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Artículos de revistas sobre el tema "Lunar wake plasma"

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Autor: Grafiati
Publicado: 6 de septiembre de 2023

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1

Yan, Bo, Punam K. Prasad, Sayan Mukherjee, Asit Saha y Santo Banerjee. "Dynamical Complexity and Multistability in a Novel Lunar Wake Plasma System". Complexity 2020 (16 de marzo de 2020): 1–11. http://dx.doi.org/10.1155/2020/5428548.

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Dynamical complexity and multistability of electrostatic waves are investigated in a four-component homogeneous and magnetized lunar wake plasma constituting of beam electrons, heavier ions (alpha particles, He++), protons, and suprathermal electrons. The unperturbed dynamical system of the considered lunar wake plasma supports nonlinear and supernonlinear trajectories which correspond to nonlinear and supernonlinear electrostatic waves. On the contrary, the perturbed dynamical system of lunar wake plasma shows different types of coexisting attractors including periodic, quasiperiodic, and chaotic, investigated by phase plots and Lyapunov exponents. To confirm chaotic and nonchaotic dynamics in the perturbed lunar wake plasma, 0−1 chaos test is performed. Furthermore, a weighted recurrence-based entropy is implemented to investigate the dynamical complexity of the system. Numerical results show existence of chaos with variation of complexity in the perturbed dynamics.
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2

Rasca, Anthony P., Shahab Fatemi y William M. Farrell. "Modeling the Lunar Wake Response to a CME Using a Hybrid PIC Model". Planetary Science Journal 3, n.º 1 (1 de enero de 2022): 4. http://dx.doi.org/10.3847/psj/ac3fba.

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Abstract In the solar wind, a low-density wake region forms downstream of the nightside lunar surface. In this study, we use a series of 3D hybrid particle-in-cell simulations to model the response of the lunar wake to a passing coronal mass ejection (CME). Average plasma parameters are derived from the Wind spacecraft located at 1 au during three distinct phases of a passing halo (Earth-directed) CME on 2015 June 22. Each set of plasma parameters, representing the shock/plasma sheath, a magnetic cloud, and plasma conditions we call the mid-CME phase, are used as the time-static upstream boundary conditions for three separate simulations. These simulation results are then compared with results that use nominal solar wind conditions. Results show a shortened plasma void compared to nominal conditions and a distinctive rarefaction cone originating from the terminator during the CME’s plasma sheath phase, while a highly elongated plasma void reforms during the magnetic cloud and mid-CME phases. Developments of electric and magnetic field intensification are also observed during the plasma sheath phase along the central wake, while electrostatic turbulence dominates along the plasma void boundaries and 2–3 lunar radii R M downstream in the central wake during the magnetic cloud and mid-CME phases. The simulations demonstrate that the lunar wake responds in a dynamic way with the changes in the upstream solar wind during a CME.
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3

Sreeraj, T., S. V. Singh y G. S. Lakhina. "Electrostatic waves driven by electron beam in lunar wake plasma". Physics of Plasmas 25, n.º 5 (mayo de 2018): 052902. http://dx.doi.org/10.1063/1.5032141.

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4

Sreeraj, T., S. V. Singh y G. S. Lakhina. "Linear analysis of electrostatic waves in the lunar wake plasma". Physica Scripta 95, n.º 4 (19 de febrero de 2020): 045610. http://dx.doi.org/10.1088/1402-4896/ab7142.

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5

Xu, Xiaojun, Qi Xu, Qing Chang, Jiaying Xu, Jing Wang, Yi Wang, Pingbing Zuo y Vassilis Angelopoulos. "ARTEMIS Observations of Well-structured Lunar Wake in Subsonic Plasma Flow". Astrophysical Journal 881, n.º 1 (14 de agosto de 2019): 76. http://dx.doi.org/10.3847/1538-4357/ab2e0a.

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6

Guo, Dawei, Xiaoping Zhang, Lianghai Xie, Xiaojun Xu, Aoao Xu, Qi Yan, Yi Xu y Fan Yang. "Diamagnetic Plasma Clouds in the Near Lunar Wake Observed by ARTEMIS". Astrophysical Journal 883, n.º 1 (17 de septiembre de 2019): 12. http://dx.doi.org/10.3847/1538-4357/ab3652.

