus above the group NOAA 0865 and were absent during its covering by the disk of the Moon. Thermal radiation from a coronal condensation with a brightness temperature of (1?2) × 10⁶ K extending out from the visible solar disk to 2′.7 was observed during the eclipse above the eastern limb sunspot group NOAA 0866. The bright nucleus in this limb source appeared 42 min after eclipse termination and persisted in the ensuing days. This may be indicative of the time of its emergence from behind the radio horizon formed by regular refraction of radio waves in the corona. The refractive displacement was measured by comparison with the eclipse observations at a shorter wavelength of 12 cm. Its value of 0′.96 is close to the calculated value of 0′.8.     

1991年7月11日墨西哥日全食红外光谱观测及初步结果

本文概述１９９１年７月１１日日全食时中国日食观测队在墨西哥ＬａＰａｚ所作的近红外光谱观测情况及得到的初步结果。观测是用一强光力望远镜和一中小色散的光谱仪，配以ＣＣＤ摄象机、图象处理器、微机等组成的探测系统进行的。日全食时，在λ１０７１２－１０９７２波区共摄得极上层光球和色球的无缝光谱４１帧。日面外约１．０９６Ｒ处的有缝光谱３５帧。文中还介绍了拍得的色球、日珥资料概况。     

A Check on the Variations of Earth‘s Rotation with an Ancient Solar Eclipse

We address the relation between an ancient total eclipse, which occurred on A.D.1542 August 11 and the variation of Earth‘‘s rotation. The total eclipse was recorded in some ancient Chinese books, especially in local chronicles. Some of the documents include useful information for determining the location of the totality zone. The parameters of the eclipse are calculated by using the DE406 Ephemeris.A high-precision value of AT which expresses the variation of the Earth‘‘s rotation,of about 300 ～ 380 s, is obtained.     

2006年3月29日日全食白光日冕偏振测量

报告了在埃及赛路姆观测到的2006年3月29日日全食白光偏振测量的基本结果.我们使用的是一架便携式反射望远镜,焦距为640mm(F/D=8).在物镜前方安置可旋转线偏振片,每次旋转角度45°,终端为尼康数码相机.观测过程中,改变曝光时间并旋转偏振片,总共获取20张数码照片.文中讨论并呈现了介于 1.3 R⊙＜r ＜3.0 R⊙范围内的白光偏振方向和偏振度的大小分布.     

Interferometer observations of the solar brightness distribution at 8.6 mm wavelength

The brightness distribution of the quiet Sun at 8.6 mm wavelength is synthesized from off-meridian observations using an eight element east-west interferometer with a maximum base line of 16.38 m (1913). The observed brightness distribution is practically flat from the disk center to the optical limb. The effective radius of the nearly uniform component is 1.01 R . If the limb brightening is present, the brightening located between 0.95 R and 1.01 R , and the total flux density of the limb brightening is less than 1% of the total flux density of the Sun. In addition to the nearly uniform component there exists a coronal component just outside the optical limb.