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Title: Enhanced Energy Transfer Rate in Solar Wind Turbulence Observed near the Sun from Parker Solar Probe
Authors: Riddhi Bandyopadhyay
M. L. Goldstein
B. A. Maruca
W. H. Matthaeus
T. N. Parashar
D. Ruffolo
R. Chhiber
A. Usmanov
A. Chasapis
R. Qudsi
Stuart D. Bale
J. W. Bonnell
Thierry Dudok De Wit
Keith Goetz
Peter R. Harvey
Robert J. MacDowall
David M. Malaspina
Marc Pulupa
J. C. Kasper
K. E. Korreck
A. W. Case
M. Stevens
P. Whittlesey
D. Larson
R. Livi
K. G. Klein
M. Velli
N. Raouafi
Universite d'Orleans
University of Minnesota Twin Cities
Space Sciences Laboratory at UC Berkeley
University of California, Los Angeles
University of Michigan, Ann Arbor
University of California, Berkeley
University of Maryland, Baltimore County
Queen Mary, University of London
Johns Hopkins University Applied Physics Laboratory
Imperial College London
Mahidol University
The University of Arizona
Smithsonian Astrophysical Observatory
NASA Goddard Space Flight Center
The Bartol Research Institute
University of Colorado Boulder
Keywords: Earth and Planetary Sciences;Physics and Astronomy
Issue Date: 1-Feb-2020
Citation: Astrophysical Journal, Supplement Series. Vol.246, No.2 (2020)
Abstract: © 2020. The American Astronomical Society. All rights reserved.. Direct evidence of an inertial-range turbulent energy cascade has been provided by spacecraft observations in heliospheric plasmas. In the solar wind, the average value of the derived heating rate near 1 au is ∼103 Jkg-1s-1, an amount sufficient to account for observed departures from adiabatic expansion. Parker Solar Probe, even during its first solar encounter, offers the first opportunity to compute, in a similar fashion, a fluid-scale energy decay rate, much closer to the solar corona than any prior in situ observations. Using the Politano-Pouquet third-order law and the von Kármán decay law, we estimate the fluid-range energy transfer rate in the inner heliosphere, at heliocentric distance R ranging from 54 R o˙ (0.25 au) to 36 R o˙ (0.17 au). The energy transfer rate obtained near the first perihelion is about 100 times higher than the average value at 1 au, which is in agreement with estimates based on a heliospheric turbulence transport model. This dramatic increase in the heating rate is unprecedented in previous solar wind observations, including those from Helios, and the values are close to those obtained in the shocked plasma inside the terrestrial magnetosheath.
ISSN: 00670049
Appears in Collections:Scopus 2020

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