Viscous damping of Alfvén surface waves in the solar atmosphere

Rathinavelu, G. D.; Sivaraman, M. R.; Narayanan, A. Satya

doi:10.1134/s1063780x09110075

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Physical Parameters In the Atmosphere Of The Sun1

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Cited by 9 publications

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“…Table 1. Physical parameter in solar atmosphere (Priest, 1983;Hood, 1992;Nakarikov et al, 1996;Gombosi, 1998;Choudhuri, 1998;Belien et al, 1999;Keppens and Goedbloed, 2000;Velli et al, 2003;Zaliznyak et al, 2003;Verdini et al, 2005;Selwa et al, 2005;Zhelyazkov, 2009;Rathinavelu et al, 2009;Wang et al, 2009;Wang et al, 2010;Ryutova et al, 2010;Foullon et al, 2011;Ofman and Thomson, 2011;Cavus and Kazkapan, 2013).…”

Section: Physical Parameters In the Atmosphere Of The Sunmentioning

confidence: 99%

A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layer: Part II. An application to the atmosphere of the Sun

Çavuş

Hoshoudy

2019

Astrophys Space Sci

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The main aim of this submission is to investigate the effects of some parameters like wave number, shear velocity, magnetic field and temperature for the growth rate of the magnetized Kelvin-Helmholtz instability (KHI) with incessant profiles through interface of two viscous fluid layer occurred in the solar atmosphere using the model of Hoshoudy, Cavus and Mahdy (2019). In this examination, the presence of KHI is identified for the various cases of wave number, magnetic field, shear velocity and temperature in the solar atmosphere. The sensible values of these parameters were acquired.

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