34th Solar Physics Division Meeting, June 2003
Session 4 Corona II
Poster, Monday, June 16, 2003, 3:30-5:00pm, Mezzanine

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[4.13] A Model for Prominence Formation

B. T. Welsch (SSL, UC-Berkeley, and NRL-DC), C. R. DeVore (Laboratory for Computational Physics & Fluid Dynamics, NRL-DC), S. K. Antiochos, M.G. Linton (Solar Terrestrial Relationships Branch, Space Sciences Division, NRL-DC)

The essential features of a model prominence configuration include: dipped or helical field lines that are capable of supporting mass against gravity; sheared field lines that run nearly parallel to the photospheric polarity inversion line (PIL); and overlying field lines that restrain the sheared field lines.

To determine how reconnection might generate such field configurations, we have used the ARMS code, an MHD solver with adaptive refinement, to model the interaction of two active regions subjected to a shear flow, meant to approximate differential rotation.

We present preliminary results from two cases, one in which the model active region fields were potential prior to shearing, and one in which the active region fields were ``spun up'' prior to shearing, to approximate active region fields possessing twist at their emergence.

This work was supported in part by NASA, DoD's HPCMP, and AFOSR's Solar-MURI program.

The author(s) of this abstract have provided an email address for comments about the abstract: welsch@ssl.berkeley.edu

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© 2003. The American Astronomical Soceity.