Jun Cui

Sun Yat-sen University

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Jiang Yu

Sun Yat-sen University

Yong Wei

Institute of Geology and Geophysics

Jinbin Cao

Beihang University

Jing Wang

Sun Yat-sen University

R. V. Yelle

University of Arizona

Zhaopeng Wu

Chinese Academy of Sciences

Zhiyong Xiao

Sun Yat-sen University

Zhaoguo He

Macau University of Science and Technology

Y. Cao

Chinese Academy of Sciences

Jiahao Zhong

Sun Yat-sen University

Cooperative Institutions

Chinese Academy of Sciences

174

University of Chinese Academy of Sciences

Sun Yat-sen University

Institute of Geology and Geophysics

University of Science and Technology of China

National Space Science Center

National Astronomical Observatories

Planetary Science Institute

Macau University of Science and Technology

Beijing University of Chemical Technology

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The Ionosphere at Middle and Low Latitudes Under Geomagnetic Quiet Time of December 2019

Journal of Geophysical Research Space Physics (2021)

Jiawei Kuai Qiaoling Li Jiahao Zhong Xu Zhou Libo Liu

Abstract The ionospheric electron density shows remarkable day‐to‐day variability due to solar radiance, geomagnetic activity and lower atmosphere forcing. In this report, we investigated the ionospheric variations at middle and low latitudes during a period under geomagnetic quiet time ( Kp max = 1.7) from November 30 to December 8, 2019. During the quiescent period, the ionosphere is not undisturbed as expected in the Asian‐Australian and the American sectors. Total electron content (TEC) has multiple prominent enhancements at middle and low latitudes in the two sectors, and TEC depletions also occur repeatedly in the Asian‐Australian sector. The low‐latitude electric fields vary significantly, which is likely to be modulated by the notably changing tides in the mesosphere and lower thermosphere region. It is worth noting that the variations of TEC and the electric fields are not consistent in the two sectors, particularly on December 4–6. Further investigation reveals that the increase in TEC depends on altitude. The TEC enhancements are mainly contributed by the altitude below 500 km in both two sectors, which indirectly reflects that the driving sources may come from the lower atmosphere. Especially, a mid‐latitude band structure continuously appears at all local times in the North American sector on December 6–8, which is also mainly contributed by the altitude below 500 km.

Middle latitudes

Geomagnetic latitude

QUIET

10.1029/2020ja028964

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Citations (14)

Lost Volatiles During the Formation of Hollows on Mercury

Journal of Geophysical Research Planets (2020)

Yichen Wang Zhiyong Xiao Yiren Chang Jun Cui

Abstract Hollows are the key to understand the composition and evolution of volatiles in the planet Mercury. A fundamental question about the formation mechanism of hollows is the true reflectance spectra of the possible volatile compounds. We use the high‐resolution images and reflectance spectra returned by the MESSENGER spacecraft to investigate the nature and origin of hollows on Mercury. Hollows are divided as different geomorphological facies according to their morphology and possible degree of devolatilization, and reflectance spectra for different facies of hollows are extracted. Large sample analyses reveal that the spectra of hollow floors and background terrains are the two end‐members, whose mixtures can account for the observed wide ranges of reflectance spectra of hollows. Spectral analyses favor that carbon might be a volatile compound that formed hollows, although direct spectral observations for the hollow‐forming volatiles are prohibited because volatiles are mainly lost from steep hollow walls. The initiation and growth of hollows are controlled by structural heterogeneities in the subsurface, such as widespread cooling fractures that were developed in melt sheets of complex craters. A maximum model age of 103 (+200, −96) thousand years is derived for the global population of hollows, yielding an average growth rate >1,000 times that of previous estimations. Based on the geometry of the different morphological facies of all visible hollows on Mercury, the conservation of mass predicts a minimum volume of lost volatiles of 1,266 km 3 . We predict that an active rejuvenation of volatiles has occurred in the shallow crust of Mercury.

