Anticorrelation between the Bulk Speed and the Electron Temperature in the Pristine Solar Wind: First Results from the Parker Solar Probe and Comparison with Helios

0536081 - ASÚ 2021 RIV US eng J - Článek v odborném periodiku
Maksimovic, M. - Bale, S. D. - Bercic, L. - Bonnell, J. W. - Case, A.W. - de Wit, T. D. - Goetz, K. - Halekas, J. - Harvey, P.R. - Issautier, K. - Kasper, J. C. - Korreck, K.E. - Jagarlamudi, V. K. - Lahmiti, N. - Larson, D.E. - Lecacheux, A. - Livi, R. - MacDowall, R. J. - Malaspina, D. - Martinović, M. - Meyer-Vernet, N. - Moncuquet, M. - Pulupa, M. - Salem, C. - Stevens, M.L. - Štverák, Štěpán - Velli, M. - Whittlesey, P.L.
Anticorrelation between the Bulk Speed and the Electron Temperature in the Pristine Solar Wind: First Results from the Parker Solar Probe and Comparison with Helios.
Astrophysical Journal Supplement Series. Roč. 246, č. 2 (2020), č. článku 62. ISSN 0067-0049. E-ISSN 1538-4365
Institucionální podpora: RVO:67985815
Klíčová slova: quasi-thermal noise * non-maxwellian plasmas * coronal holes
Obor OECD: Astronomy (including astrophysics,space science)
Způsob publikování: Omezený přístup
https://doi.org/10.3847/1538-4365/ab61fc

We discuss the solar wind electron temperatures T-e as measured in the nascent solar wind by Parker Solar Probe during its first perihelion pass. The measurements have been obtained by fitting the high-frequency part of quasithermal noise spectra recorded by the Radio Frequency Spectrometer. In addition we compare these measurements with those obtained by the electrostatic analyzer discussed in Halekas et al. These first electron observations show an anticorrelation between T-e and the wind bulk speed V: this anticorrelation is most likely the remnant of the wellknown mapping observed at 1 au and beyond between the fast wind and its coronal hole sources, where electrons are observed to be cooler than in the quiet corona. We also revisit Helios electron temperature measurements and show, for the first time, that an in situ (T-e, V) anticorrelation is well observed at 0.3 au but disappears as the wind expands, evolves, and mixes with different electron temperature gradients for different wind speeds.
Trvalý link: http://hdl.handle.net/11104/0313921