@Article{SouzaLJSPSMAKMRG:2017:AcRaBe,
author = "Souza, Vitor Moura and Lopez, R. E. and Jauer, Paulo Ricardo and
Sibeck, D. G. and Pham, K. and Silva, L. A. da and Marchezi,
Jos{\'e} Paulo and Alves, Livia Ribeiro and Koga, Daiki and
Medeiros, Cl{\'a}udia and Rockenbach da Silva, Marlos and
Gonzalez Alarcon, Walter Dem{\'e}trio",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {University
of Texas at Arlington} and {Instituto Nacional de Pesquisas
Espaciais (INPE)} and NASA/Goddard Space Flight Center, Greenbelt
and {West Virginia University} and {Instituto Nacional de
Pesquisas Espaciais (INPE)} and {Instituto Nacional de Pesquisas
Espaciais (INPE)} and {Instituto Nacional de Pesquisas Espaciais
(INPE)} and {Instituto Nacional de Pesquisas Espaciais (INPE)} and
{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de
Pesquisas Espaciais (INPE)}",
title = "Acceleration of radiation belt electrons and the role of the
average interplanetary magnetic field Bz component in high-speed
streams",
journal = "Journal of Geophysical Research: Space Physics",
year = "2017",
volume = "122",
pages = "10084--10101",
abstract = "In this study we examine the recovery of relativistic radiation
belt electrons on 1516 November 2014, after a previous reduction
in the electron flux resulting from the passage of a corotating
interaction region (CIR). Following the CIR, there was a period of
high-speed streams characterized by large, nonlinear fluctuations
in the interplanetary magnetic field (IMF) components. However,
the outer radiation belt electron flux remained at a low level for
several days before it increased in two major steps. The first
increase is associated with the IMF background field turning from
slightly northward on average to slightly southward on average.
The second major increase is associated with an increase in the
solar wind velocity during a period of southward average IMF
background field. We present evidence that when the IMF Bz is
negative on average, the whistler mode chorus wave power is
enhanced in the outer radiation belt, and the amplification of
magnetic integrated power spectral density in the ULF frequency
range, in the nightside magnetosphere, is more efficient as
compared to cases in which the mean IMF Bz is positive.
Preliminary analysis of the time evolution of phase space density
radial profiles did not provide conclusive evidence on which
electron acceleration mechanism is the dominant. We argue that the
acceleration of radiation belt electrons requires (i) a seed
population of keV electrons injected into the inner magnetosphere
by substorms and both (ii) enhanced whistler mode chorus waves
activity as well as (iii) large-amplitude MHD waves.",
doi = "10.1002/2017JA024187",
url = "http://dx.doi.org/10.1002/2017JA024187",
issn = "2169-9402",
language = "en",
targetfile = "souza_acceleration.pdf",
urlaccessdate = "18 abr. 2024"
}