The 2001 June 21 Eclipse Polarimetric Observations of the Fe XIII 1074.7 nm Emission Line

Details The 2001 June 21 Eclipse Polarimetric Observations of the Fe XIII 1074.7 nm Emission Line The 2001 June 21 Eclipse Polarimetric Observations of the Fe XIII 1074.7 nm Emission Line

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.0409h&link_type=abstract

American Astronomical Society, SPD meeting #34, #04.09; Bulletin of the American Astronomical Society, Vol. 35, p.812

Astronomy and Astrophysics

Astronomy

Scientific paper

Polarimetric measurements of the coronal forbidden lines have been recognized for quite some time as a diagnostic tool for inferring the direction of the coronal magnetic field. Following the first successful measurements by Eddy et al. (1973) during the total solar eclipse of 1966, an observing campaign using the coronagraph at Sacramento Peak Observatory was pursued between 1977-1980 (Arnaud and Newkirk, 1987). All these measurements yielded the surprising result that the direction of polarization implied a predominantly radial coronal magnetic field. We report on the polarization measurements of the Fe XIII 1074.7nm line, the strongest of the coronal forbidden lines, which were obtained during the total solar eclipse of 2001 June 21 from Zambia. In addition to confirming the earlier results of a predominantly radial field, the signature of nano-size interplanetary dust in the inner corona, most likely in the form of silicon nanoparticles, appeared for the first time in these measurements. The signature of these particles also coincides with the radial expansion of coronal holes outwards from the Sun, a signature that has never appeared in any measurement before.
Support for this work was provided by NSF grant ATM-0003661 and NASA grant NAG5-10873

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