{"title":"Magnetohydrodynamic instabilities in developed small-scale turbulence","authors":"N. Kleeorin, M. Mond, I. Rogachevskii","doi":"10.1063/1.860582","DOIUrl":null,"url":null,"abstract":"Modification of the magnetic force by a developed small‐scale magnetohydrodynamic (MHD) turbulence can result in the sign reversal of the effective magnetic pressure. It is due to negative contribution of the MHD turbulence, to the large‐scale magnetic force. It can significantly lower the elasticity of the large‐scale magnetic field [ Sov. Phys. JETP 70, 878 (1990)]. This effect excites instabilities of the large‐scale magnetic field due to the energy transfer from the turbulent pulsations to the latter. The nonturbulent stability criteria are modified due to the effective negative magnetic pressure. These instabilities may provide a mechanism of the large‐scale magnetic ropes formation in the solar convective zone and spiral galaxies. In addition, the instabilities can excite the short‐period solar oscillations.","PeriodicalId":113346,"journal":{"name":"Physics of fluids. B, Plasma physics","volume":"73 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"1993-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"24","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Physics of fluids. B, Plasma physics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.860582","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 24
Abstract
Modification of the magnetic force by a developed small‐scale magnetohydrodynamic (MHD) turbulence can result in the sign reversal of the effective magnetic pressure. It is due to negative contribution of the MHD turbulence, to the large‐scale magnetic force. It can significantly lower the elasticity of the large‐scale magnetic field [ Sov. Phys. JETP 70, 878 (1990)]. This effect excites instabilities of the large‐scale magnetic field due to the energy transfer from the turbulent pulsations to the latter. The nonturbulent stability criteria are modified due to the effective negative magnetic pressure. These instabilities may provide a mechanism of the large‐scale magnetic ropes formation in the solar convective zone and spiral galaxies. In addition, the instabilities can excite the short‐period solar oscillations.
京公网安备 11010802042870号
京ICP备2023020795号-1
分享
求助内容：
应助结果提醒方式：
扫码关注我们
