#FIELD ANGLE OMNIWEB FULL#

Key words: comets: individual: 67P/Churyumov-Gerasimenko / magnetic fields / plasmas / methods: data analysisĬomets are well known for their luminous tails, both the curved dust tail and the ion tail that points radially away from the Sun. The Rosetta RPC has shown that (dynamic) draping also occurs as mildly active comets, as was found at highly active comets such as 1P/Halley and 21P/Giacobini-Zinner, but also that determining both dynamic and nested draping will require a combination of fast flybys and slow excursions for future missions. There is an indication of an anticorrelation between the electron density and the magnetic field strength, which might be caused by the magnetized electrons being mirrored out of the strong field regions. The ion velocity and the magnetic field strength are correlated because the unmagnetized ions are accelerated more (less) strongly by the increasing (decreasing) magnetic field strength.

The cone-angle direction shows that mass-loading of the interplanetary magnetic field of the solar wind leads to dynamic draping. This is caused by the changing directions of the interplanetary magnetic field that is transported toward the comet. During the dayside excursion, the magnetic field cone angle changed several times, which means that the magnetic field direction changes from pointing sunward to anti-sunward. Then we studied the particle data in relation to the variations that are observed in the magnetic field. Through calculating the cone and clock angle of the magnetic field, we determined the draping pattern of the magnetic field around the nucleus of the comet.

#FIELD ANGLE OMNIWEB FULL#

The data from the full Rosetta Plasma Consortium (RPC) were used to investigate the interaction of solar wind and comet, starting from boxcar-averaged magnetic field data in order to suppress high-frequency noise in the data. The goal of this study is to describe the dynamic field line draping that takes place around the comet and the plasma processes that are connected to this. The dayside excursion was planned to move through different regions that were expected upstream of the cometary nucleus, and to possibly detect the location of the bow shock.Īims. At this time, the comet was near its most active period, and its interaction with the solar wind was expected to be at its most intense, with ion pickup and magnetic field line draping. The Rosetta dayside excursion took place in September–October 2015 when comet 67P/Churyumov-Gerasimenko (67P/CG) was located at ~1.36 AU from the Sun after it had passed perihelion on 13 August 2015 at ~1.25 AU. Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E),Ĭontext. Space Research Institute, Austrian Academy of Sciences,Į-mail: for Geophysics and Extraterrestrial Physics, Technische Universität Braunschweig, Braunschweig, Germany Edberg 4, Anders Eriksson 4, Pierre Henri 5, Kristie Llera 6, Hans Nilsson 3, Ingo Richter 2, Gabriella Stenberg Wieser 3 and Karl-Heinz Glassmeier 2 Martin Volwerk 1, Charlotte Goetz 2, Etienne Behar 3, Magda Delva 1, Niklas J. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.

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