Abstracts > Abstract list by author > Sanjay Gusain

Gusain Sanjay  1@  , Brigitte Schmieder  2@  , Guy Artzner  3@  , Sergey Bogachev  4@  , Tibor Torok  5@  
1 : National Solar Observatory  (NSO, Tucson, AZ, USA)
950 N. Cherry Avenue, Tucson 85719, AZ, USA -  United States
2 : Laboratoire d'études spatiales et d'instrumentation en astrophysique  (LESIA)  -  Website
Université Pierre et Marie Curie - Paris VI, Observatoire de Paris, INSU, CNRS : UMR8109, Université Paris Diderot - Paris 7
5, place Jules Janssen 92190 MEUDON -  France
3 : Institut d'astrophysique spatiale  (IAS)  -  Website
CNRS : UMR8617, INSU, Université Paris Sud - Paris XI
bat. 121 91405 ORSAY CEDEX -  France
4 : Lebedev Physical Institute of Russian Academy of Sciences
Lebedev Physical Institute of Russian Academy of Science, Leninskij prospekt 53, Moscow 119991, Russia -  Russia
5 : Predictive Science Inc.  (PSI)
Predictive Science, Inc., 9990 Mesa Rim Rd., Suite 170, San Diego, CA 92121, USA -  United States

We analyze multi-spacecraft observations of a giant filament eruption
that occurred during 26 and
27 September 2009. The filament eruption was associated with a
relatively slow coronal mass ejection
(CME). The filament consisted of a large and a small part, both parts
erupted nearly simultaneously.
Here we focus on the eruption associated with the larger part of the
filament. The STEREO
satellites were separated by about 117 degree during this event, so we
additionally used SoHO/EIT and
CORONAS/TESIS observations as a third eye (Earth view) to aid our
measurements. We measure
the plane-of-sky trajectory of the filament as seen from STEREO-A and
TESIS view-points. Using
a simple trigonometric relation, we then use these measurements to
estimate the true direction
of propagation of the filament which allows us to derive the true
R=R⊙-time profile of the filament
apex. Furthermore, we develop a new tomographic method that can
potentially provide a more robust
three-dimensional reconstruction by exploiting multiple simultaneous
views. We apply this method
also to investigate the 3D evolution of the top part of filament. We
expect this method to be useful
when SDO and STEREO observations are combined. We then analyze the
kinematics of the eruptive
filament during its rapid acceleration phase by fitting different
functional forms to the height-time
data derived from the two methods. We find that, for both methods, an
exponential function fits the
rise profile of the filament slightly better than parabolic or cubic
functions. Finally, we confront these
results with the predictions of theoretical eruption models.

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