The Experts below are selected from a list of 237 Experts worldwide ranked by ideXlab platform
Ingrid Mann - One of the best experts on this subject based on the ideXlab platform.
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Dusty Plasma Effects in Near Earth Space and Interplanetary Medium
Space Science Reviews, 2011Co-Authors: Ingrid Mann, Asta Pellinen-wannberg, Edmond Murad, Olga Popova, Nicole Meyer-vernet, Marlene Rosenberg, Tadashi Mukai, Andrzej Czechowski, Sonoyo Mukai, Jana SafrankovaAbstract:We review dust and meteoroid fluxes and their dusty plasma effects in the Interplanetary Medium near Earth orbit and in the Earth’s ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the Interplanetary Medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process, as well as of the dust charging processes. The latter are also important for further studying nanodust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nanodust fluxes is still a challenge.
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Dusty Plasma Effects in Near Earth Space and Interplanetary Medium
Space Science Reviews, 2011Co-Authors: Ingrid Mann, Asta Pellinen-wannberg, Edmond Murad, Olga Popova, Nicole Meyer-vernet, Marlene Rosenberg, Tadashi Mukai, Andrzej Czechowski, Sonoyo Mukai, Jana SafrankovaAbstract:We review dust and meteoroid fluxes and their dusty plasma effects in the Interplanetary Medium near Earth orbit and in the Earth’s ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the Interplanetary Medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process,as well as of the dust charging processes. The latter are also important for further studying nanodust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nanodust fluxes is still a challenge.540010117 Gästprofessur Mann540010110 Driftsmedel Pellinen-Wannber
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Dust in the Interplanetary Medium
Plasma Physics and Controlled Fusion, 2010Co-Authors: Ingrid Mann, Nicole Meyer-vernet, Andrzej Czechowski, Arnaud Zaslavsky, Hervé LamyAbstract:The mass density of dust particles that form from asteroids and comets in the Interplanetary Medium of the solar system is, near 1 AU, comparable to the mass density of the solar wind. It is mainly contained in particles of micrometer size and larger. Dust and larger objects are destroyed by collisions and sublimation and hence feed heavy ions into the solar wind and the solar corona. Small dust particles are present in large number and as a result of their large charge to mass ratio deflected by electromagnetic forces in the solar wind. For nano dust particles of sizes 1 - 10 nm, recent calculations show trapping near the Sun and outside from about 0.15 AU ejection with velocities close to solar wind velocity. The fluxes of ejected nano dust are detected near 1AU with the plasma wave instrument onboard the STEREO spacecraft. Though such electric signals have been observed during dust impacts before, the interpretation depends on several different parameters and data analysis is still in progress.
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dust in the Interplanetary Medium interactions with the solar wind
Twelfth International Solar Wind Conference, 2010Co-Authors: Ingrid Mann, A Czechowski, N MeyervernetAbstract:We discuss cosmic dust in the Interplanetary Medium focusing on its interaction with the solar wind and recent observational results related to such interactions. The dust contributes to pick‐up ions in the solar wind and dust collisional vaporization can explain the observed heavy inner source pick‐up ions, as well as the presence of molecular ions. We predict that ions generated by dust destruction inside 0.1 AU are multiply charged in the solar wind near 1 AU. The mass loading of the solar wind during passage of cometary dust trails appears too small to explain the Interplanetary field enhancements that are observed in solar wind magnetic field measurements. Nano dust in the Interplanetary Medium can be efficiently accelerated in the solar wind and hypervelocity impacts of nano dust onto the spacecraft can explain frequent events measured with the plasma instrument onboard STEREO.
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Interplanetary Medium a dusty plasma
Advances in Space Research, 2008Co-Authors: Ingrid MannAbstract:The average mass of dust per volume in space equals that of the solar wind so that the Interplanetary Medium should provide an obvious region to study dust plasma interactions. While dust collective behavior is typically not observed in the Interplanetary Medium, the dust component rather consists of isolated grains screened by and interacting with the plasma. Space measurements have revealed several phenomena possibly resulting from dust plasma interactions, but most of the dust plasma interactions are at present not quantified. Examples are the production of neutrals and pick-up ions from the dust, dust impact generated field variations at spacecraft and magnetic field variations possibly caused by solar wind interacting with dust trails. Since dust particles carry a surface charge, they are exposed to the Lorentz force in the Interplanetary magnetic field and for grains of sub-micrometer sizes acceleration can be substantial.
