Trajectories of Microwave Prominence Eruptions

Details Trajectories of Microwave Prominence Eruptions Trajectories of Microwave Prominence Eruptions

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..305h&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Physics

Scientific paper

We examine the trajectories of 50 prominence eruptions observed in microwave continuum emission near solar maximum (1999-2000). On the basis of Nobeyama Radioheliograph 17 GHz images, we address two major questions; i) what triggers the prominence activity, and ii) how does the prominence motion affect or reflect the surrounding coronal structures. We found that most prominence activity is related to some weak energy release (or heating) taking place in the lower corona as suggested by the increase of the brightness temperature. By combining the 17 GHz prominence images with white-light synoptic maps from the LASCO C2 coronagraph on the SOHO spacecraft, we verify that 94% of the prominence eruptions were associated with coronal mass ejections (CMEs) and that the remaining 6% show weak mass motions confined to streamers. We confirm that coronal mass motions involving prominence eruptions and CMEs are not random but are organized by bundles of streamers. The large scale evolution of coronal features within 4.5 solar radii suggests that streamers are a signature of multiple plasma sheets emanating from active region belts, arcades, trans-equatorial interconnecting loops, and polar crown filaments, through which coronal mass is transported toward interplanetary space. This implies that magnetic forces exerted by streamers (or plasma sheets) play an important role in driving transient mass motions away from the Sun, against solar gravity.

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