火星与金星弓激波上游的太阳风减速与偏转

火星和金星由于缺乏内禀磁场，弓激波距离行星表面较近，其高层大气可以延伸至弓激波上游，与太阳风直接发生相互作用。在这一过程中，行星高层大气中的中性原子被电离并在太阳风对流电场和行星际磁场的共同作用下，与太阳风共同流动成为拾起离子。由于动量守恒定律，拾起离子质量加载效应将引起太阳风速度的相应改变。这一过程在火星与金星这样的无内禀磁场的类地行星与太阳风的相互作用中扮演了重要的角色。%本文通过卫星观测数据、测试粒子模拟和理论模型，研究了火星和金星弓激波上游的太阳风减速和偏转现象，为太阳风与非磁化类地行星之间的能量传输过程提供了理论与观测依据。

首先，本文利用火星大气与挥发性演化探测器的数据对火星弓激波上游太阳风的减速现象进行了定量分析。分析时段覆盖2015年1月至2019年12月，结果表明在排除了激波过程的影响后，太阳风在火星上游的减速约为未受扰动太阳风速度的0.7%。研究使用简单的动量守恒模型评估了拾起离子质量加载所引起的太阳风减速。结果表明在假设拾起离子的拾起过程瞬间完成的情形下，拾起氢离子对于质量加载的贡献并不能如前人所认为的那样被忽略；统计结果和模型结果的对比表明观测到的太阳风减速与质量加载机制的预期相符。

此外，本研究利用相同的数据集对火星弓激波上游的太阳风偏转进行了统计分析，得到火星弓激波上游太阳风偏转的中位值约为-3.2 km/s。为了深入理解火星弓激波上游的质量加载过程，使用测试粒子模拟对拾起氢离子和拾起氧离子在火星弓激波上游的运动特性进行了分析。结果表明，拾起氢离子可以被太阳风对流电场加速至接近太阳风速度，且密度分布与假设其拾起过程瞬间完成时的结果一致。而拾起氧离子在火星弓激波上游的平均速度则远低于太阳风速度，且密度分布呈现出明显的不对称性。进一步地，使用多流体近似下的动量守恒模型对太阳风减速和偏转进行了定量评估，模型结果给出的太阳风偏转与统计结果一致。

本研究还使用金星快车在2007年至2013年期间的太阳风观测数据，对金星弓激波上游的太阳风减速进行了统计分析。结果表明，平均太阳风速度在弓激波附近区域与在金星快车远金点区域相比下降了约20 km/s。此外，太阳风速度沿着太阳风流动方向的减速值约为15 km/s。这一数值远大于拾起离子质量加载所能提供的减速。在排除超低频波造成的太阳风减速后，金星弓激波上游的太阳风减速依旧大于拾起离子质量加载机制给出的预期。

作为对激波过程如何导致激波上游太阳风减速的初步探索，本文利用测试粒子模拟的方法对离子在垂直激波的加速过程进行了研究。整体而言，离子的能量增益随着离子上游平均动能的增大而升高；且当离子上游平均动能较低（离子回旋半径小于激波面厚度或相当）时，激波横越电势和磁过冲对离子的能量增益起到促进作用；而当离子上游平均动能较高时，激波内部结构对于离子能量增益的影响逐渐可以被忽略。此外，与激波横越电势相比，激波磁过冲的强度对离子能量增益的影响占主导，离子的能量增益随着磁过冲的增强而增强。同时，磁场过冲和横越电势对于离子能量增益的影响之间的关系较为复杂，并非简单的叠加，有时甚至存在相互抵消的作用。

[1] 涂传诒, 宗秋刚, 周煦之. 日地空间物理学（第二版）上册·日球层物理: 第1 卷[M]. 第二版. 北京: 科学出版社, 2020.
[2] ALFVÉN H. On the Theory of Comet Tails[J/OL]. Tellus, 1957, 9(1): 92-96. https://doi.org/10.1111/j.2153-3490.1957.tb01855.x.
[3] LUHMANN J G. The solar wind interaction with Venus[J/OL]. Space Science Reviews, 1986,44: 241–30. https://doi.org/10.1007/BF00200818.
