@Article{FranzEchSouDubZha:2017:ObVeEx,
author = "Franz, M. and Echer, Ezequiel and Souza, Adriane Marques de and
Dubinin, E. and Zhang, T. L.",
affiliation = "{Max-Planck-Institut f{\"u}r Sonnensystemforschung} and
{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Max-Planck-Institut
f{\"u}r Sonnensystemforschung} and {Space Research Institute of
the Austrian Academy of Sciences}",
title = "Ultra low frequency waves at Venus: observations by the venus
express spacecraft",
journal = "Planetary and Space Science",
year = "2017",
volume = "146",
pages = "55--65",
month = "Oct.",
keywords = "Solar wind-Venus interactionPlanetary magnetosheathsPlasma
wavesInduced magnetospheres.",
abstract = "The generation of waves with low frequencies (below 100 mHz) has
been observed in the environment of most bodies in the solar
system and well studied at Earth. These waves can be generated
either upstream of the body in the solar wind by ionization of
planetary exospheres or ions reflected from a bow shock or in the
magnetosheath closer to the magnetic barrier. For Mars and Venus
the waves may have special importance since they can contribute to
the erosion of the ionopause and by that enhance atmospheric
escape. While over the past years many case studies on wave
phenomena observed at Venus have been published most statistical
studies have been based on magnetic observations only. On the
other hand the generation mechanisms and transport of these waves
through the magnetosphere can only be quantified using both
magnetic and particle observations. We use the long time
observations of Venus Express (20062014) to determine the
predominant processes and transport parameters. First we
demonstrate the analysis methods in four case studies, then we
present a statistical analysis by determining transport ratios
from the complete Venus Express dataset. We find that Alfvenic
waves are very dominant (>80%) in the solar wind and in the core
magnetosheath. Fast waves are observed mainly at the bow shock
(around 40%) but also at the magnetic barrier where they may be
most important for the energy transfer into the ionosphere. Their
occurrence in the magnetotail may be an artifact of the detection
of individual plasma jets in this region. Slow mode waves are
rarely dominating but occur with probability of about 10% at the
bow shock and in the pile-up-region. Mirror mode waves have
probability <20% in the magnetosheath slightly increasing towards
the pile-up-boundary.",
doi = "10.1016/j.pss.2017.08.011",
url = "http://dx.doi.org/10.1016/j.pss.2017.08.011",
issn = "0032-0633",
language = "en",
targetfile = "franz_ultra.pdf",
urlaccessdate = "19 mar. 2024"
}