Astronomy and Astrophysics – Astronomy
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.9807l&link_type=abstract
American Astronomical Society Meeting 204, #98.07; Bulletin of the American Astronomical Society, Vol. 36, p.985
Astronomy and Astrophysics
Astronomy
Scientific paper
A critical problem for understanding the solar corona has been to measure its magnetic field that we believe determines its structure and dynamics from the upper chromosphere out into the heliospheric environment. The direct measurement of this field has been a longstanding problem. Only recently have Zeeman splitting observations of infrared coronal emission lines (Lin et al. 2000) been used to deduce the coronal magnetic flux density. We have extended this technique and report here our first results from a novel coronal magnetometer that uses an off-axis reflecting coronagraph (SOLARC) and optical fiber-bundle imaging spectropolarimeter (OFIS). Our results reveal the line-of-sight magnetic flux density with a sensitivity of a few gauss with 20 arcsec spatial resolution and approximately 60min temporal resolution. These full Stokes spectropolarimetric data of the forbidden FeXIII emission line at 1075nm imply a line-of-sight coronal magnetic field above an active region with a flux density of 9G. Although these first results from SOLARC/OFIS have relatively coarse resolution, they have potential for solving our coronal "dark energy" problem with infrared magnetometry. This research has been supported by the Multidisciplinary University Research Initiative (MURI) of the DOD, NASA, and the National Science Foundation Atmospheric Research Program.
Coulter Roy
Kuhn Jeff R.
Lin Hainan
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