SOHO 20

1
Coronal Waves Magnetic Footprints
ofLarge-Scale CMEs?
Gemma Attrill1, Louise Harra1, Lidia van
Driel-Gesztelyi1,2,3 and Pascal
Démoulin2 1University College London, Mullard
Space Science Laboratory, UK. 2Observatoire de
Paris, Meudon, France. 3Konkoly Observatory,
Budapest, Hungary.
2
Are there 2 types of EIT coronal waves?
Thompson et al. 2000 Sept 24th 1997
Sometimes co-spatial with a Moreton wave
Podladchikova Berghmans (2005) May 12th 1997
S H A R P
S-waves - Biesecker et al. 2002
High velocity gt 250 km/s
Khan Aurass 2002 Nov 3rd 1997
Restricted angle of propagation
D I F F U S E
Semi-isotropic
Controversial result
ROTATING!
Thompson et al. 1998 May 12th 1997
Thompson et al. 1999 April 7th 1997
3
Analysis Expansion of coronal bright fronts
Observer
Bright fronts appear to be generated in the low
corona
4
Intensity around bright front
12th May 1997 event
7th April 1997 event
5
Standard Model (Sturrock, 1966 Shibata et al.
1995)
Leamon, Canfield Pevtsov (2002)