Paola Ballatore - One of the best experts on this subject based on the ideXlab platform.
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Comment on: Effects of fast and slow solar wind on the correlation between Interplanetary Medium and geomagnetic activity. Author's reply
Journal of Geophysical Research, 2003Co-Authors: C. B. Wang, J. K. Chao, Paola BallatoreAbstract:Ballatore [2002] has investigated the correlations between the Interplanetary Medium and the geomagnetic indices Kp and Dst for different ranges of solar wind speed. She found that the correlation coefficients obtained for data points corresponding to a solar wind slower than 550 km s -1 are equal to or slightly higher than the global correlations. The observations show generally lower correlation coefficients for solar wind speeds greater than 550 km s -1 . From these results she verified that at high solar wind speeds the processes responsible for the energy transfer between the Interplanetary Medium and the magnetosphere saturate. We have recalculated the correlation coefficients using the most recent OMNI data and found, contrary to her results, that the global correlation coefficients between Kp, Dst, and the Interplanetary parameters are generally higher than the correlations obtained for data points corresponding to different solar wind speed intervals. From statistical tests we demonstrate that the correlations for solar wind speeds greater than 550 km s -1 are not significantly different from the correlations in other solar wind speed intervals. There is insufficient evidence to show that, from an investigation of the correlation coefficients between the Interplanetary Medium and the geomagnetic indices Kp and Dst, a threshold exists at a solar wind speed of ∼550 km s -1 for the coupling of the Interplanetary-magnetosphere system. This conclusion is also supported by analysis of the correlations between the time derivation of Dst and the Interplanetary Medium.
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Effects of fast and slow solar wind on the correlations between Interplanetary Medium and geomagnetic activity
Journal of Geophysical Research, 2002Co-Authors: Paola BallatoreAbstract:[1] The coupling between Interplanetary parameters and geomagnetic activity has been investigated. In particular, the correlations between the Interplanetary Medium and the geomagnetic indices Kp and Dst have been calculated for different ranges of solar wind speed. The correlation coefficients obtained for data points corresponding to solar wind slower than 550 km/s are equal or slightly higher than the global correlations. The observations show generally lower correlation coefficients for solar wind speeds faster than 550 km/s. These results suggest that at high solar wind speeds the processes responsible for the energy transfer between the Interplanetary Medium and the magnetosphere saturate. In addition, the influence of internal magnetospheric plasma physics on the geomagnetic activity may be larger for the faster solar wind intervals. In the context of the deterministically chaotic approximations we discuss how the threshold at ∼550 km/s might represent the break of the order in the Interplanetary-geomagnetic coupling system, so that the linear correlations or the correlations with a relatively weak departure from linearity are significant mostly during the slower solar wind.
Nicole Meyer-vernet - One of the best experts on this subject based on the ideXlab platform.
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Effect of the Interplanetary Medium on Nanodust Observations by the Solar Terrestrial Relations Observatory
Solar Physics, 2015Co-Authors: G. Le Chat, Nicole Meyer-vernet, Karine Issautier, A. Zaslavsky, Filippo Pantellini, S. Belheouane, Milan MaksimovicAbstract:Dust particles provide an important part of the matter composing the Interplanetary Medium; their mass flux at 1 AU is similar to that of the solar wind. Dust grains of nanometer size-scale can be detected using radio and plasma wave instruments because they move at roughly the solar wind speed. The high-velocity impact of a dust particle generates a small crater on the spacecraft: the dust particle and the crater material are vaporized. This produces a plasma cloud whose associated electrical charge induces an electric pulse measured with radio and plasma instruments. Since their first detection in the Interplanetary Medium, nanodust particles have been routinely measured using the Solar Terrestrial Relations Observatory/WAVES experiment [S/WAVES]. We present the nanodust properties measured using S/WAVES/Low Frequency Receiver [LFR] observations between 2007 and 2013, and for the first time present evidence of coronal mass ejection interaction with the nanodust, leading to a higher nanodust flux measured at 1 AU. Finally, possible influences of the inner planets on the nanodust flux are presented and discussed.
