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Turbulent heating and anisotropy in ...

Montagud-Camps, Victor.

Turbulent heating and anisotropy in the solar winda numerical study /

Record Type:	Electronic resources : Monograph/item
Title/Author:	Turbulent heating and anisotropy in the solar windby Victor Montagud-Camps.
Reminder of title:	a numerical study /
Author:	Montagud-Camps, Victor.
Published:	Cham :Springer International Publishing :2019.
Description:	xvii, 123 p. :ill. (some col.), digital ;24 cm.
Contained By:	Springer eBooks
Subject:	Solar wind.
Online resource:	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

Turbulent heating and anisotropy in the solar winda numerical study /
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100 1 $a Montagud-Camps, Victor. $3 853956
245 1 0 $a Turbulent heating and anisotropy in the solar wind $h [electronic resource] : $b a numerical study / $c by Victor Montagud-Camps.
260 $a Cham : $b Springer International Publishing : $b Imprint: Springer, $c 2019.
300 $a xvii, 123 p. : $b ill. (some col.), digital ; $c 24 cm.
490 1 $a Springer theses, $x 2190-5053
505 0 $a 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.
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.
650 0 $a Solar wind. $3 323090
650 0 $a Turbulence. $3 188320
650 0 $a Magnetohydrodynamics. $3 207822
650 1 4 $a Solar and Heliospheric Physics. $3 771511
650 2 4 $a Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics) $3 770123
650 2 4 $a Theoretical Astrophysics. $3 821426
710 2 $a SpringerLink (Online service) $3 273601
773 0 $t Springer eBooks
830 0 $a Springer theses. $3 557607
856 4 0 $u https://doi.org/10.1007/978-3-030-30383-9
950 $a Physics and Astronomy (Springer-11651)