Mercury

10.1029/2020je006559

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Citations (16)

Martian Proton Aurora Brightening Reveals Atmospheric Ion Loss Intensifying

Geophysical Research Letters (2023)

Fei He Kai Fan A. C. G. Hughes Yong Wei Jun Cui

Abstract The Martian proton aurora is a distinct aurora phenomenon resulting from the direct deposition of solar wind energy into Mars' dayside atmosphere. What solar wind parameters influence the aurora activity in the short term is yet unknown, as are the associated repercussions in the Martian atmospheric ion loss. Here we present observational evidence of synchronized proton aurora brightening and atmospheric ion loss intensifying on Mars, controlled by solar wind dynamic pressure, using observations by the Mars Atmosphere and Volatile Evolution spacecraft. The solar wind dynamic pressure possibly has a saturation effect on brightening proton aurora. Significant erosion of the Martian ionosphere during periods of high dynamic pressure indicates at least five‐to‐tenfold increase in atmospheric ion loss. An empirical relationship between ion escape rate and auroral emission enhancement is established, providing a new proxy of Mars' atmospheric ion loss with optical imaging that may be used remotely and with greater flexibility.

Atmosphere of Mars

Atmospheric escape

Dynamic pressure

10.1029/2023gl102723

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Topographic Gravity Waves Observed in the Martian Thermosphere: A Statistical Perspective From a 1‐D Full‐Wave Model

Journal of Geophysical Research Space Physics (2022)

Jianping Huang Zhaopeng Wu Jun Cui Yongqiang Hao Wei Cao

Abstract Gravity waves (GWs) are significant dynamical processes in planetary atmospheres due to their efficient transport of momentum and energy from the lower to the upper atmosphere. Recent observations from in‐situ measurements by spacecraft like Mars Atmosphere and Volatile Evolution (MAVEN) also reveal ubiquitous GW activity in the Martian thermosphere. As a critical parameter for characterizing GWs, the wavelength spectrum has been studied for years. However, most of the current observations for the Martian thermosphere can only determine the apparent GW wavelength because they usually take one‐dimensional measurements within a typical GW period. In this work, we adopt a full‐wave GW model to statistically investigate the upward propagation of the topographic‐generated GWs and how their wavelength spectrum apparently looks in the thermosphere when observed by a spacecraft like MAVEN. We find that the wind significantly modifies the vertical wavelengths of GWs in the Martian atmosphere. Considering the GWs generated from topographic sources, we calculate their wavelength distribution in the thermosphere, with a most probable apparent vertical wavelength of around 14 km, consisting with the MAVEN observation. However, our theoretical wavelength spectrum is mainly concentrated in the low wavelength part (10–20 km), while the observed result contains a long‐tailed component in the long wavelength part. The mismatch between our model and observations indicates that at least 72% of the observed GWs in the thermosphere are not generated from topographic sources.

Atmosphere of Mars

10.1029/2022ja030846

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Citations (7)

Empirical Models of Ion Density Distribution in the Dayside Martian Ionosphere

Journal of Geophysical Research Space Physics (2021)

Jianping Huang Y. Cao Jun Cui Yongqiang Hao Xiaoshu Wu

Abstract With the aid of the recent Neutral Gas and Ion Mass Spectrometer (NGIMS) measurements made onboard the Mars Atmosphere and Volatile Evolution spacecraft, we construct empirical models for the vertical density distributions of 12 species in the dayside Martian ionosphere over the altitude range of 150–450 km, from abundant species such as , , and O + to trace species such as and OCOH + . Two different sets of formulism are proposed to parameterize the ion density distribution characterized either by a distinctive layer structure or by a near exponential decay above 150 km. Both the solar control and magnetic control of ion distribution are taken into account in our modelings. In general, our empirical models are in good agreement with the NGIMS measurements. The full set of parameters constrained by data‐model comparison is tabulated for reference. This allows the easy computation of any individual ion density profile for a unique combination of solar zenith angle, solar extreme ultraviolet flux, and ambient magnetic elevation, which in turn facilitates comparisons with photochemical model results. The empirical models reported in this study are an extension of previous empirical models constructed for the electron distribution in the dayside Martian ionosphere using both radar sounding and radio occultation data.

