Rosetta spacecraft influence on the mutual impedance probe frequency response in the long Debye length mode

Geiswiller, J.; Béghin, C.; Колесникова, Е. В.; Lagoutte, D.; Mīchau, J. L.; Trotignon, J. G.

doi:10.1016/s0032-0633(00)00173-2

Cited by 14 publications

(15 citation statements)

References 18 publications

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“…In this study, the plasma frequency is identified as the frequency of peak power in MIP spectra. While this is consistent with MIP models in plasma characterized by small enough Debye lengths (compared to the transmitter‐receiver distance), the plasma frequency is expected to be located below the mutual impedance spectral power peak for larger Debye length (closer to the transmitter‐receiver distance, Geiswiller et al, ; Gilet et al, . The MIP density may therefore be slightly overestimated.…”

Section: Discussionsupporting

confidence: 77%

Ion Velocity and Electron Temperature Inside and Around the Diamagnetic Cavity of Comet 67P

et al. 2018

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A major point of interest in cometary plasma physics has been the diamagnetic cavity, an unmagnetized region in the innermost part of the coma. Here we combine Langmuir and Mutual Impedance Probe measurements to investigate ion velocities and electron temperatures in the diamagnetic cavity of comet 67P, probed by the Rosetta spacecraft. We find ion velocities generally in the range 2–4 km/s, significantly above the expected neutral velocity ≲1 km/s, showing that the ions are (partially) decoupled from the neutrals, indicating that ion‐neutral drag was not responsible for balancing the outside magnetic pressure. Observations of clear wake effects on one of the Langmuir probes showed that the ion flow was close to radial and supersonic, at least with respect to the perpendicular temperature, inside the cavity and possibly in the surrounding region as well. We observed spacecraft potentials ≲−5 V throughout the cavity, showing that a population of warm (∼5 eV) electrons was present throughout the parts of the cavity reached by Rosetta. Also, a population of cold ( ≲0.11emeV) electrons was consistently observed throughout the cavity, but less consistently in the surrounding region, suggesting that while Rosetta never entered a region of collisionally coupled electrons, such a region was possibly not far away during the cavity crossings.

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Section: Discussionsupporting

confidence: 77%

Ion Velocity and Electron Temperature Inside and Around the Diamagnetic Cavity of Comet 67P

et al. 2018

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“…The results are shown in Figure : the DSCD method, which uses a sum of point charges, enables to reproduce the signal emitted by a finite‐size source. It is therefore possible to extend the computation of the mutual impedance by taking into account a non punctual probe geometry, and/or the spacecraft itself to allow to measure the interaction with the spacecraft body (Geiswiller et al, ).…”

Section: Discussionmentioning

confidence: 99%

Electrostatic Potential Radiated by a Pulsating Charge in a Two‐Electron Temperature Plasma

et al. 2017

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Mutual impedance experiments have been developed to constrain the plasma bulk properties, such as density and temperature, of ionospheric and later space plasmas, through the electric coupling between an emitter and a receiver electric antennas. So far, the analytical modeling of such instruments has enabled to treat ionospheric plasmas, where charged particles are usually well characterized by Maxwellian electron distributions. With the growth of planetary exploration, mutual impedance experiments are or will be used to constrain space plasma bulk properties. Space plasmas are usually out of local thermodynamic equilibrium; therefore, new methods to calibrate and analyze mutual impedance experiments are now required in such non‐Maxwellian plasmas. To this purpose, this work aims at modeling the electric potential generated in a two‐electron temperature plasma by a pulsating point charge. A numerical method is developed for the computation of the electrostatic potential in a sum of Maxwellian plasmas. After validating the method, the results are used to build synthetic mutual impedance spectra and quantify the effect of a warm electron population on mutual impedance experiments, in order to illustrate how the method could be applied for recent and future planetary space missions, such as Rosetta, BepiColombo, and JUICE. In particular, we show how it enables to separate the densities and temperatures of two different electron populations using in situ measurements from the RPC‐MIP mutual impedance experiment on board Rosetta.

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“…: MODELING AND TESTING CLUSTER'S ANTENNAS This linear system is closed, and the computation consists of inverting the (N q + N v )-dimensional complex matrix. The only difficulty for the code developer is to optimize the accuracy and the efficiency for a large number of elements which can be as much as several thousand in some instances [Geiswiller et al, 2001].…”

Section: Surface Charge Distribution Methodsmentioning

confidence: 99%

Modeling of Cluster's electric antennas in space: Application to plasma diagnostics

et al. 2005

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[1] The main characteristics of the long-boom electric antennas installed on board the Cluster satellites are derived from finite element modeling in a kinetic and isotropic space plasma, in the frequency range of about 1-100 kHz. The model is based on the surface charge distribution method in quasi-static conditions. The impedances of both types of antenna, i.e., the double-wire and the double-probe, are computed versus the frequency normalized with respect to the local plasma frequency and for several different Debye lengths. Most of the code outputs are checked using analytic estimations for better understanding of the involved physical mechanisms. As a by-product, the effective length of the double-probe antenna and the mutual impedance between the two antennas are computed by the code. It is shown that if it had been possible to implement such measurements on board, one would have been able not only to determine accurately the electric characteristics of the antennas but also to estimate the local plasma parameters. Nevertheless, an interesting feature predicted by the model has been checked recently in orbit by running a special mode of operation for testing the mutual impedance measurement. The preliminary results are globally consistent with the predictions, except that they suggest that our Maxwellian model for the electron distribution should be revised in order to explain the unexpected low-frequency response. After analysis of the electron flux measurements obtained simultaneously, it appears that a rough adjustment of the electron distribution with a two-component distribution allows us to account for the observations. Citation: Béghin, C., P. M. E. Décréau, J. Pickett, D. Sundkvist, and B. Lefebvre (2005), Modeling of Cluster's electric antennas in space: Application to plasma diagnostics, Radio Sci., 40, RS6008,

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Rosetta spacecraft influence on the mutual impedance probe frequency response in the long Debye length mode

Cited by 14 publications

References 18 publications

Ion Velocity and Electron Temperature Inside and Around the Diamagnetic Cavity of Comet 67P

Ion Velocity and Electron Temperature Inside and Around the Diamagnetic Cavity of Comet 67P

Electrostatic Potential Radiated by a Pulsating Charge in a Two‐Electron Temperature Plasma

Modeling of Cluster's electric antennas in space: Application to plasma diagnostics

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