Solar wind energy flux observations in the inner heliosphere: First results from Parker Solar Probe. (arXiv:2101.03121v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Liu_M/0/1/0/all/0/1">M. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Issautier_K/0/1/0/all/0/1">K. Issautier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_Vernet_N/0/1/0/all/0/1">N. Meyer-Vernet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moncuquet_M/0/1/0/all/0/1">M. Moncuquet</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:+Halekas_J/0/1/0/all/0/1">J. S. Halekas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">J. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Griton_L/0/1/0/all/0/1">L. Griton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bale_S/0/1/0/all/0/1">S. Bale</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnell_J/0/1/0/all/0/1">J. W. Bonnell</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:+Goetz_K/0/1/0/all/0/1">K. Goetz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harvey_P/0/1/0/all/0/1">P. R. Harvey</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:+MacDowall_R/0/1/0/all/0/1">R. J. MacDowall</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:+Pulupa_M/0/1/0/all/0/1">M. 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 investigate the solar wind energy flux in the inner heliosphere using
12-day observations around each perihelion of Encounter One (E01), Two (E02),
Four (E04), and Five (E05) of Parker Solar Probe (PSP), respectively, with a
minimum heliocentric distance of 27.8 solar radii ($R_odot{}$). Energy flux
was calculated based on electron parameters (density $n_e$, core electron
temperature $T_{c}$, and suprathermal electron temperature $T_{h}$) obtained
from the simplified analysis of the plasma quasi-thermal noise (QTN) spectrum
measured by RFS/FIELDS and the bulk proton parameters (bulk speed $V_p$ and
temperature $T_p$) measured by the Faraday Cup onboard PSP, SPC/SWEAP.
Combining observations from E01, E02, E04, and E05, the averaged energy flux
value normalized to 1 $R_odot{}$ plus the energy necessary to overcome the
solar gravitation ($W_{R_odot{}}$) is about 70$pm$14 $W m^{-2}$, which is
similar to the average value (79$pm$18 $W m^{-2}$) derived by Le Chat et al
from 24-year observations by Helios, Ulysses, and Wind at various distances and
heliolatitudes. It is remarkable that the distributions of $W_{R_odot{}}$ are
nearly symmetrical and well fitted by Gaussians, much more so than at 1 AU,
which may imply that the small heliocentric distance limits the interactions
with transient plasma structures.
We investigate the solar wind energy flux in the inner heliosphere using
12-day observations around each perihelion of Encounter One (E01), Two (E02),
Four (E04), and Five (E05) of Parker Solar Probe (PSP), respectively, with a
minimum heliocentric distance of 27.8 solar radii ($R_odot{}$). Energy flux
was calculated based on electron parameters (density $n_e$, core electron
temperature $T_{c}$, and suprathermal electron temperature $T_{h}$) obtained
from the simplified analysis of the plasma quasi-thermal noise (QTN) spectrum
measured by RFS/FIELDS and the bulk proton parameters (bulk speed $V_p$ and
temperature $T_p$) measured by the Faraday Cup onboard PSP, SPC/SWEAP.
Combining observations from E01, E02, E04, and E05, the averaged energy flux
value normalized to 1 $R_odot{}$ plus the energy necessary to overcome the
solar gravitation ($W_{R_odot{}}$) is about 70$pm$14 $W m^{-2}$, which is
similar to the average value (79$pm$18 $W m^{-2}$) derived by Le Chat et al
from 24-year observations by Helios, Ulysses, and Wind at various distances and
heliolatitudes. It is remarkable that the distributions of $W_{R_odot{}}$ are
nearly symmetrical and well fitted by Gaussians, much more so than at 1 AU,
which may imply that the small heliocentric distance limits the interactions
with transient plasma structures.
http://arxiv.org/icons/sfx.gif
