Observations and Nonlinear Force-Free Field Modeling of Active Region 10953

Details Observations and Nonlinear Force-Free Field Modeling of Active Region 10953 Observations and Nonlinear Force-Free Field Modeling of Active Region 10953

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...691..105s&link_type=abstract

The Astrophysical Journal, Volume 691, Issue 1, pp. 105-114 (2009).

Astronomy and Astrophysics

Astronomy

20

Sun: Corona, Sun: Filaments, Sun: Flares, Sun: Magnetic Fields, Sun: Photosphere, Sun: X-Rays, Gamma Rays

Scientific paper

We present multiwavelength observations of a simple bipolar active region (NOAA 10953), which produced several small flares (mostly B class and one C8.5 class) and filament activations from April 30 to May 3 in 2007. We also explore nonlinear force-free field (NLFFF) modeling of this region prior to the C8.5 flare on May 2, using magnetograph data from SOHO/MDI and Hinode/SOT. A series of NLFFF models are constructed using the flux-rope insertion method. By comparing the modeled field lines with multiple X-ray loops observed by Hinode/XRT, we find that the axial flux of the flux rope in the best-fit models is (7± 2)× 1020 Mx, while the poloidal flux has a wider range of (0.1-10)× 1010 Mx cm-1. The axial flux in the best-fit model is well below the upper limit (~15× 1020 Mx) for stable force-free configurations, which is consistent with the fact that no successful full filament eruption occurred in this active region. From multiwavelength observations of the C8.5 flare, we find that the X-ray brightenings (in both RHESSI and XRT) appeared about 20 minutes earlier than the EUV brightenings seen in TRACE 171 Å images and filament activations seen in MLSO Hα images. This is interpreted as an indication that the X-ray emission may be caused by direct coronal heating due to reconnection, and the energy transported down to the chromosphere may be too low to produce EUV brightenings. This flare started from nearly unsheared flare loop, unlike most two-ribbon flares that begin with highly sheared footpoint brightenings. By comparing with our NLFFF model, we find that the early flare loop is located above the flux rope that has a sharp boundary. We suggest that this flare started near the outer edge of the flux rope, not at the inner side or at the bottom as in the standard two-ribbon flare model.

Affiliated with

Also associated with

No associations

Rating

Observations and Nonlinear Force-Free Field Modeling of Active Region 10953 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Observations and Nonlinear Force-Free Field Modeling of Active Region 10953, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Observations and Nonlinear Force-Free Field Modeling of Active Region 10953 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1782889