03934nam 22006255 450 991034950520332120200630011112.03-030-30383-710.1007/978-3-030-30383-9(CKB)4100000009523020(DE-He213)978-3-030-30383-9(MiAaPQ)EBC5941797(PPN)248600982(EXLCZ)99410000000952302020191011d2019 u| 0engurnn|008mamaatxtrdacontentcrdamediacrrdacarrierTurbulent Heating and Anisotropy in the Solar Wind A Numerical Study /by Victor Montagud-Camps1st ed. 2019.Cham :Springer International Publishing :Imprint: Springer,2019.1 online resource (XVII, 123 p. 45 illus., 13 illus. in color.) Springer Theses, Recognizing Outstanding Ph.D. Research,2190-5053"Doctoral thesis accepted by Paris-Sud University, Orsay, France"--Title page.3-030-30382-9 Includes bibliographical references and index.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 Alfvén 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 Alfvén 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. .Springer Theses, Recognizing Outstanding Ph.D. Research,2190-5053Solar systemSpace sciencesAstrophysicsMathematical physicsSolar and Heliospheric Physics https://scigraph.springernature.com/ontologies/product-market-codes/P22070Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics)https://scigraph.springernature.com/ontologies/product-market-codes/P22030Theoretical Astrophysicshttps://scigraph.springernature.com/ontologies/product-market-codes/P22080Solar system.Space sciences.Astrophysics.Mathematical physics.Solar and Heliospheric Physics .Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics).Theoretical Astrophysics.523.2523.58Montagud-Camps Victorauthttp://id.loc.gov/vocabulary/relators/aut838642MiAaPQMiAaPQMiAaPQBOOK9910349505203321Turbulent Heating and Anisotropy in the Solar Wind2522948UNINA