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7

Halekas, J. S., S. D. Bale, D. L. Mitchell y R. P. Lin. "Correction to “Electrons and magnetic fields in the lunar plasma wake”". Journal of Geophysical Research: Space Physics 116, A7 (julio de 2011): n/a. http://dx.doi.org/10.1029/2011ja016929.

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8

Xu, Xiaojun, Jiaying Xu, Qi Xu, Qing Chang y Jing Wang. "Rapid Refilling of the Lunar Wake under Transonic Plasma Flow: ARTEMIS Observations". Astrophysical Journal 908, n.º 2 (1 de febrero de 2021): 227. http://dx.doi.org/10.3847/1538-4357/abd6f1.

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9

Halekas, J. S., V. Angelopoulos, D. G. Sibeck, K. K. Khurana, C. T. Russell, G. T. Delory, W. M. Farrell et al. "First Results from ARTEMIS, a New Two-Spacecraft Lunar Mission: Counter-Streaming Plasma Populations in the Lunar Wake". Space Science Reviews 165, n.º 1-4 (20 de enero de 2011): 93–107. http://dx.doi.org/10.1007/s11214-010-9738-8.

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10

Yu, William, Joseph Wang y Kevin Chou. "Laboratory Measurement of Lunar Regolith Simulant Surface Charging in a Localized Plasma Wake". IEEE Transactions on Plasma Science 43, n.º 12 (diciembre de 2015): 4175–81. http://dx.doi.org/10.1109/tps.2015.2492551.

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11

Dhanya, M. B., A. Bhardwaj, Y. Futaana, S. Fatemi, M. Holmström, S. Barabash, M. Wieser, P. Wurz, A. Alok y R. S. Thampi. "Proton entry into the near-lunar plasma wake for magnetic field aligned flow". Geophysical Research Letters 40, n.º 12 (18 de junio de 2013): 2913–17. http://dx.doi.org/10.1002/grl.50617.

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12

Ogilvie, K. W., J. T. Steinberg, R. J. Fitzenreiter, C. J. Owen, A. J. Lazarus, W. M. Farrell y R. B. Torbert. "Observations of the lunar plasma wake from the WIND spacecraft on December 27, 1994". Geophysical Research Letters 23, n.º 10 (15 de mayo de 1996): 1255–58. http://dx.doi.org/10.1029/96gl01069.

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13

Farrell, W. M., M. L. Kaiser y J. T. Steinberg. "Electrostatic instability in the central lunar wake: A process for replenishing the plasma void?" Geophysical Research Letters 24, n.º 9 (1 de mayo de 1997): 1135–38. http://dx.doi.org/10.1029/97gl00878.

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14

Farrell, W. M., M. L. Kaiser, J. T. Steinberg y S. D. Bale. "A simple simulation of a plasma void: Applications to Wind observations of the lunar wake". Journal of Geophysical Research: Space Physics 103, A10 (1 de octubre de 1998): 23653–60. http://dx.doi.org/10.1029/97ja03717.

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15

Roussos, E., J. Müller, S. Simon, A. Bößwetter, U. Motschmann, N. Krupp, M. Fränz, J. Woch, K. K. Khurana y M. K. Dougherty. "Plasma and fields in the wake of Rhea: 3-D hybrid simulation and comparison with Cassini data". Annales Geophysicae 26, n.º 3 (26 de marzo de 2008): 619–37. http://dx.doi.org/10.5194/angeo-26-619-2008.

