@Article{HessEcheZark:2012:SoWiPr,
author = "Hess, S. L. G. and Echer, E. and Zarka, P.",
affiliation = "LATMOS, IPSL-CNRS, Universit{\'e} Versailles-St Quentin, France
and {Instituto Nacional de Pesquisas Espaciais (INPE)} and LESIA,
Observatoire de Paris, CNRS, Univ. Paris-Diderot, Meudon, France",
title = "Solar wind pressure effects on Jupiter decametric radio emissions
independent of Io",
journal = "Planetary and Space Science",
year = "2012",
volume = "70",
number = "1",
pages = "114--125",
month = "Sept.",
keywords = "Auroral radio emissions, Electrodynamic interaction,
Interplanetary fast shocks, Jovian magnetosphere, Jupiters,
Michigan, Propagation models, Radio data, Radio emission, Solar
wind dynamic pressure, Solar wind interactions, Solar wind
pressure, Ultra-violet, Wind conditions, Decametric radio
emission, Jupiter auroral radio emission, Jupiter magnetosphere,
Solar wind.",
abstract = "This paper investigates the effects of the solar wind dynamic
pressure on Jupiter auroral radio emissions at decametric
wavelengths that are not controlled by the electrodynamic
interaction with the moon Io (non-Io DAM). In order to conduct
this study, Nanc¸ay decametric array radio data are analyzed for
the 1996-1999 period. Solar wind conditions at Jupiter's orbit are
studied using the Michigan University solar wind propagation model
(mSWiM). Interplanetary fast shocks (forward shocks, FS, or
reverse shocks, RS), and average solar wind dynamic pressure are
correlated with non-Io DAM emission occurrence, duration and
power. It is found that non-Io DAM emissions occur preferentially
during periods of enhanced solar wind dynamic pressure and after a
FS or a RS arrival at Jupiter. The dawn (non-Io B-type) and dusk
(non-Io-A-type) radio emissions are investigated separately and
show (1) a dawn-dusk asymmetry consistent with prior studies and
auroral ultraviolet (UV) observations, and (2) different behaviors
in response to solar wind shocks. Our study confirms the solar
wind control of - at least a part of - the non-Io DAM, and refines
the scenario of response of the radio emissions to the solar wind
interaction with the Jovian magnetosphere.",
doi = "10.1016/j.pss.2012.05.011;",
url = "http://dx.doi.org/10.1016/j.pss.2012.05.011;",
issn = "0032-0633",
language = "en",
urlaccessdate = "03 maio 2024"
}