The Experts below are selected from a list of 243 Experts worldwide ranked by ideXlab platform
S Fatemi - One of the best experts on this subject based on the ideXlab platform.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies reflected lunar protons
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or back-streaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the un-magnetized surface reflects between 0.1-1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward-Scattering at solar zenith angles near 90° . Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or backstreaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS (Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun) observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the unmagnetized surface reflects between 0.1 and 1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward Scattering at solar zenith angles near 90°. Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
A R Poppe - One of the best experts on this subject based on the ideXlab platform.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies reflected lunar protons
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or back-streaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the un-magnetized surface reflects between 0.1-1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward-Scattering at solar zenith angles near 90° . Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or backstreaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS (Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun) observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the unmagnetized surface reflects between 0.1 and 1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward Scattering at solar zenith angles near 90°. Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
J S Halekas - One of the best experts on this subject based on the ideXlab platform.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies reflected lunar protons
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or back-streaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the un-magnetized surface reflects between 0.1-1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward-Scattering at solar zenith angles near 90° . Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or backstreaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS (Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun) observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the unmagnetized surface reflects between 0.1 and 1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward Scattering at solar zenith angles near 90°. Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
Charles Lue - One of the best experts on this subject based on the ideXlab platform.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies reflected lunar protons
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or back-streaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the un-magnetized surface reflects between 0.1-1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward-Scattering at solar zenith angles near 90° . Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
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artemis observations of the solar wind proton Scattering Function from lunar crustal magnetic anomalies
Journal of Geophysical Research, 2017Co-Authors: A R Poppe, J S Halekas, Charles Lue, S FatemiAbstract:Despite their small scales, lunar crustal magnetic fields are routinely associated with observations of reflected and/or backstreaming populations of solar wind protons. Solar wind proton reflection locally reduces the rate of space weathering of the lunar regolith, depresses local sputtering rates of neutrals into the lunar exosphere, and can trigger electromagnetic waves and small-scale collisionless shocks in the near-lunar space plasma environment. Thus, knowledge of both the magnitude and Scattering Function of solar wind protons from magnetic anomalies is crucial in understanding a wide variety of planetary phenomena at the Moon. We have compiled 5.5 years of ARTEMIS (Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun) observations of reflected protons at the Moon and used a Liouville tracing method to ascertain each proton's reflection location and Scattering angles. We find that solar wind proton reflection is largely correlated with crustal magnetic field strength, with anomalies such as South Pole/Aitken Basin (SPA), Mare Marginis, and Gerasimovich reflecting on average 5-12% of the solar wind flux while the unmagnetized surface reflects between 0.1 and 1% in charged form. We present the Scattering Function of solar wind protons off of the SPA anomaly, showing that the Scattering transitions from isotropic at low solar zenith angles to strongly forward Scattering at solar zenith angles near 90°. Such Scattering is consistent with simulations that have suggested electrostatic fields as the primary mechanism for solar wind proton reflection from crustal magnetic anomalies.
Han Vu Thien - One of the best experts on this subject based on the ideXlab platform.
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A New Theoretical Approach of Wavelet-Based Multifractal Characterization of HF Channel Scattering Function: Theoretical and Physical Interpretations
IEEE Transactions on Geoscience and Remote Sensing, 2012Co-Authors: Ali Dziri, C. Goutelard, Abderrazek Abdaoui, Han Vu ThienAbstract:In high-frequency (HF) ionospheric communications, the dynamic nature of the high-latitude ionosphere creates small-scale ionospheric irregularities capable of Scattering HF radio waves. In addition, there are large-scale irregularities which may be identified using some specific methods. However, small-scale irregularities cannot be easily identified and characterized. The aim of this paper is to introduce a new wavelet-based multifractal dimension mapping approach for the identification and the quantification of the small-scale irregularities. Numerical results show the improvement of the proposed methods compared to those obtained by the classical Legendre multifractal analysis. In our analysis, we have used the Scattering Function as a tool for the HF channel characterization. Our analysis deals with experimental Scattering Functions measured during the solar eclipse on August 11, 1999.