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Abstract. Rhea's magnetospheric interaction is simulated using a three-dimensional, hybrid plasma simulation code, where ions are treated as particles and electrons as a massless, charge-neutralizing fluid. In consistency with Cassini observations, Rhea is modeled as a plasma absorbing obstacle. This leads to the formation of a plasma wake (cavity) behind the moon. We find that this cavity expands with the ion sound speed along the magnetic field lines, resulting in an extended depletion region north and south of the moon, just a few Rhea radii (RRh) downstream. This is a direct consequence of the comparable thermal and bulk plasma velocities at Rhea. Perpendicular to the magnetic field lines the wake's extension is constrained by the magnetic field. A magnetic field compression in the wake and the rarefaction in the wake sides is also observed in our results. This configuration reproduces well the signature in the Cassini magnetometer data, acquired during the close flyby to Rhea on November 2005. Almost all plasma and field parameters show an asymmetric distribution along the plane where the corotational electric field is contained. A diamagnetic current system is found running parallel to the wake boundaries. The presence of this current system shows a direct corelation with the magnetic field configuration downstream of Rhea, while the resulting j×B forces on the ions are responsible for the asymmetric structures seen in the velocity and electric field vector fields in the equatorial plane. As Rhea is one of the many plasma absorbing moons of Saturn, we expect that this case study should be relevant for most lunar-type interactions at Saturn.
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16

Fatemi, S., M. Holmström y Y. Futaana. "The effects of lunar surface plasma absorption and solar wind temperature anisotropies on the solar wind proton velocity space distributions in the low-altitude lunar plasma wake". Journal of Geophysical Research: Space Physics 117, A10 (octubre de 2012): n/a. http://dx.doi.org/10.1029/2011ja017353.

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17

Hutchinson, Ian H. y David M. Malaspina. "Prediction and Observation of Electron Instabilities and Phase Space Holes Concentrated in the Lunar Plasma Wake". Geophysical Research Letters 45, n.º 9 (11 de mayo de 2018): 3838–45. http://dx.doi.org/10.1029/2017gl076880.

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18

Bale, S. D., C. J. Owen, J. L. Bougeret, K. Goetz, P. J. Kellogg, R. P. Lepping, R. Manning y S. J. Monson. "Evidence of currents and unstable particle distributions in an extended region around the lunar plasma wake". Geophysical Research Letters 24, n.º 11 (1 de junio de 1997): 1427–30. http://dx.doi.org/10.1029/97gl01193.

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19

Lou, Yuequn, Xudong Gu, Xing Cao, Mingyu Wu, Sudong Xiao, Guoqiang Wang, Binbin Ni y Tielong Zhang. "Statistical Analysis of Lunar 1 Hz Waves Using ARTEMIS Observations". Astrophysical Journal 943, n.º 1 (1 de enero de 2023): 17. http://dx.doi.org/10.3847/1538-4357/aca767.

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Abstract Like 1 Hz waves occurring in the upstream of various celestial bodies in the solar system, 1 Hz narrowband whistler-mode waves are often observed around the Moon. However, wave properties have not been thoroughly investigated, which makes it difficult to proclaim the generation mechanism of the waves. Using 5.5 yr wave data from ARTEMIS, we perform a detailed investigation of 1 Hz waves in the near-lunar space. The amplitude of lunar 1 Hz waves is generally 0.05–0.1 nT. In the geocentric solar ecliptic coordinates, the waves show no significant regional differentiation pattern but show an absence inside the magnetosphere. Correspondingly, in the selenocentric solar ecliptic coordinates, the waves can occur extensively at ∼1.1–12 RL, while few events are observed in the lunar wake due to a lack of interaction with the solar wind. Furthermore, the wave distributions exhibit modest day–night and dawn–dusk asymmetries but less apparent north–south asymmetry. Compared with the nightside, more intense waves with lower peak wave frequency are present on the dayside. The preferential distribution of 1 Hz waves exhibits a moderate correlation with strong magnetic anomalies. The waves propagate primarily at wave normal angles <60° with an ellipticity of [−0.8, −0.3]. For stronger wave amplitudes and lower latitudes, 1 Hz waves generally have smaller wave normal angles and become more left-hand circularly polarized. Owing to the unique interaction between the Moon and solar wind, our statistical results might provide new insights into the generation mechanism(s) of 1 Hz waves in planetary plasma environments and promote the understanding of lunar plasma dynamics.
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20

Lakhina, Gurbax Singh, Satyavir Singh, Rajith Rubia y Selvaraj Devanandhan. "Electrostatic Solitary Structures in Space Plasmas: Soliton Perspective". Plasma 4, n.º 4 (21 de octubre de 2021): 681–731. http://dx.doi.org/10.3390/plasma4040035.

