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Title: RESOLVING THE INTERNAL MAGNETIC STRUCTURE OF THE SOLAR NETWORK

Abstract

We analyze the spectral asymmetry of Stokes V (circularly polarized) profiles of an individual network patch in the quiet Sun observed by Sunrise/IMaX. At a spatial resolution of 0.''15-0.''18, the network elements contain substructure which is revealed by the spatial distribution of Stokes V asymmetries. The area asymmetry between the red and blue lobes of Stokes V increases from nearly zero at the core of the structure to values close to unity at its edges (single-lobed profiles). Such a distribution of the area asymmetry is consistent with magnetic fields expanding with height, i.e., an expanding magnetic canopy (which is required to fulfill pressure balance and flux conservation in the solar atmosphere). Inversion of the Stokes I and V profiles of the patch confirms this picture, revealing a decreasing field strength and increasing height of the canopy base from the core to the periphery of the network patch. However, the non-roundish shape of the structure and the presence of negative area and amplitude asymmetries reveal that the scenario is more complex than a canonical flux tube expanding with height surrounded by downflows.

Authors:
;  [1]; ;  [2]; ;  [3];  [4]
  1. Instituto de Astrofisica de Canarias, Via Lactea s/n, E-38205 La Laguna, Tenerife (Spain)
  2. Instituto de Astrofisica de Andalucia (CSIC), Apdo. de Correos 3004, E-18080 Granada (Spain)
  3. Max-Planck-Institut fuer Sonnensystemforschung, D-37191 Katlenburg-Lindau (Germany)
  4. KIS Kiepenheuer-Institut fuer Sonnenphysik, D-79104 Freiburg (Germany)
Publication Date:
OSTI Identifier:
22078478
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 758; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; AMPLITUDES; ASYMMETRY; HEIGHT; MAGNETIC FIELDS; POLARIZATION; SOLAR ATMOSPHERE; SPATIAL DISTRIBUTION; SPATIAL RESOLUTION; SUN

Citation Formats

Martinez Gonzalez, M. J., Martinez Pillet, V., Bellot Rubio, L. R., Del Toro Iniesta, J. C., Solanki, S. K., Barthol, P., and Schmidt, W. RESOLVING THE INTERNAL MAGNETIC STRUCTURE OF THE SOLAR NETWORK. United States: N. p., 2012. Web. doi:10.1088/2041-8205/758/2/L40.
Martinez Gonzalez, M. J., Martinez Pillet, V., Bellot Rubio, L. R., Del Toro Iniesta, J. C., Solanki, S. K., Barthol, P., & Schmidt, W. RESOLVING THE INTERNAL MAGNETIC STRUCTURE OF THE SOLAR NETWORK. United States. doi:10.1088/2041-8205/758/2/L40.
Martinez Gonzalez, M. J., Martinez Pillet, V., Bellot Rubio, L. R., Del Toro Iniesta, J. C., Solanki, S. K., Barthol, P., and Schmidt, W. Sat . "RESOLVING THE INTERNAL MAGNETIC STRUCTURE OF THE SOLAR NETWORK". United States. doi:10.1088/2041-8205/758/2/L40.
@article{osti_22078478,
title = {RESOLVING THE INTERNAL MAGNETIC STRUCTURE OF THE SOLAR NETWORK},
author = {Martinez Gonzalez, M. J. and Martinez Pillet, V. and Bellot Rubio, L. R. and Del Toro Iniesta, J. C. and Solanki, S. K. and Barthol, P. and Schmidt, W.},
abstractNote = {We analyze the spectral asymmetry of Stokes V (circularly polarized) profiles of an individual network patch in the quiet Sun observed by Sunrise/IMaX. At a spatial resolution of 0.''15-0.''18, the network elements contain substructure which is revealed by the spatial distribution of Stokes V asymmetries. The area asymmetry between the red and blue lobes of Stokes V increases from nearly zero at the core of the structure to values close to unity at its edges (single-lobed profiles). Such a distribution of the area asymmetry is consistent with magnetic fields expanding with height, i.e., an expanding magnetic canopy (which is required to fulfill pressure balance and flux conservation in the solar atmosphere). Inversion of the Stokes I and V profiles of the patch confirms this picture, revealing a decreasing field strength and increasing height of the canopy base from the core to the periphery of the network patch. However, the non-roundish shape of the structure and the presence of negative area and amplitude asymmetries reveal that the scenario is more complex than a canonical flux tube expanding with height surrounded by downflows.},
doi = {10.1088/2041-8205/758/2/L40},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 2,
volume = 758,
place = {United States},
year = {2012},
month = {10}
}