Solar Source and Heliospheric Consequences of the 2010 April 3 Coronal Mass Ejection: A Comprehensive View

Details Solar Source and Heliospheric Consequences of the 2010 April 3 Coronal Mass Ejection: A Comprehensive View Solar Source and Heliospheric Consequences of the 2010 April 3 Coronal Mass Ejection: A Comprehensive View

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...734...84l&link_type=abstract

The Astrophysical Journal, Volume 734, Issue 2, article id. 84 (2011).

Astronomy and Astrophysics

Astronomy

6

Shock Waves, Solar-Terrestrial Relations, Solar Wind, Sun: Coronal Mass Ejections: Cmes, Sun: Particle Emission, Sun: Radio Radiation

Scientific paper

We study the solar source and heliospheric consequences of the 2010 April 3 coronal mass ejection (CME) in the frame of the Sun-Earth connection using observations from a fleet of spacecraft. The CME is accompanied by a B7.4 long-duration flare, dramatic coronal dimming, and EUV waves. It causes significant heliospheric consequences and space weather effects such as radio bursts, a prominent shock wave, the largest/fastest interplanetary CME at 1 AU since the 2006 December 13 CME, the first gradual solar energetic particle (SEP) events in solar cycle 24, and a prolonged geomagnetic storm resulting in a breakdown of the Galaxy 15 satellite. This event, together with several following periods of intense solar activities, indicates awakening of the Sun from a long minimum. The CME EUV loop begins to rise at least 10 minutes before the flare impulsive phase. The associated coronal wave forms an envelope around the CME, a large-scale three-dimensional structure that can only be explained by a pressure wave. The CME and its preceding shock are imaged by both STEREO A and B almost throughout the whole Sun-Earth space. CME kinematics in the ecliptic plane are obtained as a function of distance out to 0.75 AU by a geometric triangulation technique. The CME has a propagation direction near the Sun-Earth line and a speed that first increases to 1000-1100 km s-1 and then decreases to about 800 km s-1. Both the predicted arrival time and speed at the Earth are well confirmed by the in situ measurements. The gradual SEP events observed by three widely separated spacecraft show time profiles much more complicated than suggested by the standard conceptual picture of SEP event heliolongitude distribution. Evolving shock properties, the realistic time-dependent connection between the observer and shock source, and a possible role of particle perpendicular diffusion may be needed to interpret this SEP event spatial distribution.

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