[4] ESPOSITO L, et al. Chemistry of lower atmosphere and clouds. Venus II[M]. The Universityof Arizona Press, 1997.
[5] DE BERGH C, MOROZ V, TAYLOR F W, et al. The composition of the atmosphere of Venusbelow 100 km altitude: An overview[J]. Planetary and space Science, 2006, 54(13-14): 1389-1397.
[6] RUSSEL C T. Does Venus have an intrinsic magnetic field?[J/OL]. Nature, 1978, 275: 692-692.https://api.semanticscholar.org/CorpusID:4158706.
[7] LUHMANN J, LEDVINA S, LYON J, et al. Venus O+ pickup ions: Collected PVO results andexpectations for Venus Express[J]. Planetary and Space Science, 2006, 54(13-14): 1457-1471.
[8] BARABASH S, FEDOROV A, SAUVAUD J, et al. The loss of ions from Venus through theplasma wake[J]. Nature, 2007, 450(7170): 650-653.
[9] 肖苏东. 太阳风与金星感应磁层相互作用[D]. 中国科学技术大学, 2018.
[10] KALLIO E. An empirical model of the solar wind flow around Mars[J/OL]. Journal of GeophysicalResearch: Space Physics, 1996, 101(A5): 11133-11147. https://doi.org/10.1029/96JA00164.
[11] Solar wind flow past nonmagnetic planets—Venus and Mars[J/OL]. Planetary and Space Science,1970, 18(9): 1281-1299. https://doi.org/10.1016/0032-0633(70)90139-X.
[12] LUHMANN J G, TATRALLYAY M, PEPIN R O. Venus and Mars: atmospheres, ionospheres,and solar wind interactions[J]. Geophysical Monograph Series, 1992, 66.
[13] CRAVENS T E, KOZYRA J U, NAGY A F, et al. Electron impact ionization in the vicinityof comets[J/OL]. Journal of Geophysical Research: Space Physics, 1987, 92(A7): 7341-7353.https://doi.org/10.1029/JA092iA07p07341.
[14] LUHMANN J, ELPHIC R, RUSSELL C, et al. Observations of large scale steady magneticfields in the nightside Venus ionosphere and near wake[J]. Geophysical Research Letters, 1981,8(5): 517-520.
[15] ZHANG T, BAUMJOHANN W, DU J, et al. Hemispheric asymmetry of the magnetic fieldwrapping pattern in the Venusian magnetotail[J/OL]. Geophysical Research Letters, 2010, 37(14). https://doi.org/10.1029/2010GL044020.
[16] VIGNES D, MAZELLE C, RME H, et al. The solar wind interaction with Mars: Locationsand shapes of the bow shock and the magnetic pile-up boundary from the observations of theMAG/ER Experiment onboard Mars Global Surveyor[J/OL]. Geophysical Research Letters,2000, 27(1): 49-52. https://doi.org/10.1029/1999GL010703.
[17] SLAVIN J A, ELPHIC R, RUSSELL C T. A comparison of Pioneer Venus and Venera bowshock observations: Evidence for a solar cycle variation[J/OL]. Geophysical Research Letters,1979, 6: 905-908. https://api.semanticscholar.org/CorpusID:122555314.
[18] VERIGIN M I, KOTOVA G A, SHUTTE N M, et al. Quantitative model of the Martian magnetopauseshape and its variation with the solar wind ram pressure based on Phobos 2 observations[J/OL]. Journal of Geophysical Research, 1997, 102: 2147-2155. https://api.semanticscholar.org/CorpusID:119801215.
[19] ZHANG T, SCHWINGENSCHUH K, LICHTENEGGER H I M, et al. Interplanetary magneticfield control of the Mars bow shock - Evidence for Venuslike interaction[J/OL]. Journal ofGeophysical Research, 1991, 96: 11265-11269. https://api.semanticscholar.org/CorpusID:120940400.
[20] ACUÑA M, CONNERNEY J, WASILEWSKI P A, et al. Magnetic field and plasma observationsat Mars: Initial results of the Mars Global Surveyor mission[J]. Science, 1998, 279(5357):1676-1680.
