Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.2104v&link_type=abstract
American Astronomical Society, SPD meeting #40, #21.04; Bulletin of the American Astronomical Society, Vol. 41, p.855
Astronomy and Astrophysics
Astronomy
Scientific paper
The availability of high quality synoptic observations of the EUV and visible corona during the SOHO mission has advanced our understanding of the low corona manifestations of CMEs. The EUV imager/White light coronagraph connection has been proven so powerful, it is routinely assumed that if no EUV signatures are present when a CME is observed by a coronagraph, then the event must originate behind the visible limb. This assumption carries strong implications for space weather forecasting but has not been put to the test. This paper presents the first detailed analysis of a frontside, large-scale CME that has no obvious counterparts in the low corona. The event was observed by the SECCHI instruments on the STEREO mission. The COR2A coronagraph observed the event as a typical flux-rope type CME, while an extremely faint partial halo was observed in COR2B. The event evolved very slowly and is typical of the streamer-blowout CME class. EUVI-A 171A images show a concave feature above the east limb, relatively stable for about two days before the eruption, when it rises into the coronagraphic fields and develops into the core of the CME. None of the typical low corona signatures of a CME (flaring, EUV dimming, filament eruption, waves) were observed. Thanks to the two STEREO viewpoints we were able to identify the likely source region. The event originated along a quiet sun neutral line. No active regions were present anywhere on the visible face of the disk. Leaving no trace behind, this observation shows unambiguously that a CME eruption does not need to have clear on-disk signatures. Also it sheds light on the question of `mystery' geomagnetic storms; storms without clear solar origin. Preliminary inspection of STEREO data indicates that events like this are not uncommon, particularly during the ongoing period of deep solar minimum.
Patsourakos Spiros
Robbrecht Eva
Vourlidas Angelos
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