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Title: MAGNETIC LOOPS IN THE QUIET SUN

Abstract

We investigate the fine structure of magnetic fields in the atmosphere of the quiet Sun. We use photospheric magnetic field measurements from SUNRISE/IMaX with unprecedented spatial resolution to extrapolate the photospheric magnetic field into higher layers of the solar atmosphere with the help of potential and force-free extrapolation techniques. We find that most magnetic loops that reach into the chromosphere or higher have one footpoint in relatively strong magnetic field regions in the photosphere. Ninety-one percent of the magnetic energy in the mid-chromosphere (at a height of 1 Mm) is in field lines, whose stronger footpoint has a strength of more than 300 G, i.e., above the equipartition field strength with convection. The loops reaching into the chromosphere and corona are also found to be asymmetric in the sense that the weaker footpoint has a strength B < 300 G and is located in the internetwork (IN). Such loops are expected to be strongly dynamic and have short lifetimes, as dictated by the properties of the IN fields.

Authors:
; ; ;  [1]; ;  [2]; ;  [3];  [4];  [5];  [6];  [7]
  1. Max-Planck-Institut fuer Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau (Germany)
  2. Kiepenheuer-Institut fuer Sonnenphysik, Schoeneckstr. 6, 79104 Freiburg (Germany)
  3. Instituto de Astrofisica de Canarias, C/Via Lactea s/n, 38200 La Laguna, Tenerife (Spain)
  4. Instituto de Astrofisica de Andalucia (CSIC), Apartado de Correos 3004, 18080 Granada (Spain)
  5. Grupo de Astronomia y Ciencias del Espacio, Universidad de Valencia, 46980 Paterna, Valencia (Spain)
  6. High Altitude Observatory, National Center for Atmospheric Research Boulder, CO 80307 (United States)
  7. Lockheed Martin Solar and Astrophysics Laboratory, Bldg. 252, 3251 Hanover Street, Palo Alto, CA 94304 (United States)
Publication Date:
OSTI Identifier:
21457030
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 723; Journal Issue: 2; Other Information: DOI: 10.1088/2041-8205/723/2/L185
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASYMMETRY; CHROMOSPHERE; CONVECTION; MAGNETIC FIELDS; PHOTOSPHERE; SPATIAL RESOLUTION; SUN; ATMOSPHERES; ENERGY TRANSFER; HEAT TRANSFER; MAIN SEQUENCE STARS; MASS TRANSFER; RESOLUTION; SOLAR ATMOSPHERE; STARS; STELLAR ATMOSPHERES

Citation Formats

Wiegelmann, T., Solanki, S. K., Barthol, P., Gandorfer, A., Borrero, J. M., Schmidt, W., Pillet, V. MartInez, Bonet, J. A., Del Toro Iniesta, J. C., Domingo, V., Knoelker, M., and Title, A. M., E-mail: wiegelmann@mps.mpg.d. MAGNETIC LOOPS IN THE QUIET SUN. United States: N. p., 2010. Web. doi:10.1088/2041-8205/723/2/L185.
Wiegelmann, T., Solanki, S. K., Barthol, P., Gandorfer, A., Borrero, J. M., Schmidt, W., Pillet, V. MartInez, Bonet, J. A., Del Toro Iniesta, J. C., Domingo, V., Knoelker, M., & Title, A. M., E-mail: wiegelmann@mps.mpg.d. MAGNETIC LOOPS IN THE QUIET SUN. United States. doi:10.1088/2041-8205/723/2/L185.
Wiegelmann, T., Solanki, S. K., Barthol, P., Gandorfer, A., Borrero, J. M., Schmidt, W., Pillet, V. MartInez, Bonet, J. A., Del Toro Iniesta, J. C., Domingo, V., Knoelker, M., and Title, A. M., E-mail: wiegelmann@mps.mpg.d. Wed . "MAGNETIC LOOPS IN THE QUIET SUN". United States. doi:10.1088/2041-8205/723/2/L185.
@article{osti_21457030,
title = {MAGNETIC LOOPS IN THE QUIET SUN},
author = {Wiegelmann, T. and Solanki, S. K. and Barthol, P. and Gandorfer, A. and Borrero, J. M. and Schmidt, W. and Pillet, V. MartInez and Bonet, J. A. and Del Toro Iniesta, J. C. and Domingo, V. and Knoelker, M. and Title, A. M., E-mail: wiegelmann@mps.mpg.d},
abstractNote = {We investigate the fine structure of magnetic fields in the atmosphere of the quiet Sun. We use photospheric magnetic field measurements from SUNRISE/IMaX with unprecedented spatial resolution to extrapolate the photospheric magnetic field into higher layers of the solar atmosphere with the help of potential and force-free extrapolation techniques. We find that most magnetic loops that reach into the chromosphere or higher have one footpoint in relatively strong magnetic field regions in the photosphere. Ninety-one percent of the magnetic energy in the mid-chromosphere (at a height of 1 Mm) is in field lines, whose stronger footpoint has a strength of more than 300 G, i.e., above the equipartition field strength with convection. The loops reaching into the chromosphere and corona are also found to be asymmetric in the sense that the weaker footpoint has a strength B < 300 G and is located in the internetwork (IN). Such loops are expected to be strongly dynamic and have short lifetimes, as dictated by the properties of the IN fields.},
doi = {10.1088/2041-8205/723/2/L185},
journal = {Astrophysical Journal Letters},
number = 2,
volume = 723,
place = {United States},
year = {Wed Nov 10 00:00:00 EST 2010},
month = {Wed Nov 10 00:00:00 EST 2010}
}