[21] CONNERNEY J, ESPLEY J, LAWTON P, et al. The MAVEN magnetic field investigation[J/OL]. Space Science Reviews, 2015, 195(1-4): 257-291. https://doi.org/10.1007/s11214-015-0169-4.
[22] CRIDER D H, VIGNES D, KRYMSKII A M, et al. A proxy for determining solar wind dynamicpressure at Mars using Mars Global Surveyor data[J/OL]. Journal of Geophysical Research:Space Physics, 2003, 108(A12). https://doi.org/10.1029/2003JA009875.
[23] BERTAUX J L, LEBLANC F, WITASSE O, et al. Discovery of an aurora on Mars[J]. Nature,2005, 435(7043): 790-794.
[24] BRAIN D A, BARABASH S, BOUGHER S W, et al. Solar wind interaction and atmosphericescape[J]. The atmosphere and climate of Mars, 2017: 464-496.
[25] CRIDER D H, BRAIN D A, ACUÑA M H, et al. Mars Global Surveyor observations of solarwind magnetic field draping around Mars[J]. Mars’magnetism and its interaction with the solarwind, 2004: 203-221.
[26] GRUESBECK J R, ESPLEY J R, CONNERNEY J E P, et al. The Three-Dimensional BowShock of Mars as Observed by MAVEN[J/OL]. Journal of Geophysical Research: SpacePhysics, 2018, 123(6): 4542-4555. https://doi.org/10.1029/2018JA025366.
[27] SZEGÖ K, GLASSMEIER K H, BINGHAM R, et al. Physics of mass loaded plasmas[J]. SpaceScience Reviews, 2000, 94: 429-671.
[28] CHAUFRAY J Y, GONZALEZ-GALINDO F, FORGET F, et al. Variability of the hydrogen inthe Martian upper atmosphere as simulated by a 3D atmosphere–exosphere coupling[J]. Icarus,2015, 245: 282-294.
[29] GRUCHOLA S, GALLI A, VORBURGER A, et al. The upper atmosphere of Venus: Modelpredictions for mass spectrometry measurements[J]. Planetary and space science, 2019, 170:29-41.
[30] RUSSELL C T, LUHMANN J G, STRANGEWAY R J. The solar wind interaction with Venusthrough the eyes of the Pioneer Venus Orbiter[J/OL]. Planetary and Space Science, 2006, 54(13): 1482-1495. DOI: https://doi.org/10.1016/j.pss.2006.04.025.
[31] FUTAANA Y, STENBERG WIESER G, BARABASH S, et al. Solar wind interaction andimpact on the Venus atmosphere[J]. Space Science Reviews, 2017, 212: 1453-1509.
[32] DONG Y, FANG X, BRAIN D, et al. Strong plume fluxes at Mars observed by MAVEN: Animportant planetary ion escape channel[J]. Geophysical Research Letters, 2015, 42(21): 8942-8950.
[33] DUBININ E, FRAENZ M, PäTZOLD M, et al. Solar Wind Deflection by Mass Loading in theMartian Magnetosheath Based on MAVEN Observations[J/OL]. Geophysical Research Letters,2018, 45(6): 2574-2579. DOI: 10.1002/2017gl076813.
[34] ROMANELLI N, DIBRACCIO G, HALEKAS J, et al. Variability of the Solar Wind FlowAsymmetry in the Martian Magnetosheath Observed by MAVEN[J/OL]. Geophysical ResearchLetters, 2020, 47(22). DOI: 10.1029/2020gl090793.
[35] ROMEO O, ROMANELLI N, ESPLEY J, et al. Variability of upstream proton cyclotron waveproperties and occurrence at Mars observed by MAVEN[J]. Journal of Geophysical Research:Space Physics, 2021, 126(2): e2020JA028616.
[36] CHENG K, LIU K, MOUSAVI A, et al. Hybrid Simulation of Proton Cyclotron Waves Upstreamof Mars Generated by Pickup Ion Beam Distribution[J/OL]. Geophysical Research Letters,2023, 50(11). https://doi.org/10.1029/2023gl103180.
