Structure of a large low-latitude coronal hole

被引：32

作者：

Bromage, BJJ ^{[1
]}

Alexander, D

Breen, A

Clegg, JR

Del Zanna, G

DeForest, C

Dobrzycka, D

Gopalswamy, N

Thompson, B

Browning, PK

机构：

[1] Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England

[2] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA USA

[3] Max Planck Inst Aeron, Katlenburg Lindau, Germany

[4] NASA, Goddard Space Flight Ctr, SOHO SOI MDI, Greenbelt, MD 20771 USA

[5] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[6] Catholic Univ Amer, NASA, GSFC, Greenbelt, MD USA

[7] NASA, Goddard Space Flight Ctr, Space Applicat Corp, Greenbelt, MD 20771 USA

[8] Univ Manchester, Inst Sci & Technol, Manchester M60 1QD, Lancs, England

来源：

SOLAR PHYSICS | 2000年 / 193卷 / 1-2期

关键词：

D O I：

10.1023/A:1005209725885

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Coronal holes on the Sun are the source of high-speed solar wind streams that produce magnetic disturbances at the Earth. A series of multi-wavelength, multi-instrument observations obtained during the 1996 'Whole Sun Month' campaign examined a large coronal hole in greater detail than ever before. It appeared on the Sun in August, and extended from the north pole to a large active region in the southern hemisphere. Its physical and magnetic structure and subsequent evolution are described.

引用

页码：181 / 193

页数：13

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