Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere
We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to so...
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| Published in | Advances in space research Vol. 61; no. 2; pp. 617 - 627 |
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| Main Authors | , |
| Format | Journal Article |
| Language | English |
| Published |
Elsevier Ltd
15.01.2018
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| Subjects | |
| Online Access | Get full text |
| ISSN | 0273-1177 1879-1948 |
| DOI | 10.1016/j.asr.2017.05.032 |
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| Abstract | We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to solar gravity. Incorporating specific forms of current density and gas pressure in the Grad–Shafranov equation, we solve the magnetic flux function, and find it to be separable with a Coulomb wave function in radial direction while the vertical part of the solution decreases exponentially. We employ improved fluxtube boundary conditions and take a realistic ambient external pressure for the photosphere to transition region, to derive a family of solutions for reasonable values of the fluxtube radius and magnetic field strength at the base of the axis that are the free parameters in our model. We find that our model estimates are consistent with the magnetic field strength and the radii of Magnetic bright points (MBPs) as estimated from observations. We also derive thermodynamic quantities inside the fluxtube. |
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| AbstractList | We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume that the fluxtube containing twisted magnetic fields is in magnetohydrostatic equilibrium within a realistic stratified atmosphere subject to solar gravity. Incorporating specific forms of current density and gas pressure in the Grad–Shafranov equation, we solve the magnetic flux function, and find it to be separable with a Coulomb wave function in radial direction while the vertical part of the solution decreases exponentially. We employ improved fluxtube boundary conditions and take a realistic ambient external pressure for the photosphere to transition region, to derive a family of solutions for reasonable values of the fluxtube radius and magnetic field strength at the base of the axis that are the free parameters in our model. We find that our model estimates are consistent with the magnetic field strength and the radii of Magnetic bright points (MBPs) as estimated from observations. We also derive thermodynamic quantities inside the fluxtube. |
| Author | Sen, S. Mangalam, A. |
| Author_xml | – sequence: 1 givenname: S. surname: Sen fullname: Sen, S. email: samrat@iiap.res.in – sequence: 2 givenname: A. surname: Mangalam fullname: Mangalam, A. email: mangalam@iiap.res.in |
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| Cites_doi | 10.1086/164837 10.1086/157188 10.1007/s11207-016-0922-1 10.1007/s11207-016-0889-y 10.1051/0004-6361/201629773 10.1007/s11207-011-9851-1 10.1051/0004-6361/200810867 10.1017/S0074180900237856 10.1051/0004-6361/201116894 10.1007/s11207-010-9534-3 10.1051/0004-6361/201424545 10.1007/s11207-009-9407-9 10.1134/S1063773715050072 10.1051/0004-6361/201322882 10.1093/mnras/stt1328 10.1086/521726 10.1007/s11207-015-0740-x 10.1088/2041-8205/723/2/L164 10.1051/0004-6361/200913846 10.1007/BF00151313 10.1007/BF00148783 10.1086/528956 10.1086/378512 10.1086/176504 10.1086/523671 10.1063/1.1756167 10.1051/0004-6361/200912450 |
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| Keywords | Magnetohydrodynamics (MHD) Sun: photosphere Sun: transition region Magnetohydrostatics Sun: magnetic fields |
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| Snippet | We build a single vertical straight magnetic fluxtube spanning the solar photosphere and the transition region which does not expand with height. We assume... |
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| SubjectTerms | Magnetohydrodynamics (MHD) Magnetohydrostatics Sun: magnetic fields Sun: photosphere Sun: transition region |
| Title | Model of a fluxtube with a twisted magnetic field in the stratified solar atmosphere |
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