Three dimensional structure of a regular sunspot from the inversion of IR Stokes profiles

• DOI: 10.1051/0004-6361:20031282
• Publication Date: 2003-10-14T13:14:18Z
• Authors: S. K. Mathew; A. Lagg; S. K. Solanki; M. Collados; J. M. Borrero; S. Berdyugina; N. Krupp; J. Woch; C. Frutiger
• Keywords: Sunspot; Zenith; Penumbra; Field strength

The magnetic, thermal and velocity structure of a regular sunspot, observed close to solar disk center is presented. Spectropolarimetric data obtained with the Tenerife Infrared Polarimeter (TIP) in two infrared Fe I lines at 15 648.5 Åand 652.8 Åare inverted employing technique based on response functions retrieve atmospheric stratification every point sunspot. In order improve results for umbra, profiles Zeeman split OH blending also consistently fit. Thus we obtain maps temperature, line-of-sight velocity, magnetic field strength, inclination, azimuth, as function both location within sunspot height atmosphere. We present these an optical depth range between log = 0 , where provide accurate results. find decreasing strength increasing all over particularly large vertical gradient ~-4 G km-1 umbra. observe so called “spine” structures penumbra, i.e. extended radial features stronger more than surroundings. Also found that zenith angle increases height. From map it clear Evershed flow avoids spines mostly concentrates inclined intervening field. inclination few locations outer penumbra lower layers goes beyond 90°. These coincide strongest flows map.