Heliospheric Computations. Dusan Odstrcil University of Colorado/CIRES and NOAA/Space Environment Center. Solar MURI Team Meeting, Berkeley CA, December 5, 2002. Outline. Programming Activities Merging of Coronal and Heliospheric Models - requirements for coupled simulations
University ofColorado/CIRES and NOAA/Space Environment Center
Solar MURI Team Meeting, Berkeley CA, December 5, 2002
SDSC, San Diego, CA NCAR/SCD, Boulder, CO
Solar eruption evolves into a traveling disturbance of interplanetary magnetic field that significantly exceeds its original angular size
Flux rope (white lines) is initially connected to the Sun, but magnetic field lines reconfigure during its propagation. Color shows density in the equatorial plane. Black circle is boundary between the coronal and heliospheric regions (30 Rs).
N, T, and Bphi in the equatorial plane and model interface seen from below. (Computations are not performed for +-30 deg from the poles). Magnetic field is traced back to Sun.
The same but 20 hours later. Magnetic field lines (tracing starts from the heliosphere) does not reach the Sun; they reconfigure in the coronal region.