Publications (8)2.78 Total impact
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Article: Eruption and acceleration of flare-associated coronal mass ejection loops in the low corona
jgr. 11/2001; 106:25215-25226. -
Article: Observations of the 24 September 1997 Coronal Flare Waves
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ABSTRACT: We report coincident observations of coronal and chromospheric flare wave transients in association with a flare, large-scale coronal dimming, metric radio activity and a coronal mass ejection. The two separate eruptions occurring on 24September 1997 originate in the same active region and display similar morphological features. The first wave transient was observed in EUV and H data, corresponding to a wave disturbance in both the chromosphere and the solar corona, ranging from 250 to approaching 1000kms–1 at different times and locations along the wavefront. The sharp wavefront had a similar extent and location in both the EUV and H data. The data did not show clear evidence of a driver, however. Both events display a coronal EUV dimming which is typically used as an indicator of a coronal mass ejection in the inner corona. White-light coronagraph observations indicate that the first event was accompanied by an observable coronal mass ejection while the second event did not have clear evidence of a CME. Both eruptions were accompanied by metric typeII radio bursts propagating at speeds in the range of 500–750kms–1, and neither had accompanying interplanetary typeII activity. The timing and location of the flare waves appear to indicate an origin with the flaring region, but several signatures associated with coronal mass ejections indicate that the development of the CME may occur in concert with the development of the flare wave.Solar Physics 03/2000; 193(1):161-180. · 2.78 Impact Factor -
Article: Properties of coronal mass ejections: SOHO LASCO observations from January 1996 to June 1998
jgr. 01/2000; 105:18169-18186. -
Article: Observations of the September 24, 1997 Coronal Flare Waves
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ABSTRACT: We report the coincident observations of coronal and chromospheric "flare wave" transients in association with a flare, large-scale coronal dimming, metric radio activity and a coronal mass ejection. The two separate eruptions occurring on 24 September 1997 originate in the same active region and display similar morphological features. The first wave transient was observed in Extreme Ultraviolet Lithography (EUV) and H alpha data, corresponding to a wave disturbance in both the chromosphere and the solar corona, ranging from 250 to approaching 1000 km/sec at different times and locations along the wavefront. The sharp wavefront had a similar extent and location in both the EUV and H alpha data. The data did not show clear evidence of a driver, however. Both events display a coronal EUV dimming which is typically used as an indicator of a coronal mass ejection in the inner corona. White light coronagraph observations indicate that the first event was accompanied by an observable coronal mass ejection while the second event did not have clear evidence of a Coronal Mass Ejection (CME). Both eruptions were accompanied by metric type II radio bursts propagating at speeds in the range of 500-750 km/sec, and neither had accompanying interplanetary type II activity. The timing and location of the flare waves appear to indicate an origin with the flaring region, but several signatures associated with coronal mass ejections indicate that the development of the CME may occur in concert with the development of the flare wave.10/1999; -
Conference Proceeding: Is the chromosphere hotter in coronal holes?
American Institute of Physics Conference Series; 06/1999 -
Article: SOHO/EIT observations of an Earth-directed coronal mass ejection on May 12, 1997
grl. 01/1998; 25:2465-2468. -
Article: White-light coronal mass ejections: A new perspective from LASCO
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ABSTRACT: More than 275 coronal mass ejections (CMEs) were recorded by the large angle spectroscopic coronagraph (LASCO) from January 1996 through August 1997. Some of the characteristics of 65 of these CMEs, occurring during a three month period (May to July 1997) were quantified. During this time the rate of CME detection was about 0.7 CMEs per day; the distribution of apparent latitudes was clustererd near the equator with an average latitude of 3 deg N; the average width of the CMEs was 49 deg; and the average speed was 324 km/s. The statistical measures and the distributions for these CMEs agree with the existing literature. One new result was the high fraction (plus or minus 35 deg) of CMEs with at least one concave-outward morphological feature, which was considered a possible signature of magnetic disconnection. A new small-scale phenomenon that appears to be the white light counterpart of the extreme ultraviolet microjets detected in the polar coronal holes is described.01/1998; -
Article: A multi-wavelength analysis of the February 6/7, 1997 coronal mass ejection
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ABSTRACT: The coronal mass ejection (CME) event on 6 to 7 February 1997 that originate from the southwest quadrant of the sun are analyzed. The CME is accelerated from a projected speed of 170 km/s to about 650 km/s at 25 solar radii. The CME is an arcade eruption followed by bright prominence core structures. The CME was accompanied by an arcade formation. The X-ray and extreme ultraviolet observations suggest that the reconnection proceeded from the northwest and the southeast end of a filament channel. The CME event caused interplanetary effects that produced a medium size geomagnetic storm on earth. Issues relating to the origin and propagation of geo-effective solar disturbances are addressed.10/1997;