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Occurrence of electrostatic solitary waves (ESWs) is ubiquitous in space plasmas, e.g., solar wind, Lunar wake and the planetary magnetospheres. Several theoretical models have been proposed to interpret the observed characteristics of the ESWs. These models can broadly be put into two main categories, namely, Bernstein–Green–Kruskal (BGK) modes/phase space holes models, and ion- and electron- acoustic solitons models. There has been a tendency in the space community to favor the models based on BGK modes/phase space holes. Only recently, the potential of soliton models to explain the characteristics of ESWs is being realized. The idea of this review is to present current understanding of the ion- and electron-acoustic solitons and double layers models in multi-component space plasmas. In these models, all the plasma species are considered fluids except the energetic electron component, which is governed by either a kappa distribution or a Maxwellian distribution. Further, these models consider the nonlinear electrostatic waves propagating parallel to the ambient magnetic field. The relationship between the space observations of ESWs and theoretical models is highlighted. Some specific applications of ion- and electron-acoustic solitons/double layers will be discussed by comparing the theoretical predictions with the observations of ESWs in space plasmas. It is shown that the ion- and electron-acoustic solitons/double layers models provide a plausible interpretation for the ESWs observed in space plasmas.
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21

Lipatov, A. S., M. Sarantos, W. M. Farrell y J. F. Cooper. "Effects of multiscale phase-mixing and interior conductance in the lunar-like pickup ion plasma wake. First results from 3-D hybrid kinetic modeling". Planetary and Space Science 156 (julio de 2018): 117–29. http://dx.doi.org/10.1016/j.pss.2018.02.017.

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22

Szita, S., A. N. Fazakerley, P. J. Carter, A. M. James, P. Trávnícek, G. Watson, M. André, A. Eriksson y K. Torkar. "Cluster PEACE observations of electrons of spacecraft origin". Annales Geophysicae 19, n.º 10/12 (30 de septiembre de 2001): 1721–30. http://dx.doi.org/10.5194/angeo-19-1721-2001.

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Abstract. The two PEACE (Plasma Electron And Current Experiment) sensors on board each Cluster spacecraft sample the electron velocity distribution across the full 4<pi> solid angle and the energy range 0.7 eV to 26 keV with a time resolution of 4 s. We present high energy and angular resolution 3D observations of electrons of spacecraft origin in the various environments encountered by the Cluster constellation, including a lunar eclipse interval where the spacecraft potential was reduced but remained positive, and periods of ASPOC (Active Spacecraft POtential Control) operation which reduced the spacecraft potential. We demonstrate how the spacecraft potential may be found from a gradient change in the PEACE low energy spectrum, and show how the observed spacecraft electrons are confined by the spacecraft potential. We identify an intense component of the spacecraft electrons with energies equivalent to the spacecraft potential, the arrival direction of which is seen to change when ASPOC is switched on. Another spacecraft electron component, observed in the sunward direction, is reduced in the eclipse but unaffected by ASPOC, and we believe this component is produced in the analyser by solar UV. We find that PEACE anodes with a look direction along the spacecraft surfaces are more susceptible to spacecraft electron contamination than those which look perpendicular to the surface, which justifies the decision to mount PEACE with its field-of-view radially outward rather than tangentially.Key words. Magnetosheric physics (general or miscellaneous) Space plasma physics (spacecraft sheaths, wakes, charging)
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23

Rasca, A. P., S. Fatemi, W. M. Farrell, A. R. Poppe y Y. Zheng. "A Double Disturbed Lunar Plasma Wake". Journal of Geophysical Research: Space Physics, 28 de diciembre de 2020. http://dx.doi.org/10.1029/2020ja028789.

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24

Sreeraj, T., S. V. Singh y G. S. Lakhina. "Ion acoustic waves in lunar wake plasma". Advances in Space Research, enero de 2023. http://dx.doi.org/10.1016/j.asr.2023.01.034.

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25

Borovsky, Joseph E. y Gian Luca Delzanno. "Do Impulsive Solar-Energetic-Electron (SEE) Events Drive High-Voltage Charging Events on the Nightside of the Moon?" Frontiers in Astronomy and Space Sciences 8 (31 de mayo de 2021). http://dx.doi.org/10.3389/fspas.2021.655333.