[37] COWEE M, GARY S, WEI H. Pickup ions and ion cyclotron wave amplitudes upstream ofMars: First results from the 1D hybrid simulation[J/OL]. Geophysical research letters, 2012,39(8). https://doi.org/10.1029/2012GL051313.
[38] COWEE M, GARY S. Electromagnetic ion cyclotron wave generation by planetary pickupions: One‐dimensional hybrid simulations at sub‐Alfvénic pickup velocities[J/OL]. Journal ofGeophysical Research: Space Physics, 2012, 117(A6). https://doi.org/10.1029/2012JA017568.
[39] GARY S P. Electromagnetic ion/ion instabilities and their consequences in space plasmas: Areview[J]. Space Science Reviews, 1991, 56(3): 373-415.
[40] DELVA M, MAZELLE C, BERTUCCI C, et al. Proton cyclotron wave generation mechanismsupstream of Venus[J/OL]. Journal of Geophysical Research: Space Physics, 2011, 116(A2).https://doi.org/10.1029/2010JA015826.
[41] BRAIN D A, BAGENAL F, ACUÑA M H, et al. Observations of low-frequency electromagneticplasma waves upstream from the Martian shock[J]. Journal of Geophysical Research:Space Physics, 2002, 107(A6): SMP 9-1-SMP 9-11.
[42] WU P, WINSKE D, GARY S, et al. Energy dissipation and ion heating at the heliospherictermination shock[J/OL]. Journal of Geophysical Research: Space Physics, 2009, 114(A8).https://doi.org/10.1029/2009JA014240.
[43] COATES A, LIN R, WILKEN B, et al. Giotto measurements of cometary and solar wind plasmaat the comet Halley bow shock[J]. Nature, 1987, 327(6122): 489-492.
[44] COATES A, WILKEN B, JOHNSTONE A, et al. Bulk properties and velocity distributions ofwater group ions at comet Halley: Giotto measurements[J]. Journal of Geophysical Research:Space Physics, 1990, 95(A7): 10249-10260.
[45] COATES A, JOHNSTONE A, KESSEL R, et al. Plasma parameters near the comet Halley bowshock[J]. Journal of Geophysical Research: Space Physics, 1990, 95(A12): 20701-20716.
[46] COATES A. Observations of the velocity distribution of pickup ions[J]. Cometary PlasmaProcesses, 1991, 61: 301-310.
[47] FORMISANO V, AMATA E. Solar wind interaction with the Earth’magnetic field, 4. Preshockperturbation of the solar wind[J/OL]. Journal of Geophysical Research, 1976, 81(22): 3907-3912. https://doi.org/10.1029/JA081i022p03907.
[48] BAME S, ASBRIDGE J, FELDMAN W, et al. Deceleration of the solar wind upstream fromthe earth’s bow shock and the origin of diffuse upstream ions[J/OL]. Journal of GeophysicalResearch: Space Physics, 1980, 85(A6): 2981-2990. https://doi.org/10.1029/JA085iA06p02981.
[49] BONIFAZI C, MORENO G, LAZARUS A, et al. Deceleration of the solar wind in the Earth’sforeshock region: ISEE 2 and IMP 8 observations[J/OL]. Journal of Geophysical Research:Space Physics, 1980, 85(A11): 6031-6038. https://doi.org/10.1029/JA085iA11p06031.
[50] BONIFAZI C, MORENO G, RUSSELL C, et al. Solar wind deceleration and MHD turbulencein the Earth’s foreshock region: ISEE 1 and 2 and IMP 8 observations[J/OL]. Journal of GeophysicalResearch: Space Physics, 1983, 88(A3): 2029-2037. https://doi.org/10.1029/JA088iA03p02029.
[51] FU H, CAO J, ZHANG T, et al. Statistical study of the solar wind deceleration in the Earth’sforeshock region[J/OL]. Chinese Journal of Geophysics, 2009, 52(2): 361-368. https://doi.org/10.1002/cjg2.1356.
[52] 符慧山, 等. 太阳风在地球激波前兆区的减速以及地球内磁层的结构研究[D]. 北京: 中国科学院研究生院, 2010.
