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1.
都没有日全食发生,大家要想观测则要等到2015年3月20日,届时一次日全食将在北冰洋上演。2014年共有两次日食和两次月食,日食包括1次日环食和1次日偏食,而这两次日食我国都不可见。两次月食则都是月全食,其中10月8日的那次我国可见,但只有部分地区观测条件尚可。 相似文献
2.
张培瑜 《紫金山天文台台刊》1994,13(1):23-31
古代日月食观测记录是研究过去几千年地球自转长期变化的最有用的材料, 本文对文献记载的中国古代(明末以前)的日食观测作了分析讨论。指出,西汉以后资料是系统完整的。多为当时首都的观测记录。可惜的是,古人不重视记录天象发生的准确时刻。 作者从这些材料中筛选出13次观测地点明确的日全食观测,探讨分析了地球自转长期变化的趋势。 相似文献
3.
2014年已经过去四分之三,在中国境内貌似还没看过日月食。是的,对中国来说,今年是日月食比较少的年份。今年在全球会发生两次日食和两次月食,其中的一次日食和一次月食已经在4月份发生了,但是在中国几乎都看不到。另外一次日食和—次月食都将在10月份发生,我们先来看看月食的情况。 相似文献
4.
１９９７年３月９日在云南天文台对日偏食进行了光学观测，取得了不同时刻的日面掩食过程的白光资料，是射电等观测分析研究的重要依据。 相似文献
5.
本文作者是参加过5次日食观测的天文科普工作者,曾多次带领青少年天文爱好者进行观测。具有丰富的实际观测经验,作者根据多次观测的经验体会及青少年天文爱好者进行观测时容易出现的问题进行了几个方面的提示,相信定会对首次进行日食观测的老师和同学有所帮助。 相似文献
6.
本文介绍了１９９５年１０月２４日亚洲将要发生的日全食概况，提出了届时昆明日食的观测选题，文中对时频、射电和色球观测选题的意义和可能的观测结果作了预测性的讨论。 相似文献
7.
古本《竹书纪年》记载有：“周昭王十九年，天大噎，雉兔皆震，丧六师于汉。”这与阴天发生的日全食现象十分相似。事件发生在昭王末年南征荆楚的过程中，地点应当在从周都到洞庭湖以南之间的某处。由前人的研究可知昭王十九年应在公元前1010。940年之间。在充分讨论了天文计算的不确定性后得到这一地区可见的9次大食分日食，其中公元前1009和976年的两次日食可能在洞庭湖以南造成日全食，其他地点也都有相当大的食分。在对夏商周断代工程得到的西周年表作微小调整后，昭王十九年天大睦可以认定为公元前976年5月31日日全食。这对“夏商周断代工程”所定出的昭王前后年代是一个独立的支持。 相似文献
8.
苍凉西部,壮丽日食。2008年8月1日,笔者有幸在我国甘肃省酒泉市金塔县鸳鸯池水库边,观测了生平的第一次日全食。其实在今年5月号杂志的“观测攻略”系列文章中,笔者就已经对日食观测做了比较详细的介绍。不过,事实上笔者此前从未观测过日全食,文中的内容主要来自于别人的观测心得,以及自己在天文观测上的总体经验。而这次,笔者经过精心规划,终于成功观测了自己的第一次日全食。其中的一些观测体会,以及观测成果,在这里拿出来和大家分享。 相似文献
9.
本文介绍了１９９５年１０月２４日亚洲将要发生的日全食概况。提出了届时昆明日食的观测选题。文中对时频、射电和色球观测选题的意义和可能的观测结果作了预测性的讨论。 相似文献
10.
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。 相似文献
11.
日食为射电天文提供了一维高空间分辨率太阳射电观测机会．日食射电观测在太阳射电物理的发展上起过重要的作用．文中对日食射电观测的若干重要因素作了介绍和分析．日食射电观测在我国太阳射电天文发展上也起了重要作用．文中简要介绍了在我国组织观测的1958年、1968年、1980年及1987年的太阳射电日食观测及其主要结果． 相似文献
12.
The realization that solar activity probably undergoes changes in qualitative character on time scales greater than the 11 or 22 year cycle but short compared to the duration of recorded history gives renewed importance to historical documents describing the state of solar activity. Modern eclipse observation reveal the presence of solar activity through the appearance of coronal structures and prominences. It has been widely remarked that eclipse records prior to the 18th century are uniformly silent on these conspicuous solar eclipse features, raising the possibility, however unlikely, that a change in solar activity has occurred which rendered them only recently noticeable. We present here material from ancient Chinese sources, primarily astrological, that describe phenomena attending solar eclipses that are almost certainly coronal structures and prominences. Thus, these aspects of the present character of solar activity have apparently occurred at other times in history, if not continuously. 相似文献
13.
The diameter of the Sun may be measured at the time of a solar eclipse. We have performed an exhaustive search of the astronomical literature to find all existing observations of solar eclipses suitable for this purpose. We have also taken new observations by new techniques. We have undertaken a project to reduce them systematically, and in an automated, self-consistent way. This will produce determinations of the solar radius at the times of solar eclipses from 1715 to the present. Re-reduction, using newer ephemerides, of observations made in 1984 shows that the component of the residuals caused by the ephemeris is substantially reduced. This paper summarizes the research plan, outlines the detailed astronomical features included in the calculations, and presents the results available. 相似文献
14.
