Diagnosis of 3D magnetic field and mode composition in MHD turbulence with Y-parameter

被引：8

作者：

Malik, Sunil ^{[1
,2
]}

Yuen, Ka Ho ^{[3
]}

Yan, Huirong ^{[1
,2
]}

机构：

[1] Univ Potsdam, Inst Phys & Astron, Golm Haus 28, D-14476 Potsdam, Germany

[2] Deutsch Elekt Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany

[3] Los Alamos Natl Lab, Theoret Div, Los Alamos, NM 87545 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 524卷 / 04期

关键词：

magnetic fields; MHD; polarization; turbulence; ISM: general; radio continuum: general; COSMIC-RAY PROPAGATION; ROTATION MEASURE; MAGNETOHYDRODYNAMIC TURBULENCE; VELOCITY CENTROIDS; CHARGED-PARTICLES; RADIO-CONTINUUM; SOLAR-WIND; INTERSTELLAR; POLARIZATION; FLUCTUATIONS;

D O I：

10.1093/mnras/stad2225

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetic fields are crucial in numerous astrophysical processes within the interstellar medium (ISM). However, the detailed determination of magnetic field geometry is notoriously challenging. Based on the modern magnetohydrodynamic (MHD) turbulence theory, we introduce a novel statistical technique, the 'Y-parameter', to decipher the magnetic field inclination in the ISM and identify dominant turbulence modes. The Y-parameter, calculated as the ratio of anisotropies of different Stokes parameter combinations, displays contrasting trends with the mean-field inclination angle in Alfvenic and compressible turbulence modes. A Y-parameter value around 1.5 & PLUSMN; 0.5 provide a statistical boundary to determine the dominant MHD turbulence modes. We have discovered specific correlations between the Y-parameter value and the inclination angle that unveil the dominant turbulence mode. This methodology, when applied to future radio polarization surveys such as LOFAR and SKA, promises to significantly enhance our knowledge of 3D magnetic field in the ISM and improve our understanding of interstellar turbulence.

引用

页码：6102 / 6113

页数：12

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