A multi-wavelength analysis of the February 6/7, 1997 coronal mass ejection

被引：0

作者：

Plunkett, SP ^{[1
]}

Gopalswamy, N ^{[1
]}

Kundu, MR ^{[1
]}

Howard, RA ^{[1
]}

Thompson, BJ ^{[1
]}

Gurman, JB ^{[1
]}

Lepping, RP ^{[1
]}

Hudson, HS ^{[1
]}

Nitta, N ^{[1
]}

Hanaoka, Y ^{[1
]}

Kosugi, T ^{[1
]}

Burkepile, JT ^{[1
]}

机构：

[1] USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA

来源：

CORONA AND SOLAR WIND NEAR MINIMUM ACTIVITY - FIFTH SOHO WORKSHOP | 1997年 / 404卷

关键词：

coronal mass ejections; prominence eruption; interplanetary shocks; geomagnetic effects;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The partially earth-directed coronal mass ejection (CME) event of February 6-7, 1997 originated from the southwest quadrant of the sun. The CME accelerated from a projected speed of 170 km/s to about 650 km/s when it reached a distance of 25 R.. The CME was an arcade eruption followed by bright prominence core structures. The prominence core was tracked continuously from the solar surface to the interplanetary medium by combining data from the Nobeyama radioheliograph (microwaves), Mauna Loa Solar Observatory (He I 10830 Angstrom), SOHO/EIT (EUV) and SOHO/LASCO (white light). The CME was accompanied by an arcede formation, fully observed by the Yohkoh/SXT (soft X-rays) and SOHO/EIT. The X-ray and EUV observations suggest that the reconnection proceeded from the northwest end to the southeast end of a filament channel. In the SOHO/EIT images, the feet of the soft X-ray arcade were observed as EUV ribbons. The CME event also caused interplanetary effects that were observed by instruments on WIND, and produced a medium sized geomagnetic storm at Earth starting on February 9. This event confirms a number of ideas about CMEs: the three part structure (frontal bright arcade, dark cavity and prominence core), disappearing filament, elongated arcade formation, and terrestrial effects. We make use of the excellent data coverage to address a number of issues regarding the origin and propagation of geoeffective solar disturbances.

引用

页码：615 / 618

页数：4