EDP Sciences
Free Access
Volume 410, Number 2, November I 2003
Page(s) 695 - 710
Section Diffuse matter in space
DOI https://doi.org/10.1051/0004-6361:20031282
Published online 17 November 2003

A&A 410, 695-710 (2003)
DOI: 10.1051/0004-6361:20031282

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

S. K. Mathew1, A. Lagg1, S. K. Solanki1, M. Collados2, J. M. Borrero1, S. Berdyugina3, N. Krupp1, J. Woch1 and C. Frutiger3

1  Max-Planck-Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany
    e-mail: lagg@linmpi.mpg.de, solanki@linmpi.mpg.de, borrero@linmpi.mpg.de, krupp@linmpi.mpg.de, woch@linmpi.mpg.de
2  Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain
    e-mail: mcv@ll.iac.es
3  Institut für Astronomie, ETH, 8092 Zürich, Switzerland
    e-mail: sveta@astro.phys.ethz.ch, frutiger@astro.phys.ethz.ch

(Received 7 May 2003 / Accepted 8 August 2003)

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 15 652.8 Åare inverted employing a technique based on response functions to retrieve the atmospheric stratification at every point in the sunspot. In order to improve the results for the umbra, profiles of Zeeman split OH lines blending the Fe I 15 652.8 Åare also consistently fit. Thus we obtain maps of temperature, line-of-sight velocity, magnetic field strength, inclination, and azimuth, as a function of both location within the sunspot and height in the atmosphere. We present these maps for an optical depth range between log  $\tau _5$ = 0 and log  $\tau _5 = -1.5$, where these lines provide accurate results. We find decreasing magnetic field strength with increasing height all over the sunspot, with a particularly large vertical field gradient of ~ -4 G km -1 in the umbra. We also observe the so called "spine" structures in the penumbra, i.e. extended radial features with a stronger and more vertical magnetic field than the surroundings. Also we found that the magnetic field zenith angle increases with height. From the velocity map it is clear that the Evershed flow avoids the spines and mostly concentrates in the more inclined intervening field. The field inclination at a few locations in the outer penumbra in lower layers goes beyond 90°. These locations coincide with the strongest flows in the velocity map.

Key words: Sun: sunspots -- Sun: magnetic fields -- Sun: infrared -- Sun: general

Offprint request: S. K. Mathew, shibu@ll.iac.es

© ESO 2003

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