Simulating Solar Coronal Mass Ejections constrained by Observations of their Speed and Poloidal flux. (arXiv:1904.00140v1 [astro-ph.SR])

Simulating Solar Coronal Mass Ejections constrained by Observations of their Speed and Poloidal flux. (arXiv:1904.00140v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Singh_T/0/1/0/all/0/1">Talwinder Singh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yalim_M/0/1/0/all/0/1">Mehmet Sarp Yalim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pogorelov_N/0/1/0/all/0/1">Nikolai Pogorelov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gopalswamy_N/0/1/0/all/0/1">Nat Gopalswamy</a>

We demonstrate how the parameters of a Gibson-Low flux-rope-based coronal
mass ejection (CME) can be constrained using remote observations. Our Multi
Scale Fluid-Kinetic Simulation Suite (MS-FLUKSS) has been used to simulate the
propagation of a CME in a data driven solar corona background computed using
the photospheric magnetogram data. We constrain the CME model parameters using
the observations of such key CME properties as its speed, orientation, and
poloidal flux. The speed and orientation are estimated using multi-viewpoint
white-light coronagraph images. The reconnected magnetic flux in the area
covered by the post eruption arcade is used to estimate the poloidal flux in
the CME flux rope. We simulate the partial halo CME on 7 March 2011 to
demonstrate the efficiency of our approach. This CME erupted with the speed of
812 km/s and its poloidal flux, as estimated from source active region data,
was 4.9e21 Mx. Using our approach, we were able to simulate this CME with the
speed 840 km/s and the poloidal flux of 5.1e21 Mx, in remarkable agreement with
the observations.

We demonstrate how the parameters of a Gibson-Low flux-rope-based coronal
mass ejection (CME) can be constrained using remote observations. Our Multi
Scale Fluid-Kinetic Simulation Suite (MS-FLUKSS) has been used to simulate the
propagation of a CME in a data driven solar corona background computed using
the photospheric magnetogram data. We constrain the CME model parameters using
the observations of such key CME properties as its speed, orientation, and
poloidal flux. The speed and orientation are estimated using multi-viewpoint
white-light coronagraph images. The reconnected magnetic flux in the area
covered by the post eruption arcade is used to estimate the poloidal flux in
the CME flux rope. We simulate the partial halo CME on 7 March 2011 to
demonstrate the efficiency of our approach. This CME erupted with the speed of
812 km/s and its poloidal flux, as estimated from source active region data,
was 4.9e21 Mx. Using our approach, we were able to simulate this CME with the
speed 840 km/s and the poloidal flux of 5.1e21 Mx, in remarkable agreement with
the observations.

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