[53] VERIGIN M, GRINGAUZ K, KOTOVA G, et al. On the problem of the Martian atmospheredissipation: Phobos: 2 TAUS Spectrometer results[J/OL]. Journal of Geophysical Research:Space Physics, 1991, 96(A11): 19315-19320. https://doi.org/10.1029/90JA02561.
[54] BARABASH S, LUNDIN R. Reflected ions near Mars: PHOBOS‐2 observations[J/OL]. Geophysicalresearch letters, 1993, 20(9): 787-790. https://doi.org/10.1029/93GL00834.
[55] DUBININ E, OBOD D, PEDERSEN A, et al. Mass‐loading asymmetry in upstream regionnear Mars[J/OL]. Geophysical research letters, 1994, 21(24): 2769-2772. https://doi.org/10.1029/94GL02666.
[56] KOTOVA G, VERIGIN M, REMIZOV A, et al. Study of the solar wind deceleration upstreamof the Martian terminator bow shock[J/OL]. Journal of Geophysical Research: Space Physics,1997, 102(A2): 2165-2173. https://doi.org/10.1029/96JA01533.
[57] ZHANG T, SCHWINGENSCHUH K, RUSSELL C. A study of the solar wind decelerationin the Earth’s foreshock region[J/OL]. Advances in Space Research, 1995, 15(8-9): 137-140.https://doi.org/10.1016/0273-1177(94)00095-I.
[58] ZHANG T, SCHWINGENSCHUN K, RIEDLER W, et al. Solar wind deceleration at Marsand Earth: A comparison[J/OL]. Advances in Space Research, 1997, 20(2): 133-136. https://doi.org/10.1016/S0273-1177(97)00522-X.
[59] BIERMANN L, BROSOWSKI B, SCHMIDT H. The interaction of the solar wind with a comet[J/OL]. Solar Physics, 1967, 1: 254-284. https://doi.org/10.1007/BF00150860.
[60] DUBININ E, SAUER K, DELVA M, et al. Deceleration of the solar wind upstream of themartian bow shock. Mass-loading or foreshock features?[J/OL]. Advances in Space Research,2000, 26(10): 1627-1631. https://doi.org/10.1016/S0273-1177(00)00104-6.
[61] DUBININ E, SAUER K, DELVA M, et al. Multi‐instrument study of the upstream region nearMars: The Phobos 2 observations[J/OL]. Journal of Geophysical Research: Space Physics,2000, 105(A4): 7557-7571. https://doi.org/10.1029/1999JA900400.
[62] ZHANG T, LICHTENEGGER H, SHI J, et al. Hot oxygen corona at Mars and its effect onsolar wind deceleration[J/OL]. Chinese Physics Letters, 2006, 23(8): 2338-2340. https://doi.org/10.1088/0256-307X/23/8/102.
[63] HALEKAS J, RUHUNUSIRI S, HARADA Y, et al. Structure, dynamics, and seasonal variabilityof the Mars‐solar wind interaction: MAVEN Solar Wind Ion Analyzer in‐flight performanceand science results[J/OL]. Journal of Geophysical Research: Space Physics, 2017, 122(1):547-578. https://doi.org/10.1002/2016JA023167.
[64] JAKOSKY B M, LIN R P, GREBOWSKY J M, et al. The Mars atmosphere and volatile evolution(MAVEN) mission[J/OL]. Space Science Reviews, 2015, 195: 3-48. https://doi.org/10.1007/s11214-015-0139-x.
[65] HUANG H, GUO J, MAZELLE C, et al. Properties of Interplanetary Fast Shocks Close to theMartian Environment[J]. The Astrophysical Journal, 2021, 914(1): 14 (15pp).
[66] HALEKAS J, TAYLOR E, DALTON G, et al. The solar wind ion analyzer for MAVEN[J/OL].Space Science Reviews, 2015, 195: 125-151. https://doi.org/10.1007/s11214-013-0029-z.
