Solar Magnetograms at 12 μm Using the Celeste Spectrograph |
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| Authors: | Thomas G Moran Donald E Jennings L Drake Deming George H McCabe Pedro V Sada Robert J Boyle |
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| Institution: | (1) Department of Physics, The Catholic University of America, Washington, DC 20064, USA;(2) NASA’s Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA;(3) CMA Consulting Services, 700 Troy-Schenectady Road, Latham, NY 12110, USA;(4) Departamento de Fisica y Matematicas, Universidad de Monterrey, Av. I. Morones Prieto 4500 Pte., Garza Garcia, LL, 66238, Mexico;(5) Department of Physics and Astronomy, Dickinson College, P.O. Box 1773, Carlisle, PA 17013, USA |
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| Abstract: | We present the first solar vector magnetogram constructed from measurements of infra-red Mg I 12.32-μm line spectra. Observations
were made at the McMath-Pierce Telescope using the Celeste spectrometer/polarimeter. Zeeman-split Stokes line spectra were
fitted with Seares profiles to obtain the magnetic field parameters. Maps of absolute field strength, line-of-sight angle,
and azimuth are presented. Analysis shows that the variation in field strength within a spatial resolution element, 2 arcseconds,
is greatest in the sunspot penumbra and that this is most likely caused by vertical field strength gradients, rather than
horizontal image smearing. Widths of the Zeeman-split σ components, assuming a formation layer thickness of 200 km, indicate that vertical field strength gradients can be as large
as 6.5 G/km in a penumbra. |
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