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Title: Electron Energy Partition across Interplanetary Shocks. I. Methodology and Data Product

Abstract

Analyses of 15,314 electron velocity distribution functions (VDFs) within ±2 hr of 52 interplanetary (IP) shocks observed by the Wind spacecraft near 1 au are introduced. The electron VDFs are fit to the sum of three model functions for the cold dense core, hot tenuous halo, and field-aligned beam/strahl component. The best results were found by modeling the core as either a bi-kappa or a symmetric (or asymmetric) bi-self-similar VDF, while both the halo and beam/strahl components were best fit to bi-kappa VDF. This is the first statistical study to show that the core electron distribution is better fit to a self-similar VDF than a bi-Maxwellian under all conditions. The self-similar distribution deviation from a Maxwellian is a measure of inelasticity in particle scattering from waves and/or turbulence. The ranges of values defined by the lower and upper quartiles for the kappa exponents are κ ec ~ 5.40–10.2 for the core, κ eh ~ 3.58–5.34 for the halo, and κ eb ~ 3.40–5.16 for the beam/strahl. The lower-to-upper quartile range of symmetric bi-self-similar core exponents is s ec ~ 2.00–2.04, and those of asymmetric bi-self-similar core exponents are p ec ~ 2.20–4.00 for the parallel exponent and q ecmore » ~ 2.00–2.46 for the perpendicular exponent. The nuanced details of the fit procedure and description of resulting data product are also presented. The statistics and detailed analysis of the results are presented in Paper II and Paper III of this three-part study.« less

Authors:
ORCiD logo [1]; ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [3]; ORCiD logo [4]; ORCiD logo [5]; ORCiD logo [6]; ORCiD logo [7]; ORCiD logo [8]; ORCiD logo [9]; ORCiD logo [9]; ORCiD logo [9]; ORCiD logo [9]
  1. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States)
  2. NASA Goddard Space Flight Center (GSFC), Greenbelt, MD (United States); Univ. of Maryland, College Park, MD (United States)
  3. Univ. of Colorado, Boulder, CO (United States)
  4. Aerospace Corp., El Segundo, CA (United States)
  5. Harvard Univ., Cambridge, MA (United States)
  6. Univ. of Michigan, Ann Arbor, MI (United States)
  7. Univ. of Helsinki (Finland)
  8. Univ. of Chicago, IL (United States)
  9. Univ. of California, Berkeley, CA (United States)
Publication Date:
Research Org.:
Univ. of Maryland, College Park, MD (United States)
Sponsoring Org.:
USDOE Office of Science (SC); National Science Foundation (NSF); National Aeronautics and Space Administration (NASA)
OSTI Identifier:
1612467
Grant/Contract Number:  
SC0016278; 80NSSC18K1369; 80NSSC17K0012; AGS-1619584; AGS-1552142; NNX16AQ50G; NNX14AT26G; NNX13AI75G; NNX14AR78G; 80NSSC18K0986; NNX17AG30G; GO8-19110A; 80NSSC18K1726; 80NSSC18L1218; 1714658; NNX16AI59G; 162249; NNX16AP95G
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal. Supplement Series (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal. Supplement Series (Online); Journal Volume: 243; Journal Issue: 1; Journal ID: ISSN 1538-4365
Publisher:
American Astronomical Society/IOP
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; statistical methods; plasmas; shock waves; solar wind; sun; coronal mass ejections (CMEs)

Citation Formats

Wilson III, Lynn B., Chen, Li-Jen, Wang, Shan, Schwartz, Steven J., Turner, Drew L., Stevens, Michael L., Kasper, Justin C., Osmane, Adnane, Caprioli, Damiano, Bale, Stuart D., Pulupa, Marc P., Salem, Chadi S., and Goodrich, Katherine A. Electron Energy Partition across Interplanetary Shocks. I. Methodology and Data Product. United States: N. p., 2019. Web. https://doi.org/10.3847/1538-4365/ab22bd.
Wilson III, Lynn B., Chen, Li-Jen, Wang, Shan, Schwartz, Steven J., Turner, Drew L., Stevens, Michael L., Kasper, Justin C., Osmane, Adnane, Caprioli, Damiano, Bale, Stuart D., Pulupa, Marc P., Salem, Chadi S., & Goodrich, Katherine A. Electron Energy Partition across Interplanetary Shocks. I. Methodology and Data Product. United States. https://doi.org/10.3847/1538-4365/ab22bd
Wilson III, Lynn B., Chen, Li-Jen, Wang, Shan, Schwartz, Steven J., Turner, Drew L., Stevens, Michael L., Kasper, Justin C., Osmane, Adnane, Caprioli, Damiano, Bale, Stuart D., Pulupa, Marc P., Salem, Chadi S., and Goodrich, Katherine A. Wed . "Electron Energy Partition across Interplanetary Shocks. I. Methodology and Data Product". United States. https://doi.org/10.3847/1538-4365/ab22bd. https://www.osti.gov/servlets/purl/1612467.
@article{osti_1612467,
title = {Electron Energy Partition across Interplanetary Shocks. I. Methodology and Data Product},
author = {Wilson III, Lynn B. and Chen, Li-Jen and Wang, Shan and Schwartz, Steven J. and Turner, Drew L. and Stevens, Michael L. and Kasper, Justin C. and Osmane, Adnane and Caprioli, Damiano and Bale, Stuart D. and Pulupa, Marc P. and Salem, Chadi S. and Goodrich, Katherine A.},
abstractNote = {Analyses of 15,314 electron velocity distribution functions (VDFs) within ±2 hr of 52 interplanetary (IP) shocks observed by the Wind spacecraft near 1 au are introduced. The electron VDFs are fit to the sum of three model functions for the cold dense core, hot tenuous halo, and field-aligned beam/strahl component. The best results were found by modeling the core as either a bi-kappa or a symmetric (or asymmetric) bi-self-similar VDF, while both the halo and beam/strahl components were best fit to bi-kappa VDF. This is the first statistical study to show that the core electron distribution is better fit to a self-similar VDF than a bi-Maxwellian under all conditions. The self-similar distribution deviation from a Maxwellian is a measure of inelasticity in particle scattering from waves and/or turbulence. The ranges of values defined by the lower and upper quartiles for the kappa exponents are κ ec ~ 5.40–10.2 for the core, κ eh ~ 3.58–5.34 for the halo, and κ eb ~ 3.40–5.16 for the beam/strahl. The lower-to-upper quartile range of symmetric bi-self-similar core exponents is s ec ~ 2.00–2.04, and those of asymmetric bi-self-similar core exponents are p ec ~ 2.20–4.00 for the parallel exponent and q ec ~ 2.00–2.46 for the perpendicular exponent. The nuanced details of the fit procedure and description of resulting data product are also presented. The statistics and detailed analysis of the results are presented in Paper II and Paper III of this three-part study.},
doi = {10.3847/1538-4365/ab22bd},
journal = {The Astrophysical Journal. Supplement Series (Online)},
number = 1,
volume = 243,
place = {United States},
year = {2019},
month = {7}
}

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    Works referencing / citing this record:

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