Combined Analysis of Ultraviolet and Radio Observations of the 7 May 2004 CME/Shock Event

Details Combined Analysis of Ultraviolet and Radio Observations of the 7 May 2004 CME/Shock Event Combined Analysis of Ultraviolet and Radio Observations of the 7 May 2004 CME/Shock Event

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011soph..273..511m&link_type=abstract

Solar Physics, Volume 273, Issue 2, pp.511-523

Physics

1

Sun: Radio Radiation, Sun: Coronal Mass Ejections (Cmes), Shock Waves, Line: Profiles

Scientific paper

We report results from the combined analysis of UV and radio observations of a CME-driven shock observed on 7 May 2004 above the southeast limb of the Sun at 1.86 R &sun; with the Ultraviolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric Observatory (SOHO). The coronal mass ejection (CME) was first detected in white-light by the SOHO's Large Angle and Spectrometric Coronagraph (LASCO) C2 telescope and shock-associated type II metric emission was recorded simultaneously by ground-based radio spectrographs. The shock speed (˜ 690 km s-1), as deduced from the analysis of the type II emission drift in the radio spectra and the pre-shock local electron density estimated with the diagnostics provided by UVCS observations of the O vi λλ 1031.9, 1037.6 doublet line intensities, is just a factor ˜ 0.1 higher than the CME speed inferred by means of the white-light (and EUV) data in the middle corona. The local magnetosonic speed, computed from a standard magnetic field model, was estimated as high as ˜ 600 km s-1, implying that the CME speed was probably just sufficient to drive a weak fast-mode MHD shock ahead of the front. Simultaneously with the type II radio emission, significant changes in the O vi doublet line intensities and profiles were recorded in the UVCS spectra and found compatible with abrupt post-shock plasma acceleration and modest ion heating. This work provides further evidence for the CME-driven origin of the shocks observed in the middle corona.

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