Response of plasmaspheric configuration to substorms revealed by Chang’e 3

He, Hongliang; Shen, C.; Wang, Huaning; Zhang, Xiaoxin; Chen, Bin; Yan, Jun; Zou, Yongliao; Jorgensen, A. M.; He, Fei; Yan, Yan; Zhu, Xiaoshuai; Huang, Ya; Xu, Rongbin

doi:10.1038/srep32362

Cited by 22 publications

(12 citation statements)

References 65 publications

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“…Figure 3a shows the EMFISIS electron density, determined by tracking the upper hybrid resonance frequency (Kurth et al, 2015). We use the electron density as a proxy for plasmaspheric density and determine plasmasphere boundaries and trough regions by noting sharp changes in the electron density profile (He et al, 2016). Between 5:30 UT and 6:30 UT, Probe A observed two density channels in the plasmaspheric density profile between 17 and 19 MLT, L‐shells from 3 to 4, and near the geomagnetic equator, with magnetic latitudes ranging from 3° to 6°.…”

Section: Observations Of Magnetosonic Waves and O+ Heating Eventsmentioning

confidence: 99%

Local Heating of Oxygen Ions in the Presence of Magnetosonic Waves: Possible Source for the Warm Plasma Cloak?

et al. 2020

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In the energy regime between the plasmasphere (a few eV) and the ring current (greater than 1 keV), there exists another magnetospheric particle population with energies from a few eV to a few keV, the origins of which are debated. Studies explore generation mechanisms for warm plasma energies in the inner magnetosphere through two observed phenomena: the warm plasma cloak and the oxygen torus. The relations between these two populations are unclear. Recent data reveal local heating of cold H+ and He+ ions to warm plasma energies by magnetosonic waves. In this study, we report first observations of thermal O+ heating by magnetosonic waves and link the heating to a possible formation mechanism for the warm plasma cloak. The O+ heating is observed by different plasmaspheric density profiles, including density channels. We observe that O+ heating always occurs with thermal H+ and He+ heating. We investigate the harmonic structure of the observed magnetosonic waves and find intense O+ heating is accompanied by discrete heavy ion gyroharmonics. We suggest that locally heated thermal ions to 100s eV by magnetosonic waves along the plasmapause could provide a possible mechanism for warm plasma cloak generation.

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Section: Observations Of Magnetosonic Waves and O+ Heating Eventsmentioning

confidence: 99%

Local Heating of Oxygen Ions in the Presence of Magnetosonic Waves: Possible Source for the Warm Plasma Cloak?

et al. 2020

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“…This implies a causal relationship between the substorms and the formation of the three bulges on the plasmasphere. The measurements suggest that there is a strong negative correlation between the plasmaspheric configuration and geomagnetic activity intensity [19].…”

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confidence: 88%

New achievements from CE-3 mission

Zou

Wang

Yan

et al. 2017

Sci. China Phys. Mech. Astron.