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Dusty Plasma Effects in Near Earth Space and Interplanetary Medium
Space Science Reviews, 2011Co-Authors: Ingrid Mann, Asta Pellinen-wannberg, Edmond Murad, Olga Popova, Nicole Meyer-vernet, Marlene Rosenberg, Tadashi Mukai, Andrzej Czechowski, Sonoyo Mukai, Jana SafrankovaAbstract:We review dust and meteoroid fluxes and their dusty plasma effects in the Interplanetary Medium near Earth orbit and in the Earth’s ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the Interplanetary Medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process, as well as of the dust charging processes. The latter are also important for further studying nanodust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nanodust fluxes is still a challenge.
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Dusty Plasma Effects in Near Earth Space and Interplanetary Medium
Space Science Reviews, 2011Co-Authors: Ingrid Mann, Asta Pellinen-wannberg, Edmond Murad, Olga Popova, Nicole Meyer-vernet, Marlene Rosenberg, Tadashi Mukai, Andrzej Czechowski, Sonoyo Mukai, Jana SafrankovaAbstract:We review dust and meteoroid fluxes and their dusty plasma effects in the Interplanetary Medium near Earth orbit and in the Earth’s ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the Interplanetary Medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process,as well as of the dust charging processes. The latter are also important for further studying nanodust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nanodust fluxes is still a challenge.540010117 Gästprofessur Mann540010110 Driftsmedel Pellinen-Wannber
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Dust in the Interplanetary Medium
Plasma Physics and Controlled Fusion, 2010Co-Authors: Ingrid Mann, Nicole Meyer-vernet, Andrzej Czechowski, Arnaud Zaslavsky, Hervé LamyAbstract:The mass density of dust particles that form from asteroids and comets in the Interplanetary Medium of the solar system is, near 1 AU, comparable to the mass density of the solar wind. It is mainly contained in particles of micrometer size and larger. Dust and larger objects are destroyed by collisions and sublimation and hence feed heavy ions into the solar wind and the solar corona. Small dust particles are present in large number and as a result of their large charge to mass ratio deflected by electromagnetic forces in the solar wind. For nano dust particles of sizes 1 - 10 nm, recent calculations show trapping near the Sun and outside from about 0.15 AU ejection with velocities close to solar wind velocity. The fluxes of ejected nano dust are detected near 1AU with the plasma wave instrument onboard the STEREO spacecraft. Though such electric signals have been observed during dust impacts before, the interpretation depends on several different parameters and data analysis is still in progress.
Jana Safrankova - One of the best experts on this subject based on the ideXlab platform.
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Dusty Plasma Effects in Near Earth Space and Interplanetary Medium
Space Science Reviews, 2011Co-Authors: Ingrid Mann, Asta Pellinen-wannberg, Edmond Murad, Olga Popova, Nicole Meyer-vernet, Marlene Rosenberg, Tadashi Mukai, Andrzej Czechowski, Sonoyo Mukai, Jana SafrankovaAbstract:We review dust and meteoroid fluxes and their dusty plasma effects in the Interplanetary Medium near Earth orbit and in the Earth’s ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the Interplanetary Medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process, as well as of the dust charging processes. The latter are also important for further studying nanodust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nanodust fluxes is still a challenge.
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Dusty Plasma Effects in Near Earth Space and Interplanetary Medium
Space Science Reviews, 2011Co-Authors: Ingrid Mann, Asta Pellinen-wannberg, Edmond Murad, Olga Popova, Nicole Meyer-vernet, Marlene Rosenberg, Tadashi Mukai, Andrzej Czechowski, Sonoyo Mukai, Jana SafrankovaAbstract:We review dust and meteoroid fluxes and their dusty plasma effects in the Interplanetary Medium near Earth orbit and in the Earth’s ionosphere. Aside from in-situ measurements from sounding rockets and spacecraft, experimental data cover radar and optical observations of meteors. Dust plasma interactions in the Interplanetary Medium are observed by the detection of charged dust particles, by the detection of dust that is accelerated in the solar wind and by the detection of ions and neutrals that are released from the dust. These interactions are not well understood and lack quantitative description. There is still a huge discrepancy in the estimates of meteoroid mass deposition into the atmosphere. The radar meteor observations are of particular interest for determining this number. Dust measurements from spacecraft require a better understanding of the dust impact ionization process,as well as of the dust charging processes. The latter are also important for further studying nanodust trajectories in the solar wind. Moreover understanding of the complex dependencies that cause the variation of nanodust fluxes is still a challenge.540010117 Gästprofessur Mann540010110 Driftsmedel Pellinen-Wannber
