Ministerio de Economía y Competitividad Gobierno de Canarias Universidad de La Laguna CSIC Centro de Excelencia Severo Ochoa

Results Gallery

Select a year: 2017 | 2016 | 2015 | 2014 | 2013 | 2012 | 2011 | 2010 | 2009 | 2008 | 2007 | 2006 | 2005 | 2004 | 2003 |

· More scientific highlights from this year.

Resolving the Internal Magnetic Structure of the Solar Network.

Author/s: Martínez González, M. J., Bellot Rubio, L. R., Solanki, S. K., Martínez Pillet, V., Del Toro Iniesta, J. C., Barthol, P., & Schmidt, W.

Reference: 2012, ApJ, 758, 40L

Logarithm of the optical depth of the discontonuity between the magnetic and the non magnetic atmosphere (i.e. the base of the canopy). Large positive numbers mean deep in the atmosphere while large negative numbers are higher layers of the atmosphere. The increasing height of the discontinuity from the centre to the borders draw a magnetic field expanding with height.
Logarithm of the optical depth of the discontonuity between the magnetic and the non magnetic atmosphere (i.e. the base of the canopy). Large positive numbers mean deep in the atmosphere while large negative numbers are higher layers of the atmosphere. The increasing height of the discontinuity from the centre to the borders draw a magnetic field expanding with height.

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.

We use our own cookies and cookies from a third party to gather statistical information to improve our services and our website. If you continue with the navigation, you are accepting the installation and use of these cookies. You can change the configuration of your browser not to accept the installation or you can obtain more information in our Cookie Policy.

OK