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

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 hav...
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Autor*in:	R. Bandyopadhyay [verfasserIn] C. M. Meyer [verfasserIn] W. H. Matthaeus [verfasserIn] D. J. McComas [verfasserIn] S. R. Cranmer [verfasserIn] J. S. Halekas [verfasserIn] J. Huang [verfasserIn] D. E. Larson [verfasserIn] R. Livi [verfasserIn] A. Rahmati [verfasserIn] P. L. Whittlesey [verfasserIn] M. L. Stevens [verfasserIn] J. C. Kasper [verfasserIn] S. D. Bale [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics

Übergeordnetes Werk:	In: The Astrophysical Journal Letters - IOP Publishing, 2022, 955(2023), 2, p L28
Übergeordnetes Werk:	volume:955 ; year:2023 ; number:2, p L28

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/2041-8213/acf85e

Katalog-ID:	DOAJ090671945

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allfields	10.3847/2041-8213/acf85e doi (DE-627)DOAJ090671945 (DE-599)DOAJ7f2dcbfccf9a46ecaf173f66ad24076c DE-627 ger DE-627 rakwb eng QB460-466 R. Bandyopadhyay verfasserin aut Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics Astrophysics C. M. Meyer verfasserin aut W. H. Matthaeus verfasserin aut D. J. McComas verfasserin aut S. R. Cranmer verfasserin aut J. S. Halekas verfasserin aut J. Huang verfasserin aut D. E. Larson verfasserin aut R. Livi verfasserin aut A. Rahmati verfasserin aut P. L. Whittlesey verfasserin aut M. L. Stevens verfasserin aut J. C. Kasper verfasserin aut S. D. Bale verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 955(2023), 2, p L28 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:955 year:2023 number:2, p L28 https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/article/7f2dcbfccf9a46ecaf173f66ad24076c kostenfrei https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 955 2023 2, p L28
spelling	10.3847/2041-8213/acf85e doi (DE-627)DOAJ090671945 (DE-599)DOAJ7f2dcbfccf9a46ecaf173f66ad24076c DE-627 ger DE-627 rakwb eng QB460-466 R. Bandyopadhyay verfasserin aut Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics Astrophysics C. M. Meyer verfasserin aut W. H. Matthaeus verfasserin aut D. J. McComas verfasserin aut S. R. Cranmer verfasserin aut J. S. Halekas verfasserin aut J. Huang verfasserin aut D. E. Larson verfasserin aut R. Livi verfasserin aut A. Rahmati verfasserin aut P. L. Whittlesey verfasserin aut M. L. Stevens verfasserin aut J. C. Kasper verfasserin aut S. D. Bale verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 955(2023), 2, p L28 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:955 year:2023 number:2, p L28 https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/article/7f2dcbfccf9a46ecaf173f66ad24076c kostenfrei https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 955 2023 2, p L28
allfields_unstemmed	10.3847/2041-8213/acf85e doi (DE-627)DOAJ090671945 (DE-599)DOAJ7f2dcbfccf9a46ecaf173f66ad24076c DE-627 ger DE-627 rakwb eng QB460-466 R. Bandyopadhyay verfasserin aut Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics Astrophysics C. M. Meyer verfasserin aut W. H. Matthaeus verfasserin aut D. J. McComas verfasserin aut S. R. Cranmer verfasserin aut J. S. Halekas verfasserin aut J. Huang verfasserin aut D. E. Larson verfasserin aut R. Livi verfasserin aut A. Rahmati verfasserin aut P. L. Whittlesey verfasserin aut M. L. Stevens verfasserin aut J. C. Kasper verfasserin aut S. D. Bale verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 955(2023), 2, p L28 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:955 year:2023 number:2, p L28 https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/article/7f2dcbfccf9a46ecaf173f66ad24076c kostenfrei https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 955 2023 2, p L28
allfieldsGer	10.3847/2041-8213/acf85e doi (DE-627)DOAJ090671945 (DE-599)DOAJ7f2dcbfccf9a46ecaf173f66ad24076c DE-627 ger DE-627 rakwb eng QB460-466 R. Bandyopadhyay verfasserin aut Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics Astrophysics C. M. Meyer verfasserin aut W. H. Matthaeus verfasserin aut D. J. McComas verfasserin aut S. R. Cranmer verfasserin aut J. S. Halekas verfasserin aut J. Huang verfasserin aut D. E. Larson verfasserin aut R. Livi verfasserin aut A. Rahmati verfasserin aut P. L. Whittlesey verfasserin aut M. L. Stevens verfasserin aut J. C. Kasper verfasserin aut S. D. Bale verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 955(2023), 2, p L28 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:955 year:2023 number:2, p L28 https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/article/7f2dcbfccf9a46ecaf173f66ad24076c kostenfrei https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 955 2023 2, p L28
allfieldsSound	10.3847/2041-8213/acf85e doi (DE-627)DOAJ090671945 (DE-599)DOAJ7f2dcbfccf9a46ecaf173f66ad24076c DE-627 ger DE-627 rakwb eng QB460-466 R. Bandyopadhyay verfasserin aut Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier 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. Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics Astrophysics C. M. Meyer verfasserin aut W. H. Matthaeus verfasserin aut D. J. McComas verfasserin aut S. R. Cranmer verfasserin aut J. S. Halekas verfasserin aut J. Huang verfasserin aut D. E. Larson verfasserin aut R. Livi verfasserin aut A. Rahmati verfasserin aut P. L. Whittlesey verfasserin aut M. L. Stevens verfasserin aut J. C. Kasper verfasserin aut S. D. Bale verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 955(2023), 2, p L28 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:955 year:2023 number:2, p L28 https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/article/7f2dcbfccf9a46ecaf173f66ad24076c kostenfrei https://doi.org/10.3847/2041-8213/acf85e kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 955 2023 2, p L28
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callnumber-first	Q - Science
author	R. Bandyopadhyay
spellingShingle	R. Bandyopadhyay misc QB460-466 misc Solar wind misc Interplanetary physics misc Interplanetary turbulence misc Solar coronal heating misc Magnetohydrodynamics misc Astrophysics Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
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topic_title	QB460-466 Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment Solar wind Interplanetary physics Interplanetary turbulence Solar coronal heating Magnetohydrodynamics
topic	misc QB460-466 misc Solar wind misc Interplanetary physics misc Interplanetary turbulence misc Solar coronal heating misc Magnetohydrodynamics misc Astrophysics
topic_unstemmed	misc QB460-466 misc Solar wind misc Interplanetary physics misc Interplanetary turbulence misc Solar coronal heating misc Magnetohydrodynamics misc Astrophysics
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title_sort	estimates of proton and electron heating rates extended to the near-sun environment
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title_auth	Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
abstract	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.
abstractGer	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.
abstract_unstemmed	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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title_short	Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment
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Estimates of Proton and Electron Heating Rates Extended to the Near-Sun Environment

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