RAPID CHANGES IN THE FINE-STRUCTURE OF A CORONAL BRIGHT POINT AND A SMALL CORONAL ACTIVE REGION

被引：104

作者：

SHEELEY, NR ^{[1
]}

GOLUB, L ^{[1
]}

机构：

[1] HARVARD UNIV,SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138

来源：

SOLAR PHYSICS | 1979年 / 63卷 / 01期

关键词：

D O I：

10.1007/BF00155702

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A coronal 'bright point' is resolved into a pattern of emission which, at any given time, consists of 2 or 3 miniature loops (each ∼2500 km in diameter and ∼12 000 km long). During the half-day lifetime of the 'bright point' individual loops evolved on a time scale ∼6 min. A small 'ctive region' seemed to evolve in this way, but the occasional blurring together of several loops made it difficult to follow individual changes. © 1979 D. Reidel Publishing Co.

引用

页码：119 / 126

页数：8

共 18 条

[1]

Culhane J. L., 1970, Solar Physics, V15, P394, DOI 10.1007/BF00151847

[2] OBSERVATIONAL EVIDENCE OF CONTINUAL HEATING IN X-RAY EMITTING CORONAL LOOPS [J].

GERASSIMENKO, M ;

SOLODYNA, CV ;

NOLTE, JT .

SOLAR PHYSICS, 1978, 57 (01) :103-110

[3] OBSERVATION OF A NONUNIFORM COMPONENT IN DISTRIBUTION OF CORONAL BRIGHT POINTS [J].

GOLUB, L ;

KRIEGER, AS ;

VAIANA, GS .

SOLAR PHYSICS, 1975, 42 (01) :131-134

[4] MAGNETIC-PROPERTIES OF X-RAY BRIGHT POINTS [J].

GOLUB, L ;

KRIEGER, AS ;

HARVEY, JW ;

VAIANA, GS .

SOLAR PHYSICS, 1977, 53 (01) :111-121

[5] OBSERVATION OF SPATIAL AND TEMPORAL VARIATIONS IN X-RAY BRIGHT POINT EMERGENCE PATTERNS [J].

GOLUB, L ;

KRIEGER, AS ;

VAIANA, GS .

SOLAR PHYSICS, 1976, 50 (02) :311-327

[6]

GOLUB L, 1976, SOL PHYS, V49, P79, DOI 10.1007/BF00221486

[7]

Harvey J., 1977, Highlights of Astronomy, P223

[8]

HARVEY KL, 1975, SOL PHYS, V40, P87

[9] EFFECT OF NON-LINEAR CONDUCTION ON COOLING OF FLARE LOOPS [J].

KRALL, KR .

SOLAR PHYSICS, 1977, 55 (02) :455-458

[10]

Krieger A. S., 1971, SOLAR MAGNETIC FIELD, V43, P397

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