Observations of coronal mass ejections near the sun
The appearance and properties of coronal mass ejections (CMEs) near the sun provide clues for their subsequent development in interplanetary space. Observational results are now available for which most, but not all, of a solar cycle. The statistics concerning angular sizes, latitudes, and occurrence rates were compiled, but significant differences between the Skylab/SMM and SOlwind results remain. The structure of classic loop-like CMEs consists of three parts: the bright loop, a dark void, and a bright core, which correspond to coronal loop, prominence cavity, and prominence, respectively. In a few instances the late stages of CMEs have been interpreted as disconnection events with a pinching off of the magnetic field lines and the formation of a closed structure which moves into the interplanetary. Several lines of evidence now show that CMEs have a significant three-dimensional structure rather than something close to a planar shape. While the sources of cool material in CMEs are readily identified with the erupting prominences, the solar sources of hot material observed in the driver gas to interplanetary shocks are not so obvious. The leading edges of CMEs are frequently preceded by waves or shocks which produce deflections in coronal streamers. The relationship between CMEs and type II burst shocks is unclear, however, since some fast CMEs do not result in type II bursts and some type II bursts are not associated with CMEs.
- Research Organization:
- Emmanuel Coll., Boston, MA (USA). Physics Research Div.
- OSTI ID:
- 5726909
- Report Number(s):
- AD-A-207956/4/XAB; SCIENTIFIC-3
- Country of Publication:
- United States
- Language:
- English
Similar Records
Energetic interplanetary shocks, radio emission, and coronal mass ejections
THE POSSIBLE ROLE OF CORONAL STREAMERS AS MAGNETICALLY CLOSED STRUCTURES IN SHOCK-INDUCED ENERGETIC ELECTRONS AND METRIC TYPE II RADIO BURSTS
Related Subjects
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
BRIGHTNESS
COOLING
ELECTROMAGNETIC RADIATION
INTERPLANETARY SPACE
MAGNETIC FIELDS
MAIN SEQUENCE STARS
MASS TRANSFER
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
RADIATIONS
RADIOWAVE RADIATION
SATELLITES
SHAPE
SKYLAB
SOLAR ACTIVITY
SOLAR CORONA
SOLAR CYCLE
SOLAR RADIO BURSTS
SPACE
STARS
STELLAR ATMOSPHERES
STELLAR CORONAE
SUN