 |
| Titel |
Halo-coronal mass ejections near the 23rd solar minimum: lift-off, inner heliosphere, and in situ (1 AU) signatures |
| VerfasserIn |
D. B. Berdichevsky, C. J. Farrugia, B. J. Thompson, R. P. Lepping, D. V. Reames, M. L. Kaiser, J. T. Steinberg, S. P. Plunkett, D. J. Michels |
| Medientyp |
Artikel
|
| Sprache |
Englisch
|
| ISSN |
0992-7689
|
| Digitales Dokument |
URL |
| Erschienen |
In: Annales Geophysicae ; 20, no. 7 ; Nr. 20, no. 7, S.891-916 |
| Datensatznummer |
250014419
|
| Publikation (Nr.) |
 copernicus.org/angeo-20-891-2002.pdf |
|
|
|
|
|
| Zusammenfassung |
The extreme ultraviolet (EUV)
signatures of a solar lift-off, decametric and kilometric radio burst emissions
and energetic particle (EP) inner heliospheric signatures of an interplanetary
shock, and in situ identification of its driver through solar wind observations
are discussed for 12 isolated halo coronal mass ejections (H-CMEs) occurring
between December 1996 and 1997. For the aforementioned twelve and the one event
added in the discussion, it is found that ten passed several necessary
conditions for being a "Sun-Earth connection". It is found that low
corona EUV and Ha chromospheric signatures indicate
filament eruption as the cause of H-CME. These signatures indicate that the 12
events can be divided into two major subsets, 7 related to active regions (ARs)
and 5 unrelated or related to decayed AR. In the case of events related to AR,
there is indication of a faster lift-off, while a more gradual lift-off appears
to characterize the second set. Inner heliospheric signatures – the presence
of long lasting enhanced energetic particle flux and/or kilometric type II
radio bursts – of a driven shock were identified in half of the 12 events.
The in situ (1 AU) analyses using five different solar wind ejecta signatures
and comparisons with the bidirectional flow of suprathermal particles and
Forbush decreases result in indications of a strong solar wind ejecta
signatures for 11 out of 12 cases. From the discussion of these results,
combined with work by other authors for overlapping events, we conclude that
good Sun-Earth connection candidates originate most likely from solar filament
eruptions with at least one of its extremities located closer to the central
meridian than ~ 30° E or ~ 35° W with a larger extension in latitudinal
location possible. In seven of the twelve cases it appears that the encountered
ejecta was driving a shock at 1 AU. Support for this interpretation is found on
the approximately equal velocity of the shock and the ejecta leading-edge.
These shocks were weak to moderate in strength, and a comparison of their
transit time with their local speed indicated a deceleration. In
contradistinction with this result on shocks, the transit time versus the local
speed of the ejecta appeared either to indicate that the ejecta as a whole
traveled at constant speed or underwent a small amount of acceleration. This is
a result that stands for cases with and without fast stream observations at
their rear end. Seven out of twelve ejecta candidate intervals were themselves
interplanetary magnetic cloud (IMC) or contained a previously identified IMC.
As a by-product of this study, we noticed two good ejecta candidates at 1 AU
for which observation of a H-CME or CME appears to be missing.
Key words. Radio science (remote sensing); Solar
physics, astrophysics and astronomy (flares and mass ejections); Space plasma
physics (nonlinear phenomena) |
| |
|
| Teil von |
|
|
|
|
|
|
|
|