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Tracking a Ulysses high-latitude ICME event back to its solar origins  

Cristiana Dumitrache   Submitted: 2011-08-30 07:12

This abstract was corrupted following database problems and is being recovered. It will be restored as quickly as possible. Any questions, please send them to Alisdair. Sorry for any incovenience.


Authors: Dumitrache,C; Popescu, N.A.; Oncica, A.
Projects: SoHO-LASCO

Publication Status: Solar Physics 272, 137-157, DOI: 10.1007/s11207-011-9811-9, 2011
Last Modified: 2011-08-30 10:49
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An CME-ICME couple analysis  

Cristiana Dumitrache   Submitted: 2010-12-10 05:06

We analyze the interplanetary mass ejection event registered by Ulysses on 5 May 2002. We compute the track back to the Sun of this event using a linear model. The solar source of this event is a coronal mass ejection occurred from a small polar filament. This filament was registered on 23 and 24 April2002. This CME-ICME has a slow down from 576 km s-1 to about 400 km s-1 in 3.36 astronomical unities (distance from Sun to Ulysses spacecraft). This event displays all ICME characteristics and a magnetic cloud with significant rotation of magnetic field.

Authors: C.Dumitrache, N.A.Popescu
Projects: None

Publication Status: The 3rd Hinode Science Meeting, Tokyo, Japonia, ASP Conference Series, submitted
Last Modified: 2010-12-10 10:15
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On twist estimation in active regions  

Cristiana Dumitrache   Submitted: 2010-12-10 05:03

Our work had two objectives. First, we have extrapolated the 3D coronal magnetic field lines from MDI magnetograms for three active regions, in two different days for each one, and compared with coronal images from XRT/Hinode or EIT/SOHO. Additionally,we computed the force-free field parameter to estimate the twist in these active regions where more explosive events occurred.

Authors: C.Dumitrache, L.Dumitru, V.Banciu
Projects: None

Publication Status: The 3rd Hinode Science Meeting, Tokyo, Japonia, ASP Conference Series, submitted
Last Modified: 2010-12-10 10:15
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Polar flaring filament  

Cristiana Dumitrache   Submitted: 2010-12-10 04:56

A special, huge polar filament producing multiple CMEs is analyzed. Around this double-S shaped filament a two-ribbon flare occurred which rose into a CME.

Authors: C.Dumitrache
Projects: None

Publication Status: Astrophysics and Space Science Proceedings, eds. S. S. Hasan , R. Rutten, 459-463, 2010
Last Modified: 2010-12-10 10:15
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Kink Instabilities Triggering a Filament Eruption  

Cristiana Dumitrache   Submitted: 2010-12-10 04:46

A huge complex filament was observed between 28 December 2000 and 7 January 2001. We have analyzed its dynamics and its sudden disappearance. We analyze the 3-D coronal magnetic field extrapolated from MDI photospheric magnetograms and compare with filament coronal images. The filament erupted in a CME after a mild helical up-awarded movement of plasma on 7 January. We attempt to explain this CME event onset by kink instabilities. An approach to estimate the filament helicity and magnetic flux injection explain the filament destabilization.

Authors: C.Dumitrache, D.Constantin
Projects: None

Publication Status: RoAJ 20, 35-44, 2010
Last Modified: 2010-12-10 10:16
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A Case Of Filament - Active Region Interaction  

Cristiana Dumitrache   Submitted: 2010-12-10 04:43

We analyze a huge filament observed between 5 and 19 September 2001. During its evolution it is linked to the active region 9612, observed between 7 and 16 September 2001. The filament has a strange morphology and dynamics: starting as two parallel components (A and B), it becomes a double sigmoid filament when a third component (C ) appears linking the other two. An unusual magnetic topology characterizes this evolution: the active region is located between the parallel components. When the third component becomes observable, it links these ones first below the active region. After a spectacular plasma movement registered in filament (A), this one becomes linked to (B) above the active region. In spite of these dramatically changes of the magnetic topology and filament { active region switch, no CME is observed. Only a few flares occurring in AR9612 are registered and these ones can be seen in the dynamics of the filament as an expression of large scale magnetic reconnections.

Authors: C.Dumitrache, L.Dumitru
Projects: None

Publication Status: Publication of the Astronomical Observatory of Belgrade, 90, 125-130, 2010
Last Modified: 2010-12-10 10:16
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Subject will be restored when possible  

Cristiana Dumitrache   Submitted: 2007-12-15 15:10

A study of filaments observed during 1957?1989 reveals that the differential rotation velocity changes within the solar cycle. We propose that these variations are the manifestation of the torsional oscillations of the coronal magnetic field.

Authors: C.Dumitrache
Projects: None

Publication Status: Rom. Astron. J., Vol. 14, No. 2, p. 147?155, 2004
Last Modified: 2007-12-15 21:56
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Cristiana Dumitrache   Submitted: 2007-12-15 15:04

Coronal streamers are very interesting, long lived, features of solar corona. They are linked to prominences, CMEs and also to slow solar wind. The have different shape and behavior. We present a numerical simulation of a coronal streamer computed on five solar radii. Vertical motions in the streamer, both ascending and descending, are revealed during the streamer evolution, as well as eddy flows.

Authors: C.Dumitrache
Projects: None

Publication Status: AIP Conference Proceedings 934, 129-138, 2007
Last Modified: 2007-12-15 22:02
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Cristiana Dumitrache   Submitted: 2007-12-15 15:01

A complex filament composed by a main body(a huge polar filament), and a tail (a small filament situated between active regions) was observed between 6 and 14 January 2001. We have analyzed its dynamics. The tail suffered a thermal sudden disappearance and reappeared after two days. A decaying active region plays the role of attractor for the complex filament. A spectacular CME, produced after a helical up-awarded movement of plasma, movement observed in the coronal loops of the main body of the filament during three days before the CME onset. We have analyzed also the CME shape and movement using SOHO data.

Authors: D.R. Constantin, M. Mierla, C. Oprea and C. Dumitrache
Projects: None

Publication Status: AIP Conference Proceedings 934, 78-85, 2007
Last Modified: 2007-12-15 22:02
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Cristiana Dumitrache   Submitted: 2007-12-15 14:58

A huge filament was observed at Bucharest Observatory between 3 and 10 October 2001. We analyze this feature using our own observations and those from other observatories.

Authors: C. Dumitrache, C. Oprea, D. Constantin, M. Mierla, A.S. Popescu
Projects: None

Publication Status: AIP Conference Proceedings 895, 69-75, 2007
Last Modified: 2007-12-15 22:02
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Cristiana Dumitrache   Submitted: 2007-12-15 14:54

A numerical experiment shows the possibility of a coronal streamer to form after an eruptive process, e.g. after one or more CMEs ?en raffale?. This situation is sustained by some observations existing in the literature.

Authors: Cristiana Dumitrache
Projects: None

Publication Status: ASP Serie, 370, 180, 2007
Last Modified: 2007-12-15 22:02
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Abstracts by Author
Tracking a Ulysses high-latitude ICME event back to its solar origins
An CME-ICME couple analysis
On twist estimation in active regions
Polar flaring filament
Kink Instabilities Triggering a Filament Eruption
A Case Of Filament - Active Region Interaction
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Subject will be restored when possible
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