[67] ROSENBAUER H, SCHUTTE N, APATHY I, et al. The study of three-dimensional distributionfunctions of the main solar wind ions—Protons and alpha particles in Phobos mission. TAUSexperiment[J]. The Instrumentation and Methods of Space Research, 1989: 30-43.
[68] AYDOGAR O. The PHOBOS fluxgate magnetometer (MAGMA): instrument description[M].Inst. für Weltraumforschung, 1989.
[69] WOODS L. On double-structured, perpendicular, magneto-plasma shock waves[J/OL]. PlasmaPhysics, 1971, 13(4): 289. https://doi.org/10.1088/0032-1028/13/4/302.
[70] BURNE S, BERTUCCI C, MAZELLE C, et al. The Structure of the Martian Quasi-Perpendicular Supercritical Shock as Seen by MAVEN[J/OL]. Journal of Geophysical Research:Space Physics, 2021, 126(9): e2020JA028938. https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2020JA028938. DOI: https://doi.org/10.1029/2020JA028938.
[71] MODOLO R, HESS S, MANCINI M, et al. Mars‐solar wind interaction: LatHyS, an improvedparallel 3‐D multispecies hybrid model[J/OL]. Journal of Geophysical Research: SpacePhysics, 2016, 121(7): 6378-6399. https://doi.org/10.1002/2015JA022324.
[72] RAHMATI A, LARSON D, CRAVENS T, et al. Seasonal variability of neutral escape fromMars as derived from MAVEN pickup ion observations[J]. Journal of Geophysical Research:Planets, 2018, 123(5): 1192-1202.
[73] RAHMATI A. Oxygen exosphere of Mars: Evidence from pickup ions measured by MAVEN[D]. University of Kansas, 2016.
[74] RAHMATI A, LARSON D, CRAVENS T, et al. MAVEN measured oxygen and hydrogenpickup ions: Probing the Martian exosphere and neutral escape[J]. Journal of GeophysicalResearch: Space Physics, 2017, 122(3): 3689-3706.
[75] MODOLO R, CHANTEUR G M, DUBININ E, et al. Influence of the solar EUV flux on theMartian plasma environment[C/OL]//Annales Geophysicae: Vol. 23. Copernicus PublicationsGöttingen, Germany: 433-444. https://doi.org/10.5194/angeo-23-433-2005.
[76] MOTT N F, MASSEY H S W. The theory of atomic collisions: Vol. 35[M]. Clarendon PressOxford, 1965.
[77] STEBBINGS R, SMITH A, EHRHARDT H. Charge transfer between oxygen atoms and O+and H+ ions[J/OL]. Journal of Geophysical Research, 1964, 69(11): 2349-2355. https://doi.org/10.1029/JZ069i011p02349.
[78] LIU D, RONG Z, GAO J, et al. Statistical properties of solar wind upstream of Mars: MAVENobservations[J]. The Astrophysical Journal, 2021, 911(2): 113.
[79] PETROVAY K. Solar cycle prediction[J/OL]. Living Reviews in Solar Physics, 2020, 17(1):2. https://doi.org/10.1007/s41116-020-0022-z.
[80] ZOU H, LILLIS R J, WANG J S, et al. Determination of seasonal variations in the Martianneutral atmosphere from observations of ionospheric peak height[J/OL]. Journal of GeophysicalResearch: Planets, 2011, 116(E9). https://doi.org/10.1029/2011JE003833.
[81] YAMAUCHI M, HARA T, LUNDIN R, et al. Seasonal variation of Martian pick-up ions:Evidence of breathing exosphere[J/OL]. Planetary and Space Science, 2015, 119: 54-61. https://doi.org/10.1016/j.pss.2015.09.013.
[82] DONG C, BOUGHER S W, MA Y, et al. Solar wind interaction with the Martian upper atmosphere:Crustal field orientation, solar cycle, and seasonal variations[J/OL]. Journal of GeophysicalResearch: Space Physics, 2015, 120(9): 7857-7872. https://doi.org/10.1002/2015JA020990.
[83] HALEKAS J. Seasonal variability of the hydrogen exosphere of Mars[J/OL]. Journal of GeophysicalResearch: Planets, 2017, 122(5): 901-911. https://doi.org/10.1002/2017JE005306.
