Estimation of Turbulent Heating of Solar Wind Protons at 1 au

Livadiotis, G.; Dayeh, M. A.; Zank, G. P.

doi:10.3847/1538-4357/abc5c3

Cited by 9 publications

(6 citation statements)

References 45 publications

(39 reference statements)

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“…The factor g κ , N depends on the kappa index κ and the number of correlated particles; for a large number of particles, it becomes g κ , N ≈ 1. Finally, the phase-space parcel

is typically given by the Planck’s constant, but it was shown to represent a different and larger constant in space plasmas, where Debye shielding limits the distance of correlations,

[ 55 , 59 , 60 , 61 , 62 , 63 ] (namely,

, when no correlations exist among particles, and

, when significant correlations exist among particles beyond their nearest neighbors, as in the case of the majority of space plasmas).…”

Section: Entropic Formalism Associated With Kappa Distributionsmentioning

confidence: 99%

Thermodynamic Definitions of Temperature and Kappa and Introduction of the Entropy Defect

Livadiotis

McComas

2021

Entropy

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This paper develops explicit and consistent definitions of the independent thermodynamic properties of temperature and the kappa index within the framework of nonextensive statistical mechanics and shows their connection with the formalism of kappa distributions. By defining the “entropy defect” in the composition of a system, we show how the nonextensive entropy of systems with correlations differs from the sum of the entropies of their constituents of these systems. A system is composed extensively when its elementary subsystems are independent, interacting with no correlations; this leads to an extensive system entropy, which is simply the sum of the subsystem entropies. In contrast, a system is composed nonextensively when its elementary subsystems are connected through long-range interactions that produce correlations. This leads to an entropy defect that quantifies the missing entropy, analogous to the mass defect that quantifies the mass (energy) associated with assembling subatomic particles. We develop thermodynamic definitions of kappa and temperature that connect with the corresponding kinetic definitions originated from kappa distributions. Finally, we show that the entropy of a system, composed by a number of subsystems with correlations, is determined using both discrete and continuous descriptions, and find: (i) the resulted entropic form expressed in terms of thermodynamic parameters; (ii) an optimal relationship between kappa and temperature; and (iii) the correlation coefficient to be inversely proportional to the temperature logarithm.

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“…The factor g κ , N depends on the kappa index κ and the number of correlated particles; for a large number of particles, it becomes g κ , N ≈ 1. Finally, the phase-space parcel

is typically given by the Planck’s constant, but it was shown to represent a different and larger constant in space plasmas, where Debye shielding limits the distance of correlations,

[ 55 , 59 , 60 , 61 , 62 , 63 ] (namely,

, when no correlations exist among particles, and

, when significant correlations exist among particles beyond their nearest neighbors, as in the case of the majority of space plasmas).…”

Section: Entropic Formalism Associated With Kappa Distributionsmentioning

confidence: 99%

Thermodynamic Definitions of Temperature and Kappa and Introduction of the Entropy Defect

Livadiotis

McComas

2021

Entropy

Self Cite

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“…Many previous works have used the measurement of plasma properties in the solar wind to derive the rates of energy dissipation from processes such as magnetohydrodynamic (MHD) turbulence (e. g., Tu 1988;Verma et al 1995;Smith et al 2001;MacBride et al 2005;Livadiotis et al 2020;. Most of these studies, however, analyzed the energy budget of a single charged species and did not consider protons and electrons together (Hellinger et al 2011;Scudder 2015;Stverak et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment

Bandyopadhyay,

Meyer,

Matthaeus

et al. 2023

ApJL

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A central problem of space plasma physics is how protons and electrons are heated in a turbulent, magnetized plasma. The differential heating of charged species due to dissipation of turbulent fluctuations plays a key role in solar wind evolution. Measurements from previous heliophysics missions have provided estimates of proton and electron heating rates beyond 0.27 au. Using Parker Solar Probe (PSP) data accumulated during the first 10 encounters, we extend the evaluation of the individual rates of heat deposition for protons and electrons to a distance of 0.063 au (13.5 R ⊙) in the newly formed solar wind. The PSP data in the near-Sun environment show different behavior of the electron heat conduction flux from what was predicted from previous fits to Helios and Ulysses data. Consequently, the empirically derived proton and electron heating rates exhibit significantly different behavior than previous reports, with the proton heating becoming increasingly dominant over electron heating at decreasing heliocentric distances. We find that the protons receive about 80% of the total plasma heating at ≈13 R ⊙, slightly higher than the near-Earth values. This empirically derived heating partition between protons and electrons will help to constrain theoretical models of solar wind heating.

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“…Next, we connect the derived polytropic indices with the entropy gradient (Adhikari et al 2020;Livadiotis et al 2020) and the turbulent heating gradient (Verma et al 1995;Vasquez et al 2007;Livadiotis 2019Livadiotis , 2021. Combining the entropy expressed in terms of temperature and density…”

Section: Resultsmentioning

confidence: 99%

Polytropic Behavior in the Structures of Interplanetary Coronal Mass Ejections

Dayeh

Livadiotis

2022

ApJL

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The polytropic process characterizes the thermodynamics of space plasma particle populations. The polytropic index, γ, is particularly important as it describes the thermodynamic behavior of the system by quantifying the changes in temperature as the system is compressed or expanded. Using Wind spacecraft plasma and magnetic field data during 1995 February–2015 December, we investigate the thermodynamic evolution in 336 interplanetary coronal mass ejection (ICME) events. For each event, we derive the index γ in the sheath and magnetic ejecta structures, along with the pre- and post-event regions. We then examine the distributions of all γ indices in these four regions and derive the entropic gradient of each, which is indicative of the ambient heating. We find that in the ICME sheath region, where wave turbulence is expected to be highest, the thermodynamics takes longest to recover into the original quasi-adiabatic process, while it recovers faster in the quieter ejecta region. This pattern creates a thermodynamic cycle, featuring a near adiabatic value γ ∼ γ a (=5/3) upstream of the ICMEs, γ a − γ ∼ 0.26 in the sheaths, γ a − γ ∼ 0.13 in the ICME ejecta, and recovers again to γ ∼ γ a after the passage of the ICME. These results expose the turbulent heating rates in the ICME plasma: the lower the polytropic index from its adiabatic value and closer to its isothermal value, the larger the entropic gradient, and thus, the rate of turbulent heating that heats the ICME plasma.

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Estimation of Turbulent Heating of Solar Wind Protons at 1 au

Cited by 9 publications

References 45 publications

Thermodynamic Definitions of Temperature and Kappa and Introduction of the Entropy Defect

Thermodynamic Definitions of Temperature and Kappa and Introduction of the Entropy Defect

Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment

Polytropic Behavior in the Structures of Interplanetary Coronal Mass Ejections

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