The Experts below are selected from a list of 129 Experts worldwide ranked by ideXlab platform
S Fatemi - One of the best experts on this subject based on the ideXlab platform.
-
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.
-
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.
-
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.
-
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.
-
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.
-
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.
Chuji Wang - One of the best experts on this subject based on the ideXlab platform.
-
Laser spectroscopic characterization of single extraterrestrial dust particles using optical trapping-cavity ringdown and Raman spectroscopy
Journal of Quantitative Spectroscopy and Radiative Transfer, 2020Co-Authors: Haifa Alali, Zhiyong Gong, Gorden Videen, Yong-le Pan, Olga Muñoz, Chuji WangAbstract:Abstract Earth's atmosphere contains interPlanetary dust particles (IDPs), which are a key ingredient to understand Planetary Phenomena, yet the study of their physicochemical properties without external interferences at the single-particle level is limited. With the optical-trapping (OT) technique, a single dust particle can be stably trapped in air for subsequent characterization. We report on measurements of the single-particle extinction of trapped particles using cavity ringdown spectroscopy at ultraviolet wavelength around 308 nm. We also present Raman spectral features of chemical groups in individually trapped particles. Two simulants of extraterrestrial materials, (Martian and lunar analogs) along with carbon spheres and volcanic ashes were trapped and spectroscopically characterized. In addition to the on-trap measurements, the particles’ morphological and mineralogical information was obtained from off-trap measurements using scanning electron microscopy and energy dispersive spectroscopy. This study demonstrates that the integration of OT with cavity ringdown and Raman spectroscopy provides a new tool to gain multimodal information on the physicochemical properties of single IDPs with minimum to no external interferences.
Charles Lue - One of the best experts on this subject based on the ideXlab platform.
-
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.
-
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.