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Turbulent heating and anisotropy in ...

Montagud-Camps, Victor.

Turbulent heating and anisotropy in the solar winda numerical study /

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Turbulent heating and anisotropy in the solar windby Victor Montagud-Camps.
其他題名:	a numerical study /
作者:	Montagud-Camps, Victor.
出版者:	Cham :Springer International Publishing :2019.
面頁冊數:	xvii, 123 p. :ill. (some col.), digital ;24 cm.
Contained By:	Springer eBooks
標題:	Solar wind.
電子資源:	https://doi.org/10.1007/978-3-030-30383-9
ISBN:	9783030303839

Turbulent heating and anisotropy in the solar winda numerical study /
Montagud-Camps, Victor.

Turbulent heating and anisotropy in the solar winda numerical study /[electronic resource] :by Victor Montagud-Camps. - Cham :Springer International Publishing :2019. - xvii, 123 p. :ill. (some col.), digital ;24 cm. - Springer theses,2190-5053. - Springer theses..

Introduction -- Solar Wind -- Plasma description -- Turbulence -- Solar Wind turbulence -- Plan of this thesis -- The Maltese Cross revisited -- Parameters and initial conditions -- Deﬁning spectral properties in EBM simulations -- Results -- Discussion -- Can the Maltese Cross heat? -- Paper ApJ 2018: "Turbulent Heating between 0.2 and 1 au: A Numerical Study" -- Heating fast winds -- Conclusions and future work -- Conclusions -- Future work: Anisotropy temperature description -- Appendix.

This book presents two important new findings. First, it demonstrates from first principles that turbulent heating offers an explanation for the non-adiabatic decay of proton temperature in solar wind. Until now, this was only proved with reduced or phenomenological models. Second, the book demonstrates that the two types of anisotropy of turbulent fluctuations that are observed in solar wind at 1AU originate not only from two distinct classes of conditions near the Sun but also from the imbalance in Alfven wave populations. These anisotropies do not affect the overall turbulent heating if we take into account the relation observed in solar wind between anisotropy and Alfven wave imbalance. In terms of the methods used to obtain these achievements, the author shows the need to find a very delicate balance between turbulent decay and expansion losses, so as to directly solve the magnetohydrodynamic equations, including the wind expansion effects.

ISBN: 9783030303839

Standard No.: 10.1007/978-3-030-30383-9doiSubjects--Topical Terms:

323090
Solar wind.

LC Class. No.: QB529 / .M668 2019

Dewey Class. No.: 523.58

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520 $a This book presents two important new findings. First, it demonstrates from first principles that turbulent heating offers an explanation for the non-adiabatic decay of proton temperature in solar wind. Until now, this was only proved with reduced or phenomenological models. Second, the book demonstrates that the two types of anisotropy of turbulent fluctuations that are observed in solar wind at 1AU originate not only from two distinct classes of conditions near the Sun but also from the imbalance in Alfven wave populations. These anisotropies do not affect the overall turbulent heating if we take into account the relation observed in solar wind between anisotropy and Alfven wave imbalance. In terms of the methods used to obtain these achievements, the author shows the need to find a very delicate balance between turbulent decay and expansion losses, so as to directly solve the magnetohydrodynamic equations, including the wind expansion effects.
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