Interpreting Magnetic Variance Anisotropy Measurements in the Solar Wind

Дата и время публикации : 2012-05-03T16:05:32Z

Авторы публикации и институты :
J. M. TenBarge
J. J. Podesta
K. G. Klein
G. G. Howes

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 15 pages, 10 figures, accepted for publication in The Astrophysical Journal
Первичная категория: physics.space-ph

Все категории : physics.space-ph, astro-ph.SR, physics.plasm-ph

Краткий обзор статьи: The magnetic variance anisotropy ($mathcal{A}_m$) of the solar wind has been used widely as a method to identify the nature of solar wind turbulent fluctuations; however, a thorough discussion of the meaning and interpretation of the $mathcal{A}_m$ has not appeared in the literature. This paper explores the implications and limitations of using the $mathcal{A}_m$ as a method for constraining the solar wind fluctuation mode composition and presents a more informative method for interpreting spacecraft data. The paper also compares predictions of the $mathcal{A}_m$ from linear theory to nonlinear turbulence simulations and solar wind measurements. In both cases, linear theory compares well and suggests the solar wind for the interval studied is dominantly Alfv’{e}nic in the inertial and dissipation ranges to scales $k rho_i simeq 5$.

Category: Physics