Electron heat flux in the near-Sun environment. (arXiv:2010.10302v1 [astro-ph.SR])

Electron heat flux in the near-Sun environment. (arXiv:2010.10302v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Halekas_J/0/1/0/all/0/1">J. S. Halekas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whittlesey_P/0/1/0/all/0/1">P. L. Whittlesey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larson_D/0/1/0/all/0/1">D. E. Larson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGinnis_D/0/1/0/all/0/1">D. McGinnis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bale_S/0/1/0/all/0/1">S. D. Bale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berthomier_M/0/1/0/all/0/1">M. Berthomier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Case_A/0/1/0/all/0/1">A. W. Case</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chandran_B/0/1/0/all/0/1">B. D. G. Chandran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasper_J/0/1/0/all/0/1">J. C. Kasper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klein_K/0/1/0/all/0/1">K. G. Klein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korreck_K/0/1/0/all/0/1">K. E. Korreck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Livi_R/0/1/0/all/0/1">R. Livi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacDowall_R/0/1/0/all/0/1">R. J. MacDowall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maksimovic_M/0/1/0/all/0/1">M. Maksimovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malaspina_D/0/1/0/all/0/1">D. M. Malaspina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matteini_L/0/1/0/all/0/1">L. Matteini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pulupa_M/0/1/0/all/0/1">M. P. Pulupa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevens_M/0/1/0/all/0/1">M. L. Stevens</a>

We survey the electron heat flux observed by the Parker Solar Probe (PSP) in
the near-Sun environment at heliocentric distances of 0.125-0.25 AU. We
utilized measurements from the Solar Wind Electrons Alphas and Protons and
FIELDS experiments to compute the solar wind electron heat flux and its
components and to place these in context. The PSP observations reveal a number
of trends in the electron heat flux signatures near the Sun. The magnitude of
the heat flux is anticorrelated with solar wind speed, likely as a result of
the lower saturation heat flux in the higher-speed wind. When divided by the
saturation heat flux, the resulting normalized net heat flux is anticorrelated
with plasma beta on all PSP orbits, which is consistent with the operation of
collisionless heat flux regulation mechanisms. The net heat flux also decreases
in very high beta regions in the vicinity of the heliospheric current sheet,
but in most cases of this type the omnidirectional suprathermal electron flux
remains at a comparable level or even increases, seemingly inconsistent with
disconnection from the Sun. The measured heat flux values appear inconsistent
with regulation primarily by collisional mechanisms near the Sun. Instead, the
observed heat flux dependence on plasma beta and the distribution of
suprathermal electron parameters are both consistent with theoretical
instability thresholds associated with oblique whistler and magnetosonic modes.

We survey the electron heat flux observed by the Parker Solar Probe (PSP) in
the near-Sun environment at heliocentric distances of 0.125-0.25 AU. We
utilized measurements from the Solar Wind Electrons Alphas and Protons and
FIELDS experiments to compute the solar wind electron heat flux and its
components and to place these in context. The PSP observations reveal a number
of trends in the electron heat flux signatures near the Sun. The magnitude of
the heat flux is anticorrelated with solar wind speed, likely as a result of
the lower saturation heat flux in the higher-speed wind. When divided by the
saturation heat flux, the resulting normalized net heat flux is anticorrelated
with plasma beta on all PSP orbits, which is consistent with the operation of
collisionless heat flux regulation mechanisms. The net heat flux also decreases
in very high beta regions in the vicinity of the heliospheric current sheet,
but in most cases of this type the omnidirectional suprathermal electron flux
remains at a comparable level or even increases, seemingly inconsistent with
disconnection from the Sun. The measured heat flux values appear inconsistent
with regulation primarily by collisional mechanisms near the Sun. Instead, the
observed heat flux dependence on plasma beta and the distribution of
suprathermal electron parameters are both consistent with theoretical
instability thresholds associated with oblique whistler and magnetosonic modes.

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