The Incompressible Magnetohydrodynamic Energy Cascade Rate Upstream of Mars: Effects of the Total Energy and the Cross-helicity on Solar Wind Turbulence

Norberto Romanelli; Nahuel Andrés; Gina A. DiBraccio; Jaye L. Verniero; Jacob R. Gruesbeck; Adam Szabo; Jared R. Espley; Jasper S. Halekas

doi:10.3847/1538-4357/ad58b5

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The Incompressible Magnetohydrodynamic Energy Cascade Rate Upstream of Mars: Effects of the Total Energy and the Cross-helicity on Solar Wind Turbulence

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The Incompressible Magnetohydrodynamic Energy Cascade Rate Upstream of Mars: Effects of the Total Energy and the Cross-helicity on Solar Wind Turbulence

Norberto Romanelli, Nahuel Andrés, Gina A. DiBraccio, Jaye L. Verniero, Jacob R. Gruesbeck, Adam Szabo, Jared R. Espley and Jasper S. Halekas

The Astrophysical journal, Vol.971(1), 10

08/01/2024

DOI: 10.3847/1538-4357/ad58b5

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Abstract

Abstract Solar wind turbulence is a dynamical phenomenon that evolves with heliocentric distance. Orbiting Mars since 2014 September, Mars Atmosphere and Volatile EvolutioN offers a unique opportunity to explore some of its main properties beyond ∼1.38 au. Here, we analyze solar wind turbulence upstream of Mars' bow shock, utilizing more than 5 years of magnetic field and plasma measurements. This analysis is based on two complementary methodologies: (1) the computation of magnetohydrodynamic (MHD) invariants characterizing incompressible fluctuations; (2) the estimation of the incompressible energy cascade rate at MHD scales (i.e., 〈 ε T 〉 MHD ). Our results show the solar wind incompressible fluctuations are primarily in a magnetically dominated regime, with the component traveling away from the Sun having a higher median pseudoenergy. Moreover, turbulent fluctuations have a total energy per mass of up to ∼ 300 km 2 s −2 , a range smaller than reported at 1 au. For these conditions, we determine the probability distribution function of 〈 ε T 〉 MHD ranges mainly between ∼ −1 × 10 −16 and ∼1 × 10 −16 J m −3 s −1 , with a median equal to −1.8 × 10 −18 J m −3 s −1 , suggesting back transfer of energy. Our results also suggest that ∣〈 ε T 〉 MHD ∣ is correlated with the total energy per mass of fluctuations and that the median of 〈 ε T 〉 MHD does not vary significantly with the cross-helicity. We find, however, that the medians of the inward and outward pseudoenergy cascade rates vary with the solar wind cross-helicity. Finally, we discuss these results and their implications for future studies that can provide further insight into the factors affecting the solar wind energy transfer rate.

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Title: Subtitle: The Incompressible Magnetohydrodynamic Energy Cascade Rate Upstream of Mars: Effects of the Total Energy and the Cross-helicity on Solar Wind Turbulence
Creators: Norberto Romanelli
Nahuel Andrés
Gina A. DiBraccio
Jaye L. Verniero
Jacob R. Gruesbeck
Adam Szabo
Jared R. Espley
Jasper S. Halekas
Resource Type: Journal article
Publication Details: The Astrophysical journal, Vol.971(1), 10
Publisher: IOP Publishing Ltd
DOI: 10.3847/1538-4357/ad58b5
ISSN: 0004-637X
eISSN: 1538-4357
Grant note: University of Maryland College Park: 80GSFC21M0002 NASA Goddard Space Flight Center: 80GSFC21M0002
The MAVEN project is supported by NASA through the Mars Exploration Program. N.R. is supported through a cooperative agreement with the Center for Research and Exploration in Space Sciences & Technology II (CRESST II) between NASA Goddard Space Flight Center and University of Maryland College Park under award No. 80GSFC21M0002. MAVEN data are publicly available through the Planetary Data System (https://pds-ppi.igpp.ucla.edu/index.jsp).
Language: English
Date published: 08/01/2024
Academic Unit: Physics and Astronomy
Record Identifier: 9984696759402771

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