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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 27, issue 10
Ann. Geophys., 27, 3841–3851, 2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: Three eyes on the Sun – multi-spacecraft studies of...

Ann. Geophys., 27, 3841–3851, 2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

  09 Oct 2009

09 Oct 2009

Multispacecraft observations of a prominence eruption

A. Bemporad1, G. Del Zanna2, V. Andretta3, G. Poletto4, and M. Magrí3 A. Bemporad et al.
  • 1INAF – Torino Astronomical Obs., via Osservatorio 20, 10025 Pino Torinese (TO), Italy
  • 2Dept. of Applied Mathematics and Theoretical Physics, Univ. of Cambridge, Wilberforce Road, Cambridge CB3 0WA, UK
  • 3INAF – Capodimonte Astronomical Obs., salita Moiariello 16, 80131 Napoli, Italy
  • 4INAF – Arcetri Astrophysical Obs., L.go E. Fermi 5, 50125 Firenze, Italy

Abstract. On 9 May 2007 a prominence eruption occurred at the West limb. Remarkably, the event was observed by the STEREO/EUVI telescopes and by the HINODE/EIS and SOHO/UVCS spectrometers. We present results from all these instruments. High-cadence (~37 s) data from STEREO/EUVI A and B in the He II λ304 line were used to study the 3-D shape and expansion of the prominence. The high spatial resolution EUVI images (~1.5"/pixel) have been used to infer via triangulation the 3-D shape and orientation of the prominence 12 min after the eruption onset. At this time the prominence has mainly the shape of a "hook" highly inclined southward, has an average thickness of 0.068 R, a length of 0.43 R and lies, in first approximation, on a plane. Hence, the prominence is mainly a 2-D structure and there is no evidence for a twisted flux rope configuration. HINODE/EIS was scanning with the 2" slit the region where the filament erupted. The EIS spectra show during the eruption remarkable non-thermal broadening (up to ~100 km s−1) in the region crossed by the filament in spectral lines emitted at different temperatures, possibly with differences among lines from higher Fe ionization stages. The CME was also observed by the SOHO/UVCS instrument: the spectrograph slit was centered at 1.7 R, at a latitude of 5° SW and recorded a sudden increase in the O VI λλ1032–1037 and Si XII λ520 spectral line intensities, representative of the CME front transit.

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