Multi-wavelength Structure of an Active Region Filament

Details Multi-wavelength Structure of an Active Region Filament Multi-wavelength Structure of an Active Region Filament

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh52a0469b&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH52A-0469

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7507 Chromosphere, 7509 Corona, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

In this work we will compare the structure of active region filaments near a sunspot, in a number of wavelengths. The data were obtained from three sources on June 20, 2001 between 14:00 and 16:00 NSO/SP, photospheric and chromospheric observations of intensities (G-Band), and spectroscopy (Hα, MgI 5172 Å, and CaI 6122 Å) to determine velocities, and magnetic fields; TRACE observations at 1600Å continuum, and coronal measurements in 171 Å; SOHO/EIT coronal observations in Fe XII 195A, SOHO/CDS spectroscopic observations in spectral lines -- SiXII 520.66 Å, OIV 554.52 Å, NeVI 562.80 Å, HeI 584.33 Å, OIII 599.59 Å, HeII 303.78 Å, MgIX 368.07 Å, MgX 624.94 Å, OV 629.73 Å, SiXII 520.66 Å, OIV 554.52 Å, NeVI 562.80 Å, HeI 584.33 Å, OIII 599.59 Å, HeII 303.78 Å, MgIX 368.07 Å, MgX 624.94 Å, OV 629.73 Å; and SOHO/MDI magnetic and intensity images. The common FOV covers about 100 arcseconds. We will present the evolutionary nature of the photospheric magnetic field, the the corresponding chromospheric velocities and the coronal variations of this filament region. During the initial period of the observations, this active region filament system is disrupted by an adjoining solar flare. The structure and dynamics of the filament system during this eruption will be traced.

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