Plasma Parameters From Quasi‐Thermal Noise Observed by Parker Solar Probe: A New Model for the Antenna Response

Martinović, M.; Đorđević, Ana; Klein, K. G.; Maksimović, M.; Issautier, Karine; Liu, Mingzhe; Pulupa, M.; Bale, S. D.; Halekas, J. S.; McManus, Michael D.

doi:10.1029/2021ja030182

Cited by 3 publications

(2 citation statements)

References 47 publications

(78 reference statements)

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“…The FIELDS (Bale et al 2016) instrument suite measures magnetic and electric fields. Electron temperature T e and electron density n e data were evaluated from the quasithermal noise (QTN) spectrum provided by the electric field antennas (Pulupa et al 2017;Moncuquet et al 2020;Martinovic et al 2022).…”

Section: In Situ Datamentioning

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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Section: In Situ Datamentioning

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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“…It has been used in a number of space missions (e.g., Meyer-Vernet 1979;Meyer-Vernet et al 1986, 1993Meyer-Vernet et al 2017;Issautier et al 1999bIssautier et al , 2001aIssautier et al ,c, 2005Issautier et al , 2008Maksimovic et al 1995Maksimovic et al , 2005aMoncuquet et al 1995Moncuquet et al , 1997Moncuquet et al , 2005Moncuquet et al , 2006Martinović et al 2020;Le Chat et al 2011;Salem et al 2001;Lund et al 1994;Schippers et al 2013). Recent investigations (see Moncuquet et al 2020;Maksimovic et al 2020;Martinović et al 2022) have already applied this technique on PSP based on electric voltage spectra acquired by the Radio Frequency Spectrometer (RFS/FIELDS) (Pulupa et al 2017). Besides, SWEAP/PSP consists of the Solar Probe Cup (SPC) and the Solar Probe Analyzers (SPAN) (Kasper et al 2016;Case et al 2020;Whittlesey et al 2020;Livi et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Total Electron Temperature Derived from Quasi-Thermal Noise Spectroscopy In the Pristine Solar Wind: Parker Solar Probe Observations

Liu¹,

K.²,

M.³

et al. 2023

Preprint

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Aims. We apply the Quasi-thermal noise (QTN) method on Parker Solar Probe (PSP) observations to derive the total electron temperature (T e ) and present a combination of 12-day period of observations around each perihelion from Encounter One (E01) to Ten (E10) (with E08 not included) with the heliocentric distance varying from about 13 to 60 solar radii (R ). Methods. The QTN technique is a reliable tool to yield accurate measurements of the electron parameters in the solar wind. We obtain T e from the linear fit of the high-frequency part of the QTN spectra acquired by the RFS/FIELDS instrument. Then, we provide the mean radial electron temperature profile, and examine the electron temperature gradients for different solar wind populations (i.e. classified by the proton bulk speed (V p ), and the solar wind mass flux). Results. We find that the total electron temperature decreases with the distance as ∼R −0.66 , which is much slower than adiabatic. The extrapolated T e based on PSP observations is consistent with the exospheric solar wind model prediction at ∼10 R , Helios observations at ∼0.3 AU and Wind observations at 1 AU. Also, T e , extrapolated back to 10 R , is almost the same as the strahl electron temperature T s (measured by SPAN-E) which is considered to be closely related to or even almost equal to the coronal electron temperature. Furthermore, the radial T e profiles in the slower solar wind (or flux tube with larger mass flux) are steeper than those in the faster solar wind (or flux tube with smaller mass flux). More pronounced anticorrelated V p -T e is observed when the solar wind is slower and closer to the Sun.

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Association of intermittency with electron heating in the near-Sun solar wind

Phillips

Bandyopadhyay

McComas

et al. 2022

Monthly Notices of the Royal Astronomical Society: Letters

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Several studies in the near-Earth environment show that intermittent structures are important sites of energy dissipation and particle energization. Recent Parker Solar Probe (PSP) data, sampled in the near-Sun environment, have shown that proton heating is concentrated near coherent structures, suggesting local heating of protons by turbulent cascade in this region. However, whether electrons exhibit similar behavior in the near-Sun environment is not clear. Here, we address this question using PSP data collected near the Sun during the first seven orbits. We use the partial variance of increments (PVI) technique to identify coherent structures. We find that electron temperature is preferentially enhanced near strong discontinuities. Our results provide strong support for inhomogeneous heating of electrons in the ‘young’ solar wind, associated with dissipation of turbulent fluctuations near intermittent structures.

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Plasma Parameters From Quasi‐Thermal Noise Observed by Parker Solar Probe: A New Model for the Antenna Response

Cited by 3 publications

References 47 publications

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

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

Total Electron Temperature Derived from Quasi-Thermal Noise Spectroscopy In the Pristine Solar Wind: Parker Solar Probe Observations

Association of intermittency with electron heating in the near-Sun solar wind

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