[84] ZOU Y, ZHU Y, BAI Y, et al. Scientific objectives and payloads of Tianwen-1, China’sfirst Mars exploration mission[J/OL]. Advances in Space Research, 2021, 67(2): 812-823.https://doi.org/10.1016/j.asr.2020.11.005.
[85] HALEKAS J S, BRAIN D A, LUHMANN J G, et al. Flows, fields, and forces in the Marssolarwind interaction[J]. Journal of Geophysical Research: Space Physics, 2017, 122(11):11320-11341.SAUER K, BOGDANOV A, BAUMGÄRTEL K. Evidence of an ion composition boundary(protonopause) in bi-ion fluid simulations of solar wind mass loading[J]. Geophysical ResearchLetters, 1994, 21(20): 2255-2258.
[87] MARCHAND R. Test-particle simulation of space plasmas[J]. Communications in ComputationalPhysics, 2010, 8(3): 471.
[88] FANG X, LIEMOHN M W, NAGY A F, et al. Pickup oxygen ion velocity space and spatialdistribution around Mars[J/OL]. Journal of Geophysical Research: Space Physics, 2008, 113(A2). https://doi.org/10.1029/2007JA012736.
[89] SLAVIN J, ELPHIC R, RUSSELL C, et al. The solar wind interaction with Venus: PioneerVenus observations of bow shock location and structure[J]. Journal of Geophysical Research:Space Physics, 1980, 85(A13): 7625-7641.
[90] TATRALLYAY M, RUSSELL C, LUHMANN J, et al. On the proper Mach number and ratio ofspecific heats for modeling the Venus bow shock[J]. Journal of Geophysical Research: SpacePhysics, 1984, 89(A9): 7381-7392.
[91] RUSSELL C, LUHMANN J, PHILLIPS J. The location of the subsolar bow shock of Venus:Implications for the obstacle shape[J]. Geophysical research letters, 1985, 12(10): 627-630.
[92] ZHANG T L, LUHMANN J, RUSSELL C. The solar cycle dependence of the location andshape of the Venus bow shock[J]. Journal of Geophysical Research: Space Physics, 1990, 95(A9): 14961-14967.
[93] SHAN L, LU Q, MAZELLE C, et al. The shape of the Venusian bow shock at solar minimumand maximum: Revisit based on VEX observations[J]. Planetary and Space Science, 2015, 109:32-37.
[94] KALLIO E, JARVINEN R, JANHUNEN P. Venus–solar wind interaction: Asymmetries andthe escape of O+ ions[J]. Planetary and Space Science, 2006, 54(13-14): 1472-1481.
[95] EASTWOOD J, LUCEK E, MAZELLE C, et al. The foreshock[J]. Space Science Reviews,2005, 118: 41-94.
[96] BONIFAZI C, MORENO G. Reflected and diffuse ions backstreaming from the Earth’s bowshock 2. Origin[J]. Journal of Geophysical Research: Space Physics, 1981, 86(A6): 4405-4413.
[97] GEDALIN M, POGORELOV N V, ROYTERSHTEYN V. Backstreaming pickup ions[J]. TheAstrophysical Journal, 2021, 910(2): 107.
[98] SHAN L, MAZELLE C, MEZIANE K, et al. Characteristics of quasi-monochromatic ULFwaves in the Venusian foreshock[J]. Journal of Geophysical Research: Space Physics, 2016,121(8): 7385-7397.
[99] ORLOWSKI D, RUSSELL C. Ulf waves upstream of the Venus bow shock: Properties of onehertzwaves[J]. Journal of Geophysical Research: Space Physics, 1991, 96(A7): 11271-11282.
[100] SHAN L, MAZELLE C, MEZIANE K, et al. The Quasi-monochromatic ULF Wave Boundaryin the Venusian Foreshock: Venus Express Observations[J]. Journal of Geophysical Research:Space Physics, 2018, 123(1): 374-384.
[101] GREENSTADT E, BAUM L. Earth’s compressional foreshock boundary revisited: Observationsby the ISEE 1 magnetometer[J]. Journal of Geophysical Research: Space Physics, 1986,91(A8): 9001-9006.