M. J. Reiner - One of the best experts on this subject based on the ideXlab platform.
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on the deceleration of cmes in the corona and Interplanetary Medium deduced from radio and white light observations
SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference, 2003Co-Authors: M. J. Reiner, M. L. Kaiser, J.‐l. BougeretAbstract:It is generally acknowledged that CMEs, especially the faster ones, must deceleration somewhere between the high corona and Interplanetary Medium. However, the detailed characteristics and spatial region over which this deceleration occurs is still largely unknown. Simultaneous radio and white‐light observations can provide information on the speed profiles of the CME or CME/shock in the high corona and/or Interplanetary Medium. These observations are consistent with constant deceleration for most CMEs. From the theoretical or modelling point of view, it is usually assumed that the deceleration of CMEs is due to a drag term, which is usually taken to be proportional to the relative speed of the CME compared to that of the solar wind or to this relative speed squared. We point out that such a form for the drag force on the CME inevitably leads to speed profiles that are inconsistent with both the radio and white‐light observations.
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On the Deceleration of CMEs in the Corona and Interplanetary Medium deduced from Radio and White‐Light Observations
AIP Conference Proceedings, 2003Co-Authors: M. J. Reiner, M. L. Kaiser, J.‐l. BougeretAbstract:It is generally acknowledged that CMEs, especially the faster ones, must deceleration somewhere between the high corona and Interplanetary Medium. However, the detailed characteristics and spatial region over which this deceleration occurs is still largely unknown. Simultaneous radio and white‐light observations can provide information on the speed profiles of the CME or CME/shock in the high corona and/or Interplanetary Medium. These observations are consistent with constant deceleration for most CMEs. From the theoretical or modelling point of view, it is usually assumed that the deceleration of CMEs is due to a drag term, which is usually taken to be proportional to the relative speed of the CME compared to that of the solar wind or to this relative speed squared. We point out that such a form for the drag force on the CME inevitably leads to speed profiles that are inconsistent with both the radio and white‐light observations.
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radio signatures of the origin and propagation of coronal mass ejections through the solar corona and Interplanetary Medium
Journal of Geophysical Research, 2001Co-Authors: M. J. Reiner, M. L. Kaiser, J L BougeretAbstract:During a 16-day period from February 5 to 20, 2000, a series of decametric-to-kilometric wavelength type II and type III radio events was observed by the WAVES radio experiment on board the Wind spacecraft. These radio events were related to observed coronal mass ejections (CMEs) and their associated flares. Each of the solar eruptive events was initiated by an intense, complex type III radio burst, which occurred within minutes of the liftoff on the CME. Some of the CMEs produced decametric-hectometric (D-H) type II radio emissions, which, when their frequency drift rates were sufficiently well defined, were used to provide a speed estimate. The complex type III and D-H type II radio emissions gave an indication of the presence of a CME well before the CME was first observed in the coronagraph images. This series of CMEs also generated Interplanetary (kilometric) type II radio emissions that tracked the CME-associated shock through the Interplanetary Medium and established the terrestrial connection. Thus the various radio emissions associated with these solar eruptive events provided a global view of each entire Sun-Earth connection event, from the initiation and liftoff of the CME at the Sun, to the propagation of the CME-associated shock through the solar corona and Interplanetary Medium, to its arrival at 1 AU. Finally, we show that simultaneous Wind/Ulysses observations of the Interplanetary type II radio emissions on February 9–10 provide important information on the nature of the type II emission, on the type II source locations, and on the radiation characteristics of the type II emissions. For example, these simultaneous observations clearly indicate that the sporadic nature of the type II radiation was intrinsic to the radio source region.