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The Chang'E-3 (CE-3) mission began with a smooth countdown and flawless launch on the Long March 3B rocket from the Xichang satellite launch center at 01:30 CST on December 2, 2013. It landed on the northeastern Imbrium basin (340.49°E, 44.12°N) at 21:11 CST on December 14, 2013, and the Yutu rover was deployed from the lander the next morning at 04:35.The lander was equipped with a number of remote-sensing instruments including the landing camera (LCAM), terrain camera (TCAM), extreme ultraviolet camera (EUVC), and lunar-based ultraviolet telescope (LUT). The Yutu rover successfully carried the panoramic camera (PCAM), VIS-NIR imaging spectrometer (VNIS), active particle-induced X-ray spectrometer (APXS), and lunar penetrating radar (LPR) [1][2][3].Three cameras (LCAM, TCAM, and PCAM) investigated the morphological features and geological structures near the landing area. The EUVC monitored activities in the Earth's plasmasphere at extreme ultraviolet wavelengths (measurement band center frequency 30.4±0.5 nm, bandwidth ≤5 nm). The LUT performed astronomical observations at near-ultraviolet wavelengths (245-340 nm). The VNIS (visible-nearinfrared 450-950 nm, short-wave infrared 900-2400 nm) and APXS detected the mineralogical and chemical compositions along the traverse path. The LPR obtained pioneering measurements of the lunar subsurface.After the lander released the Yutu rover, the eight science instruments began operating. The Yutu rover started traversing along a planned path covering a distance of 114 m. *Corresponding author (email: wangqin@bao.ac.cn) To analyze the topography, landform, and geology of the area surrounding the landing site (Sinus Iridum and 45 km× 70 km of the landing area), high-resolution topography data, image data, and geological data were obtained [4].Thus far, eight science instrument calibration procedures, data processing methods, and inversion models have been completed [5][6][7][8][9][10][11][12]. The total science data size was 6.69 TB as of April 4, 2016.The LPR detection and integrated TCAM & PCAM data interpretation have identified more than seven subsurface layers, suggesting that the landing region has experienced complex geological processes such as basalts and pyroclastic have filled in the Imbrium basin since the Imbrian (3.9-3.2 Ga) and Eratosthenian (3.2-1.5 Ga) epochs [3]. The LPR and PCAM data provides a higher resolution to estimate lunar regolith parameters such as permittivity, density, conductivity, and FeO+TiO 2 content. The surface regolith thickness of the CE-3 landing area is (1.24±0.10) m. Meteorite impacts might have been a vital influence to the thickness and growth rate of the regolith [13].The LPR consists of two types of antenna with two channels: 60 (Channel 1) and 500 MHz (Channel 2). The LPR observations at 500 MHz reveal four major stratigraphic zones from the surface to a depth of 20 m: a layered reworked zone (<1 m), ejecta layer (~2-6 m), paleoregolith layer (~4-11 m), and the underlying mare basalts. In addition, the LPR measurements indica...

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“…Other released magnetic energy is transferred to CMEs and SEPs associated with flares. Big solar flares and the associated CMEs and SEPs can cause severe disturbances to the space weather condition in the solar-terrestrial space as well as in the whole heliosphere [14,[23][24][25].…”

Section: Author Detailsmentioning

confidence: 99%

Variation of Coronal Magnetic Field and Solar Flare Eruption

He¹

2020

Nanofluid Flow in Porous Media

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Solar flares are prominent eruptive phenomenon happening in the solar atmosphere. Major flares usually come from solar active regions (ARs) where strong and concentrated bipolar magnetic field exists and manifests as dark sunspots in photosphere. The photospheric magnetic field acts as the bottom boundary of corona system and confines the magnetic structure of the corona. For complex ARs, the coronal magnetic field generally contains electric current around the magnetic polarity inversion lines, which corresponds to the nonpotential magnetic field and manifests as twisted field lines. The coronal magnetic field structure evolves as the response to the variations of the photospheric magnetic field. This coronal evolution can be quasi-steady and approximated by the force-free condition. In some situations, the variations of photospheric magnetic field may cause sudden changes of topological structure of coronal magnetic field at certain sites in the corona. The plasmas at these sites lost equilibrium and are ejected from their original positions. This process is accompanied with magnetic reconnection and leads to the release of magnetic energy in the corona. Part of the released magnetic energy is converted to the electromagnetic emission which manifests as sudden brightening across a broad range of electromagnetic wave spectrum, and hence the flare phenomenon is initiated.

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Response of plasmaspheric configuration to substorms revealed by Chang’e 3

Cited by 22 publications

References 65 publications

Local Heating of Oxygen Ions in the Presence of Magnetosonic Waves: Possible Source for the Warm Plasma Cloak?

Local Heating of Oxygen Ions in the Presence of Magnetosonic Waves: Possible Source for the Warm Plasma Cloak?

New achievements from CE-3 mission

Variation of Coronal Magnetic Field and Solar Flare Eruption

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