[102] CRAWFORD G, STRANGEWAY R, RUSSELL C. Statistical imaging of the Venus foreshockusing VLF wave emissions[J]. Journal of Geophysical Research: Space Physics, 1998, 103(A6): 11985-12003.
[103] SUNDBERG T, HAYNES C T, BURGESS D, et al. Ion acceleration at the quasi-parallel bowshock: decoding the signature of injection[J]. The Astrophysical Journal, 2016, 820(1): 21.
[104] HUDSON P, KAHN F. Reflection of charged particles by plasma shocks[J]. Monthly Noticesof the Royal Astronomical Society, 1965, 131(1): 23-49.
[105] LEE M A, SHAPIRO V D, SAGDEEV R Z. Pickup ion energization by shock surfing[J].Journal of Geophysical Research: Space Physics, 1996, 101(A3): 4777-4789.
[106] LEVER E L, QUEST K B, SHAPIRO V D. Shock surfing vs. shock drift acceleration[J].Geophysical research letters, 2001, 28(7): 1367-1370.
[107] SHAPIRO V D, ÜÇER D. Shock surfing acceleration[J]. Planetary and Space Science, 2003,51(11): 665-680.
[108] WINSKE D, YIN L, OMIDI N, et al. Hybrid simulation codes: Past, present and future—Atutorial[J]. Space plasma simulation, 2003: 136-165.
[109] LIPATOV A S. The hybrid multiscale simulation technology: an introduction with applicationto astrophysical and laboratory plasmas[M]. Springer Science & Business Media, 2013.
[110] HELLINGER P, TRAVNICEK P, MATSUMOTO H. Reformation of perpendicular shocks:Hybrid simulations[J]. Geophysical research letters, 2002, 29(24): 87-1.
[111] LOBZIN V, KRASNOSELSKIKH V, BOSQUED J M, et al. Nonstationarity and reformationof high-Mach-number quasiperpendicular shocks: Cluster observations[J/OL]. GeophysicalResearch Letters, 2007, 34(5). https://doi.org/10.1029/2006GL029095.
[112] MAZELLE C, LEMBÈGE B, MORGENTHALER A, et al. Self-reformation of the quasiperpendicularshock: Cluster observations[C]//AIP Conference Proceedings: Vol. 1216. AmericanInstitute of Physics, 2010: 471-474.
[113] YANG Z, LU Q, WANG S. The evolution of the electric field at a nonstationary perpendicularshock[J/OL]. Physics of Plasmas, 2009, 16(12). https://doi.org/10.1063/1.3275788.
[114] YANG Z, LU Q, LEMBÈGE B, et al. Shock front nonstationarity and ion acceleration in supercriticalperpendicular shocks[J/OL]. Journal of Geophysical Research: Space Physics, 2009,114(A3). https://doi.org/10.1029/2008JA013785.
[115] WU P, LIU K, WINSKE D, et al. Hybrid simulations of the termination shock: Suprathermalion velocity distributions in the heliosheath[J/OL]. Journal of Geophysical Research: SpacePhysics, 2010, 115(A11). https://doi.org/10.1029/2010JA015384.
[116] MATSUKIYO S, SCHOLER M. Simulations of pickup ion mediated quasi-perpendicularshocks: Implications for the heliospheric termination shock[J]. Journal of Geophysical Research:Space Physics, 2014, 119(4): 2388-2399.
[117] GEDALIN M. Transmitted, reflected, quasi-reflected, and multiply reflected ions in low-Machnumber shocks[J]. Journal of Geophysical Research: Space Physics, 2016, 121(11): 10-754.
[118] 杨忠炜, 陆全明, 郭俊, 等. 垂直无碰撞激波的离子加速机制[J]. 地球物理学报, 2008, 51(4): 953-959.
[119] LIEWER P, GOLDSTEIN B, OMIDI N. Hybrid simulations of the effects of interstellar pickuphydrogen on the solar wind termination shock[J]. Journal of Geophysical Research: SpacePhysics, 1993, 98(A9): 15211-15220.