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When the Earth’s moon is in the supersonic solar wind, the darkside of the Moon and the lunar plasma wake can be very dangerous charging environments. In the absence of photoelectron emission (dark) and in the absence of cool plasma (wake), the emission or collection of charge to reduce electrical potentials is difficult. Unique extreme charging events may occur during impulsive solar-energetic-electron (SEE) events when the lunar wake is dominated by relativistic electrons, with the potential to charge and differentially charge objects on and above the lunar surface to very-high negative electrical potentials. In this report the geometry of the magnetic connections from the Sun to the lunar nightside are explored; these magnetic connections are the pathways for SEEs from the Sun. Rudimentary charging calculations for objects in the relativistic-electron environment of the lunar wake are performed. To enable these charging calculations, secondary-electron yields for impacts by relativistic electrons are derived. Needed lunar electrical-grounding precautions for SEE events are discussed. Calls are made 1) for future dynamic simulations of the plasma wake in the presence of time-varying SEE-event relativistic electrons and time-varying solar-wind magnetic-field orientations and 2) for future charging calculations in the relativistic-electron wake environment and on the darkside lunar surface.
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26

Halekas, J. S. "Electrons and magnetic fields in the lunar plasma wake". Journal of Geophysical Research 110, A7 (2005). http://dx.doi.org/10.1029/2004ja010991.

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27

Nishino, Masaki N., Yoshiya Kasahara, Yuki Harada, Yoshifumi Saito, Hideo Tsunakawa, Atsushi Kumamoto, Shoichiro Yokota et al. "An event study on broadband electric field noises and electron distributions in the lunar wake boundary". Earth, Planets and Space 74, n.º 1 (4 de enero de 2022). http://dx.doi.org/10.1186/s40623-021-01566-2.

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AbstractWave–particle interactions are fundamental processes in space plasma, and some plasma waves, including electrostatic solitary waves (ESWs), are recognised as broadband noises (BBNs) in the electric field spectral data. Spacecraft observations in recent decades have detected BBNs around the Moon, but the generation mechanism of the BBNs is not fully understood. Here, we study a wake boundary traversal with BBNs observed by Kaguya, which includes an ESW event previously reported by Hashimoto et al. Geophys Res Lett 37:L19204 10.1029/2010GL044529 (2010). Focusing on the relation between BBNs and electron pitch-angle distribution functions, we show that upward electron beams from the nightside lunar surface are effective for the generation of BBNs, in contrast to the original interpretation by Hashimoto et al. Geophys Res Lett 37:L19204 10.1029/2010GL044529 (2010) that high-energy electrons accelerated by strong ambipolar electric fields excite ESWs in the region far from the Moon. When the BBNs were observed by the Kaguya spacecraft in the wake boundary, the spacecraft’s location was magnetically connected to the nightside lunar surface, and bi-streaming electron distributions of downward-going solar wind strahl component and upward-going field-aligned beams (at $$\sim$$ ∼ 124 eV) were detected. The interplanetary magnetic field was dominated by a positive $$B_Z$$ B Z (i.e. the northward component), and strahl electrons travelled in the antiparallel direction to the interplanetary magnetic field (i.e. southward), which enabled the strahl electrons to precipitate onto the nightside lunar surface directly. The incident solar wind electrons cause negative charging of the nightside lunar surface, which generates downward electric fields that accelerate electrons from the nightside surface toward higher altitudes along the magnetic field. The bidirectional electron distribution is not a sufficient condition for the BBN generation, and the distribution of upward electron beams seems to be correlated with the BBNs. Ambipolar electric fields in the wake boundary should also contribute to the electron acceleration toward higher altitudes and further intrusion of the solar wind ions into the deeper wake. We suggest that solar wind ion intrusion into the wake boundary is also an important factor that controls the BBN generation by facilitating the influx of solar wind electrons there. Graphical Abstract
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28

Zimmerman, M. I., T. L. Jackson, W. M. Farrell y T. J. Stubbs. "Plasma wake simulations and object charging in a shadowed lunar crater during a solar storm". Journal of Geophysical Research: Planets 117, E10 (17 de agosto de 2012). http://dx.doi.org/10.1029/2012je004094.

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