A5074711585- Planetary Science and Exploration
- Astro and Planetary Science
- Solar and Space Plasma Dynamics
- Ionosphere and magnetosphere dynamics
- Earthquake Detection and Analysis
- Geomagnetism and Paleomagnetism Studies
- Laser-induced spectroscopy and plasma
- Space Satellite Systems and Control
Wuhan University
2024-2025
National Space Science Center
2022
Chinese Academy of Sciences
2022
University of Chinese Academy of Sciences
2022
Whistler mode waves are a common type of electromagnetic in the Martian induced magnetosphere. Using high‐resolution magnetic field data from Magnetometer (MAG) instrument onboard Mars Atmosphere and Volatile Evolution (MAVEN) October 2014 to November 2022, we perform detailed analysis statistical distribution occurrence rate, averaged amplitude, peak frequency, wave normal angle ellipticity left‐hand right‐hand polarized whistler Our results show that mainly...
Abstract Through the emission of high‐frequency radio waves, ground‐based heating facilities can generate Extremely‐Low‐Frequency (ELF) and Very‐Low‐Frequency (VLF) waves in ionosphere, a portion which penetrate into Earth's radiation belts influence electron population therein. Although various measurements ELF/VLF generated by ionospheric experiments have been reported, combined analysis using both observations simulations remain quite limited and, thus, underlying effects these are not...
Abstract This study delves into a Pick‐Up Ion (PUI) event captured by the Mars and Neutral Particle Analyzer aboard Tianwen‐1, revealing faster acceleration than expected within Martian magnetosheath. suggests presence of convection electric field considerably stronger that typically observed in solar wind. Through Magnetohydrodynamic simulation, we identified two regions intensified fields inner magnetosheath, prominently manifested at mid to high zenith angles (SZA = 40°–70°) X‐Z plane...
Abstract Whistler-mode waves upstream of planetary bow shock are often referred to as “1-Hz waves” due the center their observed frequency range being at ∼1 Hz. A series whistler-mode were Martian by MAVEN on 2015 August 14, with unusually low frequencies centered ∼0.4 These accompanied (though not synchronized) significant flux enhancement high-energy protons up ∼10 keV. By analyzing wave dispersion property and wave–particle interaction condition, we find that have potential resonating keV...
Abstract The mirror-mode structures in the Martian magnetosheath that were observed by Mars Atmosphere and Volatile Evolution during 2015–2018 are analyzed statistically. It is found most events occurred close to bow shock. Morphological categorization based on skewness of magnetic field shows ∼46.57% peak-like, ∼40.25% wave-like, ∼13.18% dip-like. mostly saturate a very short time after their formation near shock, which result high temperature anisotropy plasma beta at this location....
Abstract Whistler mode waves are a common type of electromagnetic in the Martian induced magnetosphere. Using high‐resolution magnetic field data from Magnetometer (MAG) instrument onboard Mars Atmosphere and Volatile Evolution (MAVEN) October 2014 to November 2022, we perform detailed analysis statistical distribution occurrence rate, averaged amplitude, peak frequency, wave normal angle ellipticity left‐hand right‐hand polarized whistler Our results show that mainly observed subsolar...
Abstract Plasmaspheric hiss plays an important role in the loss of radiation belt electrons via cyclotron resonant interactions. The cold plasma approximation is widely used evaluation hiss‐driven electron losses, which however can break down during disturbed periods geomagnetic storms and substorms. kappa particle velocity distribution, characterized by a pronounced high‐energy tail, well‐established to model profile superthermal under conditions. In present study, calculating...
Whistler-mode and ULF waves upstream of planetary bow shock play important role in energy transfer dissipation processes the environment. A series whistler-mode with their frequencies centered at ~0.4 Hz, accompanied by another ~0.04 Hz waves, were observed Martian MAVEN on 2015 August 14. During occurrence a significant flux enhancement high-energy protons up to ∼10 keV, as well response electrons also observed. The pitch angle distributions modulated differently according...
Abstract The foreshock region filled with turbulences is a natural lab for studying interactions between plasma and waves. underlying processes are vital dissipating the energy carried by solar wind into Martian environment. In this study, we analyze an ultralow-frequency wave observed on 2015 August 14 Mars Atmosphere Volatile Evolution upstream of bow shock. properties match those 30 s waves; dispersion calculation shows that was capable generating analysis ion behaviors implies generated...
Abstract Utilizing Mars Atmosphere and Volatile EvolutioN (MAVEN) observations from October 2014 to May 2023, we perform a detailed survey of magnetosonic waves generated in the solar wind (refer as upstream MS waves), with frequencies near proton gyrofrequency environment. The distribution wind‐generated has been carefully investigated, including Martian magnetosphere by propagation. results show that these are widely distributed below bow shock but more concentrated magnetic pileup...