A STUDY OF THE BUILD-UP, INITIATION, AND ACCELERATION OF 2008 APRIL 26 CORONAL MASS EJECTION OBSERVED BY STEREO

Journal Article · Thu Apr 01 00:00:00 EDT 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/712/2/1302· OSTI ID:21394182

Cheng, X; Ding, M D; Zhang, J ^[1]

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1. Department of Astronomy, Nanjing University, Nanjing 210093 (China)

In this paper, we analyze the full evolution, from a few days prior to the eruption to the initiation, final acceleration, and propagation, of the coronal mass ejection (CME) that occurred on 2008 April 26 using the unprecedented high cadence and multi-wavelength observations by the Solar Terrestrial Relations Observatory. There existed frequent filament activities and EUV jets prior to the CME eruption for a few days. These activities were probably caused by the magnetic reconnection in the lower atmosphere driven by photospheric convergence motions, which were evident in the sequence of magnetogram images from the Michelson Doppler Imager on board the Solar and Heliospheric Observatory. The slow low-layer magnetic reconnection may be responsible for the storage of magnetic free energy in the corona and the formation of a sigmoidal core field or a flux rope leading to the eventual eruption. The occurrence of EUV brightenings in the sigmoidal core field prior to the rise of the flux rope implies that the eruption was triggered by the inner tether-cutting reconnection, but not the external breakout reconnection. During the period of impulsive acceleration, the time profile of the CME acceleration in the inner corona is found to be consistent with the time profile of the reconnection electric field inferred from the footpoint separation and the Reuven Ramaty High Energy Solar Spectroscopic Imager 15-25 keV hard X-ray flux curve of the associated flare. The full evolution of this CME can be described in four distinct phases: the build-up phase, initiation phase, main acceleration phase, and propagation phase. The physical properties and the transition between these phases are discussed, in an attempt to provide a global picture of CME dynamic evolution.

• OSTI ID: 21394182
• Journal Information: Astrophysical Journal, Vol. 712, Issue 2; Other Information: DOI: 10.1088/0004-637X/712/2/1302; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ACCELERATION
ELECTRIC FIELDS
ERUPTION
FREE ENERGY
HARD X RADIATION
KEV RANGE 10-100
MAGNETIC RECONNECTION
MASS
SOLAR CORONA
SOLAR FLARES
SOLAR SYSTEM EVOLUTION
SUN
ATMOSPHERES
ELECTROMAGNETIC RADIATION
ENERGY
ENERGY RANGE
EVOLUTION
IONIZING RADIATIONS
KEV RANGE
MAIN SEQUENCE STARS
PHYSICAL PROPERTIES
RADIATIONS
SOLAR ACTIVITY
SOLAR ATMOSPHERE
STARS
STELLAR ACTIVITY
STELLAR ATMOSPHERES
STELLAR CORONAE
STELLAR FLARES
THERMODYNAMIC PROPERTIES
X RADIATION