Observations of Solar Corona at the Mexico Total Solar Eclipse of July 11, 1991

1991 年 7 月 11 日墨西哥日全食的日冕观测

• 批准号: 02041094
• 负责人: YAMASHITA Yasumasa
• 金额: $ 5.12万
• 依托单位: National Astrpopmical Observatory
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for international Scientific Research
• 财政年份: 1990
• 资助国家: 日本
• 起止时间: 1990 至 1991
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-02041094/
• 关键词: Total Solar Eclipse; 11 JUly, 1991; Solar Corona; Japanese Eclipse Expedition; Mexico; LA PAZ City; Universidad Autonoma DE Baja California Sur; MT. Popocatepetle; 予備調査; 南バハカリフォルニア自治大学

The 11-July-1991 Eclipse was one of the most important eclipse in this century because of its longest duration of totality. The purpose of this research project was to observe the solar corona and to study its physical condition by using this rare oppoetunity.Japanese Eclipse Expedition consists of three institutes, i. e. National Astronomical Observatory (6persons), Kyoto university (3persons), and Hydrographic Department of Japan (2persons). The former two institutes were supported by this Grant under The Monbusho International Scientific Research. Three teams from Nationl Astron. Obs., Kyoto Univ. and Hydro. Depart. observed at the Campus of UABCS (Universidad Autonoma de Baja California Sur), and one team from National Astr. Obs., on the top of Mt. Popocateptle. The sky condition was perfect and the seeing condition was good at UABCS. It was fine before the 2nd contact, but a thin cirrus ran over the sun at Mt. Popocatepetle.The instrumentation, general features of obtained data, a … More nd the results of a preliminary analysis are briefly summarized below.(1) Observation of Fine Structures in the Inner CoronaHigh resolution pictures of the inner corona were obtained in the lights of FeX6374A, FeXIV5303A, CaXV5694A, Halpha lines and 6100A continuum. The 6374 loop structures are found to be finer than any other 10^6K coronal loops which have ever been published. The emission-line images represent the fine structures of 1x10^6K (FeX), 2x10^6K (FeXIV), 3.5xl0^6K (CAXV) and 1x10^4 (HI) respectively, and the continuum images show the electron column density distribution. The detailed cottiparison of thein enables us to study the temperature-density structures of various types of coronal fine structures.(2) Observation of the Cool Material in the CoronaThe coronal images were taken in the light of HeI10830A, Fe5303A linese and 10000 continuum. Spectrographic observations were also made in the wavelength region of violet (lambda lambda3760-4060) and infrared (lambda lambda10745-10835)to obtain the detailed physical condition of the corona, especially of its cool part. The data obtained does not show any distinct cool structures other than ordinary prominences.(3) Observation of the Coronal RaysWhite light coronal pictures were observed to study the width-variations of the coronal rays. It is found that most of the rays expand lineally with distance with the rate of 20-50 arcsec per solar radius.(4) Polarization Observation of the Solar F-CoronaPolarization of F-corona was measured in four wavelengths, i. e., 5325A, 5965A, 7200A, 8015A to study how far interplanetary dust grains reach to sun. With some assumptions, the map of two dimensional polarization distribution of the outer corona was obtained. It shows high polarization regions co-incident with coronal streamers. Less