Solar zenith angle

Radio occultation

10.1029/2021ja029226

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The Relationship Between Photoelectron Boundary and Steep Electron Density Gradient on Mars: MAVEN Observations

Journal of Geophysical Research Space Physics (2019)

Qianqian Han Kai Fan Jun Cui Yong Wei M. Fräenz

Abstract The Martian ionopause is generally identified as a steep electron density gradient and the peak of photoelectrons near 27 eV. However, it is not clear whether these two criteria identify the same position in the Martian ionopause region. The Mars Atmosphere and Volatile Evolution Mission (MAVEN) provides a good chance to compare both criteria for the first time with electron density data taken from the Langmuir probe and electron energy spectra from the Solar Wind Electron Analyzer. We identified 1,121 steep electron density gradients and 4,275 photoelectron boundary crossings within the first 2.7 years of MAVEN data. Observations show that two boundaries are nearly collocated when being observed simultaneously (about 15% of the available dataset). But when averaged over all observations, the photoelectron boundary locates higher than the steep electron density gradient. This may suggest a strong dependency of the Martian ionopause on magnetic field configuration in the Martian ionosphere. Results are generally consistent with previous observations made by Mars Express (MEX) and improve our understanding of the Martian ionosphere.

Atmosphere of Mars

Photoelectric effect

10.1029/2019ja026739

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Citations (15)

A One‐Dimensional Model of Atmospheric Sputtering at Io Driven by S⁺⁺ and O⁺

Journal of Geophysical Research Planets (2024)

Xu Huang Hao Gu Yangxin Ni Jinjin Zhao Jun Cui

Abstract Io, the closest of Jupiter's four Galilean moons, suffers from intense ion bombardment from Jupiter's magnetosphere. The constant atmospheric erosion by energetic ion precipitation, referred to atmospheric sputtering, serves as an important mechanism of Io's atmospheric escape. This study is devoted to a state‐of‐the‐art study of atmospheric sputtering at Io, with the aid of constantly accumulated understandings of Io's space environment and atmospheric photochemistry, as well as the updated laboratory measurements. A Monte Carlo model is constructed to track the energy degradation of incident S ++ and O + and atmospheric recoils from which the sputtering yields of different atmospheric species are determined. Our calculations suggest a total escape rate of 3 × 10 29 atom s −1 on Io, and SO 2 is the dominant sputtered species. Further investigations reveal that S ++ is the most efficient species for atmospheric sputtering on Io, and sputtering yields increase substantially with increasing incident ion mass, energy, and incidence angle. The model sensitivity to different influence factors is also discussed, including scattering angle distribution, atmospheric column density, proton precipitation, inelastic process, and surface sputtering, of which the former two dominate.

10.1029/2023je008129

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Citations (1)

Analysis of Titan's neutral upper atmosphere from Cassini Ion Neutral Mass Spectrometer measurements

Icarus (2008)

Jun Cui R. V. Yelle V. Vuitton J. H. Waite W. T. Kasprzak

Atmosphere of Titan

Atmospheric chemistry

10.1016/j.icarus.2008.12.005

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Citations (312)

Superior electron utilization of the intermetallic L10‑FePt-dispersed g-C3N4 for high-efficiency activating peroxymonosulfate

Separation and Purification Technology (2022)

Meng Ren Jiaqi Hou Jun Ma Yinjie Zhang Meng Liu

10.1016/j.seppur.2022.122105

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Citations (3)

An efficient hexadecimal network flow watermark method for tracking attack traffic

Scientific Reports (2023)

Jun Cui Keya Han Lin Sha Wei Liu Xiaofeng Zhang

Abstract Network flow watermark technology is a traffic marking technique that embeds watermark information into the characteristics of network flows to mark and trace attack flows generated by network attackers. However, with the development of network attack techniques, the time and number of packets required for network attacks have decreased. Existing network flow watermark technologies fail to balance watermark robustness and efficiency, resulting in poor practicality. To address this issue, this paper proposes an efficient hexadecimal network flow watermark method. The method introduces an efficient interval watermark algorithm and utilizes an interval synchronization algorithm to self-learn watermark parameters, thereby improving the encoding efficiency of the watermark. The design of watermark start and end markers ensures the practicality of network watermarks, enabling traceability and source attribution of attack flows in real network environments. The proposed method is experimentally tested using real network traffic, and the results demonstrate that even in the presence of a network jitter, the watermark detection success rate of this scheme remains above 95%. Compared to other network flow watermark schemes, the hexadecimal network flow watermark proposed in this paper achieves a 50% improvement in encoding and decoding efficiency while ensuring robustness. It also exhibits excellent resistance to network jitter, packet loss, and false packet insertion.

Tracking (education)

10.1038/s41598-023-48552-0

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Citations (0)