V. M. Bogod O. A. Golubchina G. N. Zhekanis A. N. Korzhavin V. S. Kotel’nikov N. A. Nizhel’skij P. G. Tsybulev 《Astrophysical Bulletin》2007,62(4):360-368
We report the results of unique observations of the solar eclipse of March 29, 2006 over a wide radio-wavelength range from 1 to 50 cm made with the large RATAN-600 stationary radio telescope during the maximum eclipse phase performed using the method of the source transit across the fixed beam pattern. The multifunctional opportunities of the radio telescope allowed observations to be performed simultaneously in a part of the Northern sector of RATAN-600 and in the Southern-sector plus periscope mode using all the available receiving equipment at the corresponding secondary mirrors. At the time of maximum eclipse phase a narrow 1—3-arcsec wide crescent-shaped band near the North Solar Pole remained visible out of the entire solar disk covered by the Moon. We achieved high flux sensitivity, which allowed us to discover a large polar radio source located above the North Solar Pole and obtain detailed data on its radiation and spatial structure. Moreover, we detected optically thin radiation of the solar corona at the brightness-temperature level of several K or several tens of K. We find this radiation to extend beyond the solar limb out to the heliocentric distances of one solar radius. These data are unique in that they are not contaminated by scattered radiation of the solar radio disk, which usually shows up in ordinary observations. We are the first to obtain a detailed spectrum of the radiation of a high-latitude prominence at many wavelengths with a 1% frequency resolution in the microwave range, which allowed us to estimate its magnetic field at a number of levels in the lower corona. 相似文献
15.
周树荣 《紫金山天文台台刊》1998,17(4):1-7
本文介绍了日食射电观测及其资料预处理的基本方法。其中包括日食观测点的选址、观测前的准备、日食观测和食后资料的预处理等。通过资料预处理 ,可得到归一化天线温度和斜率食变曲线 ,为研究日面亮度温度分布和射电源参数等基本物理量提供基本数据和资料 相似文献
16.
Jay M.Pasachoff 《中国天文和天体物理学报》2009,9(6)
The occasion of the longest totality of an eclipse in the 18 yr 111/3 d saros cycle leads to taking stock of the scientific value of ground-based eclipse observations in this space age. Though a number of space satellites from the U.S., Europe, Japan, and Russia study the Sun, scientists at eclipses can observe the solar chromosphere and corona at higher spatial resolution, at higher temporal resolution, and at higher spectral resolution than are possible aloft. Furthermore, eclipse expeditions can transport a wide variety of state-of-the-art equipment to the path of totality. Thus, for at least some years to come, solar eclipse observations will remain both scientifically valuable and cost-effective ways to study the outer solar atmosphere. 相似文献
17.
Cowsik Ramanath Singh Jagdev Saxena A.K. Srinivasan R. Raveendran A.V. 《Solar physics》1999,188(1):89-98
Encouraged by the detection of high-frequency, low-amplitude continuum intensity oscillations in the solar corona during the total solar eclipse of 1995, we designed and fabricated a six-channel photometer incorporating low-noise Hamamatsu R647 photomultipliers. Fast photometry at five different locations in the solar corona was performed at Don Bosco Mission, Venezuela during the total solar eclipse of 26 February 1998. Three interference filters with passbands of about 150 Å and centered around 4700, 4900, and 5000 Å were used. The photometric data were recorded at a rate of 20 Hz in three channels and 50 Hz in the remaining three channels. The power spectrum analysis of one of the channels that recorded appreciable counts indicates the existence of intensity oscillations in the frequency range 0.01–0.2 Hz. A least-squares analysis yields 90.1, 25.2, and 6.9 s periods for the three prominent components which have amplitudes in the range 0.5–3.5% of the coronal brightness. These periods and their amplitudes are similar to those detected in the coronal intensity oscillations during the 1995 eclipse. 相似文献
18.
The brightness temperature distributions of the solar atmosphere in the polar region at the distances from one to two solar radii during the solar activity minimum are reported. Observations of the maximum phase of the solar eclipse of March 29, 2006 were carried out simultaneously on two sectors of the RATAN-600 radio telescope over a wide range of centimeter waves, 1–31 cm. This study is based on a comparison of models and observations carried out on the northeastern sector of the RATAN-600. 相似文献
19.
Yoichiro Hanaoka Jun Nakazawa Osamu Ohgoe Yoshiaki Sakai Kazuo Shiota 《Solar physics》2014,289(7):2587-2599
White-light observations of the total solar eclipse on 13 November 2012 were made at two sites, where the totality occurred 35 min apart. The structure of the corona from the solar limb to a couple of solar radii was observed with a wide dynamic range and a high signal-to-noise ratio. An ongoing coronal mass ejection (CME) and a pre-CME loop structure just before the eruption were observed in the height range between 1?–?2 R⊙. The source region of CMEs was revealed to be in this height range, where the material and the magnetic field of CMEs were located before the eruption. This height range includes the gap between the extreme ultraviolet observations of the low corona and the spaceborne white-light observations of the high corona, but the eclipse observation shows that this height range is essential for the study of CME initiation. The eclipse observation is basically just a snapshot of CMEs, but it indicates the importance of a continuous coverage of CME observations in this height range in the future. 相似文献
20.
A. A. Nusinov T. V. Kazachevskaya V. V. Katyushina K. V. Kuimov O. I. Bugaenko V. A. Slemzin N. I. Lebedev 《Solar System Research》2006,40(4):348-353
The CORONAS-F spacecraft crossed the zone of the ring solar eclipse three times on May 31, 2003. A considerable decrease in solar radiation was detected by the spacecraft instruments for these moments. The passages through the eclipse zone were registered by the VUSS instrument, which measured the shortwave solar radiation flux near the hydrogen Lyman alpha line, and by the DIFOS instrument, which was sensitive to infrared, visible, and near-ultraviolet radiation. The eclipse is also clearly seen in solar images obtained by the X-ray SPIRIT telescope. Some details of measurement results are discussed. 相似文献