Conveners
Deep seated vs. distributed magnetic field generation in the Sun
- Alexander Kosovichev (New Jersey Institute of Technology)
Deep seated vs. distributed magnetic field generation in the Sun
- Aimee Norton (Stanford University)
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Yuhong Fan (NCAR)10/03/2015, 11:30We report the results of a magneto-hydrodynamic (MHD) simulation of a convective dynamo in a model solar convective envelope driven by the solar radiative diffusive heat flux. The convective dynamo produces a large-scale mean magnetic field that exhibits irregular cyclic behavior with oscillation time scales ranging from about 5 to 15 yr and undergoes irregular polarity reversals. The...Go to contribution page
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Yori Fournier (Leibniz Institute for Astrophysics)10/03/2015, 12:10We would like to introduce a robust but still under work method to probe the existence of flux tubes in low mass stars. This method is based on the ability of numerical simulations to predict a magnetic-field--rotation relation for solar-like stars. Thanks to the observations compiled up to the present day, this theoretical relation can be compared with the corresponding observed...Go to contribution page
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Gustavo Guerrero (Universidade Federal de Minas Gerais)10/03/2015, 12:30The solar dynamo, responsible for sunspot formation, is thought to be operating somewhere within the solar interior. Unfortunately, the available observation techniques are not able to observe magnetic field in inner convection zone but only at the solar surface. There are, however, several observational constrains like the cycle period, magnetic field migration or the phase lag between...Go to contribution page
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Hideyuki Hotta (HAO/NCAR)10/03/2015, 14:30Recent results of high-resolution MHD calculation of solar convection zone will be shown. Higher-resolution calculations enable us to investigate the efficient small-scale dynamo in the solar global convection zone. In our highest resolution, efficient small-scale dynamo is excited throughout the convection zone and magnetic field can reach almost equipartition strength. The...Go to contribution page
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Jörn Warnecke (Max-Planck-Institut für Sonnesystemforschung)10/03/2015, 15:10Sunspots occurring on the solar surface following a typical pattern during the activity cycle. At the beginning of the cycle they appear at high latitude, whereas at the end they appear close to the equator. This is associated with an underlying strong toroidal field which migrates equatorward. Since a few years this behavior has been reproduced in global convective dynamo simulations. I...Go to contribution page
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Bidya Binay Karak (Nordita)10/03/2015, 15:30One of the most striking aspects of 11-year sunspot cycles is that there have been times in the past when sunspots did not appear for several years. The most well-known example of this is the Maunder minimum during 1645-1715. Analyses of cosmogenic isotopes (14C and 10Be) indicate that there have been about 27 grand minima in the last 11,000 yr. In my talk I shall address the question...Go to contribution page
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Rohan Eugene Louis (Leibniz Institute for astrophysics (AIP))10/03/2015, 15:50Sunspots are ideal candidates for probing and understanding the coupling between various layers of the solar atmosphere. In this talk I shall describe how this coupling spans a broad range of spatial and temporal scales in the context of existing theoretical interpretations and the ever increasing need for coordinated observations between ground and space-based facilities.Go to contribution page