Abstract
Abstract. 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)
Highlights
Before halo coronal mass ejections (H-CMEs) were first observed, eruptive prominences were known to relate to major Hα-flares and to CMEs and were suspected of being directly connected to geomagnetic activity
In our search of the ejecta candidate time-interval(s) in Events 3, 4, 5, 9, 10, 12, 13, and 14, we focus on solar wind conditions downstream to the passage of the possibly driven interplanetary shock
The events presented in the analysis correspond to the near solar minimum epoch
Summary
Before halo coronal mass ejections (H-CMEs) were first observed, eruptive prominences were known to relate to major Hα-flares (see, e.g. Zirin, 1966; Martin, 1973) and to CMEs (see e.g. Munro et al, 1979) and were suspected of being directly connected to geomagnetic activity (see, e.g. Joselyn and McIntosh, 1981). We present a study, statistical in nature, of a larger set of events, with their source at the front side of the Sun, than the sets investigated in some of the resent statistical studies (Brueckner et al, 1998; Cane et al, 1998; Webb et al, 2000b) We complement those studies with a more detailed analysis of the occurrence of many hours, up to more than two days, of unusual solar wind condition. Their main signatures in chronological order from the Sun, through the inner heliosphere and the in situ solar wind observations at 1 AU are analyzed statistically in Sect.
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