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Flux tube model in the solar atmosphere

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dc.contributor.author Sen, Samrat
dc.contributor.author Mangalam, A
dc.date.accessioned 2020-11-10T13:31:12Z
dc.date.available 2020-11-10T13:31:12Z
dc.date.issued 2018-02
dc.identifier.citation Proceedings of the International Astronomical Union, Vol. 340, pp. 55-56 en_US
dc.identifier.issn 1743-9213
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6765
dc.description Restricted Access © International Astronomical Union https://doi.org/10.1017/S1743921318001096 en_US
dc.description.abstract We construct two classes of the magnetohydrostatic equilibria of the axisymmetric flux tubes with twisted magnetic fields in the stratified solar atmosphere that span from the photosphere to the transition region. We built the models by incorporating specific forms of the gas pressure and poloidal current in the Grad-Shafranov equation. This model gives both closed and open field structure of the flux tube. The other open field model we construct is based on the self-similar formulation, where we have incorporated specific forms of the gas pressure, poloidal current and two different shape functions. We study the homology of the parameter space that is consistent with the solar atmosphere and find that the estimation of the magnetic structure inside the flux tubes is consistent with the observation and simulation results of the magnetic bright points. en_US
dc.language.iso en en_US
dc.publisher Cambridge University Press en_US
dc.subject Magnetohydrodynamics (MHD) en_US
dc.subject Sun: photosphere en_US
dc.subject Sun: transition region en_US
dc.subject Sun: magnetic fields en_US
dc.title Flux tube model in the solar atmosphere en_US
dc.type Article en_US


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