On the origin of the magnetic energy in the quiet solar chromosphere
| Autor: | Boris V. Gudiksen, Mats Carlsson, Juan Martinez-Sykora, Bart De Pontieu, Milan Gošić, Viggo Hansteen |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
Physics
Photosphere 010504 meteorology & atmospheric sciences Magnetic energy FOS: Physical sciences Astronomy and Astrophysics Astrophysics 01 natural sciences Magnetic flux Magnetic field Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science 0103 physical sciences Physics::Space Physics Radiative transfer Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Magnetohydrodynamics 010303 astronomy & astrophysics Chromosphere Solar and Stellar Astrophysics (astro-ph.SR) 0105 earth and related environmental sciences Dynamo |
| ISSN: | 0004-637X |
| Popis: | The presence of magnetic field is crucial in the transport of energy through the solar atmosphere. Recent ground-based and space-borne observations of the quiet Sun have revealed that magnetic field accumulates at photospheric heights, via a local dynamo or from small-scale flux emergence events. However, most of this small-scale magnetic field may not expand into the chromosphere due to the entropy drop with height at the photosphere. Here we present a study that uses a high resolution 3D radiative MHD simulation of the solar atmosphere with non-grey and non-LTE radiative transfer and thermal conduction along the magnetic field to reveal that: 1) the net magnetic flux from the simulated quiet photosphere is not sufficient to maintain a chromospheric magnetic field (on average), 2) processes in the lower chromosphere, in the region dominated by magneto-acoustic shocks, are able to convert kinetic energy into magnetic energy, 3) the magnetic energy in the chromosphere increases linearly in time until the r.m.s. of the magnetic field strength saturates at roughly 4 to 30 G (horizontal average) due to conversion from kinetic energy, 4) and that the magnetic features formed in the chromosphere are localized to this region. 12 pages, 14 figures, accepted to be published in ApJ |
| Databáze: | OpenAIRE |
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