1991年7月11日的日食是本世纪最重要的日食之一，因为它的全食持续时间最长。日本日蚀考察队由日蚀观测所、日蚀观测所、日蚀观测所和日蚀观测所组成。e.国立天文台（6人）、京都大学（3人）、日本水文厅（2人）。前两个研究所得到了Monbusho国际科学研究基金会的资助。三支来自国家宇航局的队伍，京都大学和Hydro.出发吧在UABCS（南下加利福尼亚自治大学）的校园里观察到，在山顶上。波波卡特普特天空条件是完美的，在UABCS的视情况是好的。在第二次接触之前，天气很好，但是在Mt. Popocatepetle。仪器，获得的数据的一般特征， ...更多信息 现将初步分析的结果简述如下。(1)利用FeX 6374 A、FeXIV 5303 A、CaXV 5694 A、H α谱线和6100 A连续谱线，获得了高分辨率的内日冕图象。发现6374个环结构比任何其他已发表的10^6K日冕环都要精细。发射谱线图像分别代表了1 × 10^6K（FeX）、2 × 10^6K（FeXIV）、3.5 × 10^6K（CAXV）和1 × 10^4（HI）的精细结构，连续图像显示了电子柱密度分布。详细的计算结果使我们能够研究各种类型日冕精细结构的温度-密度结构。(2)日冕中冷物质的观测用HeI 10830 A、Fe 5303 A谱线和10000连续谱线拍摄日冕象。还在紫波段（λ = 3760 -4060）和红外波段（λ = 10745 -10835）进行了光谱观测，以获得日冕，特别是其冷部分的详细物理状况。获得的数据没有显示出任何明显的冷结构以外的普通双折射。(3)日冕射线的观测观测了白光日冕照片，研究了日冕射线的宽度变化。发现大部分射线的膨胀与距离成线性关系，膨胀率为20-50弧秒/太阳半径。(4)太阳F-日冕的偏振观测在四个波长上测量了F-日冕的偏振。例如，5325 A，5965 A，7200 A，8015 A，研究行星际尘埃颗粒到达太阳的距离。在一定的假设条件下，得到了外日冕的二维极化分布图。它显示了与日冕流光同时发生的高偏振区域。少

项目成果

S. ISOBE: "Dust Surrounding the Sun - F Corona" Observation of Solar Corona at the Mexico Total Solar Eclipse of July 11.1991. 95-102 (1992)

S. ISOBE：“太阳周围的尘埃 - F Corona”1991 年 7 月 11 日墨西哥日全食的日冕观测。

黒河 宏企,北井 礼三郎,石浦 清美: "THE OBSERVATION OF THE INNER CORONA AT THE 1991 TOTAL SOLAR ECLIPSE" 平成3年7月11日メキシコ日食による太陽コロナの観測. 10-41 (1992)

Hiroshi Kurokawa、Reisaburo Kitai、Kiyomi Ishiura：“THE OBSERVATION OF THE INNER CORONA AT THE 1991 TOTAL SOLAR ECLIPSE” 1991年7月11日墨西哥日食期间日冕的观测。10-41 (1992)

H. KUROKAWA, R. KITAI, K. ISIURA: "The Observation of the inner Corona at the 1991 Total Solar Eclipse" Observation of Solar Corona at the Mexico Total Solar Eclipse of July 11, 1991. 10-41 (1992)

H. KUROKAWA、R. KITAI、K. ISIURA：“1991 年日全食时内日冕的观测”1991 年 7 月 11 日墨西哥日全食的日冕观测。10-41 (1992)

S. ISOBE, M. NOGUTHI, T. TANABE: "Total Solar Eclipse 1991, Observation of F-Corona at MT. Popokatepetoru" Observation of Solar Corona at the Mexico Total Solar Eclipse of July 11.1991. 42-45 (1992)

S. ISOBE、M. NOGUTHI、T. TANABE：“1991 年日全食，MT. Popokatepetoru 的 F 日冕观测” 1991 年 7 月 11 日墨西哥日全食的日冕观测。

福島 英雄,末松 芳法,西野 洋平: "THE STRUCTURE OF THE CORONAL RAYS(STREAMLINES)AT THE ECLIPSE ON JULY 11,1991,IN IN LA PAZ,BCS,MEXICO" 平成3年7月11日メキシコ日食による太陽コロナの観測. 62-66 (1992)

Hideo Fukushima、Yoshinori Suematsu、Yohei Nishino：“1991 年 7 月 11 日日食中日冕射线（流线）的结构，位于墨西哥BCS 拉巴斯” 1991 年 7 月 11 日墨西哥日食造成的太阳观测电晕 62-66 (1992)