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Title:
Relation Between Type II Bursts and CMEs Inferred from STEREO Observations [ Erratum: 2012SoPh..277..459G ]
Authors:
Gopalswamy, N.; Thompson, W. T.; Davila, J. M.; Kaiser, M. L.; Yashiro, S.; Mäkelä, P.; Michalek, G.; Bougeret, J.-L.; Howard, R. A.
Affiliation:
AA(NASA Goddard Space Flight Center), AB(NASA Goddard Space Flight Center), AC(NASA Goddard Space Flight Center), AD(NASA Goddard Space Flight Center), AE(Interferometrics), AF(The Catholic University of America), AG(The Catholic University of America), AH(Paris Observatory), AI(Naval Research Laboratory)
Publication:
Solar Physics, Volume 259, Issue 1-2, pp. 227-254 (SoPh Homepage)
Publication Date:
10/2009
Origin:
SPRINGER
Keywords:
Coronal mass ejections, Type II radio bursts, Shocks, Flares, Dynamic spectrum
DOI:
10.1007/s11207-009-9382-1
Bibliographic Code:
2009SoPh..259..227G

Abstract

The inner coronagraph (COR1) of the Solar Terrestrial Relations Observatory (STEREO) mission has made it possible to observe CMEs in the spatial domain overlapping with that of the metric type II radio bursts. The type II bursts were associated with generally weak flares (mostly B and C class soft X-ray flares), but the CMEs were quite energetic. Using CME data for a set of type II bursts during the declining phase of solar cycle 23, we determine the CME height when the type II bursts start, thus giving an estimate of the heliocentric distance at which CME-driven shocks form. This distance has been determined to be ˜1.5 R s (solar radii), which coincides with the distance at which the Alfvén speed profile has a minimum value. We also use type II radio observations from STEREO/WAVES and Wind/WAVES observations to show that CMEs with moderate speed drive either weak shocks or no shock at all when they attain a height where the Alfvén speed peaks (˜3 R s - 4 R s). Thus the shocks seem to be most efficient in accelerating electrons in the heliocentric distance range of 1.5 R s to 4 R s. By combining the radial variation of the CME speed in the inner corona (CME speed increase) and interplanetary medium (speed decrease) we were able to correctly account for the deviations from the universal drift-rate spectrum of type II bursts, thus confirming the close physical connection between type II bursts and CMEs. The average height (˜1.5 R s) of STEREO CMEs at the time of type II bursts is smaller than that (2.2 R s) obtained for SOHO ( Solar and Heliospheric Observatory) CMEs. We suggest that this may indicate, at least partly, the density reduction in the corona between the maximum and declining phases, so a given plasma level occurs closer to the Sun in the latter phase. In two cases, there was a diffuse shock-like feature ahead of the main body of the CME, indicating a standoff distance of 1 R s - 2 R s by the time the CME left the LASCO field of view.

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