Plasmapause surface wave oscillates the magnetosphere and diffuse aurora

He, Fei; Guo, Ruilong; Dunn, W. R.; Yao, Zhonghua; Zhang, Hua-Sen; Hao, Yixin; Shi, Quanqi; Rong, Zhaojin; Liu, Jiang; Tian, Anmin; Zhang, Xiao‐Xin; Wei, Yong; Zhang, Yongliang; Zong, Qiugang; Pu, Z. Y.; Wan, Weixing

doi:10.1038/s41467-020-15506-3

Cited by 44 publications

(97 citation statements)

References 77 publications

(99 reference statements)

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“…The strong similarities shown by the surface waves near the plasmapause and the K-H waves near the magnetopause demonstrate the coupling of these waves via the eigenfrequency of the NEPS resonator (Mazur & Leonovich, 2006). The surface waves near the plasmapause were first identified by He et al (2020) as plasmapause surface waves. In this study, according to our specification, these plasmapause surface waves appeared in the hot zone.…”

Section: Discussionmentioning

confidence: 98%

“…As depicted by global auroral pictures, taken by the Defense Meteorological Satellite Program (DMSP) satellites in the topside ionosphere, large‐scale auroral undulations appear with amplitudes (∼40–400 km) and wavelengths (∼200–900 km), which are comparable, and can persist for up to 3.5 h (Lui et al., 1982; Nishitani et al., 1994). Large‐scale auroral undulations are also called sawtooth aurora (He et al., 2020) and giant undulations (Henderson et al., 2010). Typical features, which are consistent with the DMSP photographs‐shown characteristics (Lui et al., 1982), are also depicted by other types of images.…”

Section: Introductionmentioning

confidence: 99%

“…In this study, we investigate how the K‐H waves on the magnetopause impacted the subauroral and auroral regions during the strong May 27–29 and moderate July 16, 2017 geomagnetic storms in the coupled M‐I system, and the K‐H waves‐driven undulations in the NEPS, in the hot zone, on July 16, 2017. The significance of these storms is the prolonged detections of K‐H waves on the magnetopause on the dusk and dawn sides on May 29, 2017 (Lu et al., 2019) and the occurrence of plasmapause surface waves oscillating the diffuse aurora's equatorward edge on July 16, 2017 (He et al., 2020).…”

Section: Introductionmentioning

confidence: 99%

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Subauroral Flow Channel Structures and Auroral Undulations Triggered by Kelvin‐Helmholtz Waves

Horvath

Lovell

2021

JGR Space Physics

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The diffuse aurora appears as a quasi-circular band situated equatorward of the auroral oval wherein the discrete aurora forms. According to the classification of Feldshtein and Galperin (1996), the diffuse aurora maps along the magnetic field lines to the remnant layer of the radiation belt (L ≈ 4 R E ), overlapping with both the ring current (RC) and the Region 2 (R2) field-aligned currents (FACs), while the auroral oval maps to the full thickness (L ≈ 12 R E ) of the central plasma sheet (

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Section: Discussionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Subauroral Flow Channel Structures and Auroral Undulations Triggered by Kelvin‐Helmholtz Waves

Horvath

Lovell

2021

JGR Space Physics

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“…It is also very interesting to note that Zhang et al (2005) also find that a number of detached forms were associated with large-scale undulations in the equatorward boundary of the aurora found poleward, and He et al (2020) have recently shown that such auroral structuring is associated with actual structuring of the equatorial plasmapause. He et al (2020) also demonstrated that energetic electron and proton populations intrude into the low density regions which could be scattered to produce auroras.…”

Section: Detached Subauroral Patchesmentioning

confidence: 94%

Generation of Subauroral Longitudinally Extended Emissions Following Intensifications of the Poleward Boundary of the Substorm Bulge and Streamer Production

Henderson

2021

JGR Space Physics

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In the phenomenological model of auroral substorm development, first introduced by Akasofu (1964), the ionospheric disturbance begins with a brightening of an arc near the equatorward regions of the auroral distribution in the premidnight sector which can last for up to ∼5 min. Following this initial brightening phase, a rapid poleward motion ensues whereby an auroral "bulge" expands poleward, eastward, and westward to encompass wide sectors of the nightside auroral distribution. The bulge is comprised of intense active auroral bands at its poleward edge and typically develops a westward propagating wave-like "surge" at the westward edge of the poleward boundary (the so-called westward traveling surge [WTS]). There is often a decrease in luminosity below the active poleward boundary with significant structuring equatorward. The expansion phase of the substorm can last ∼0.5-1 h or more until the poleward boundary of the bulge merges with the pre-existing poleward arcs (that likely reside close to the open/closed field line boundary). The intensity and dynamics of the disturbance eventually subsides and recovers to its pre-existing configuration over a time scale of tens of minutes to hours and in the course of the auroral substorm process, other complex types of auroral forms can appear including torches, omega bands and pulsating patches. Over the years, numerous refinements have been made to this schematic, and we now have a very detailed picture of how the auroral substorm develops and how it is related to other types of auroral disturbances. Perhaps the most important early addition to the Akasofu picture was made by Montbriand (1969, 1971) who was the first to recognize a "previously unnoticed major feature of substorms" that he described as "… the occurrence of small, short-lived, clockwise rotating loops (as seen from above) which form along the PAB [Polar Activated Bands], rapidly orientate into an approximate north-south direction, and quickly degenerate into north-south oriented band segments. These occur between substorm time (ST) 10-15 min" after onset. Montbriand referred to these as North-South Segments (NSS), and they have since been referred Abstract Observations showing the development of Subauroral Longitudinally Extended Emigerssions on a global scale are presented. It is demonstrated that they occur as a separation of an eastwest arc-like band of luminosity that detaches away from the equatorward edge of the auroral distribution following episodes of auroral streamer production. They persist for time intervals on the order of ∼30 min and devolve into patchy disjointed segments before they fade. Emissions are seen in both 557.7 nm OI and 391.4 nm  2 N 1NG lines, and 630.0 nm emissions are often observed equatorward. The 391.4 nm emissions are typically weaker and fade away more quickly than the 557.7 nm emissions, suggesting that an auroral precipitation source is initially present but is rapidly depleted as the forms age. All cases are associated with enhanced Subauroral Polarization Stream (S...

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“…The nighttime ionospheric disk image can be used to investigate the structure and Optical Remote Sensing of Planetary Space Environment DOI: http://dx.doi.org/10.5772/intechopen.98427 evolution of equatorial ionization anomaly [25]. The auroral image can be used to manifest the thermal plasma transportation in the Earth's magnetosphere and to denote the substorm activity in Earth's space [26]. The plasmaspheric images can be used to characterize the large-scale convections in the Earth's magnetosphere [27,28].…”

Section: Optical Remote Sensing Images Of Planetary Spacementioning

confidence: 99%

Optical Remote Sensing of Planetary Space Environment

He¹,

Yao²,

Wei³

2022

Recent Remote Sensing Sensor Applications - Satellites and Unmanned Aerial Vehicles (UAVs)

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Planetary science is the scientific investigations of the basic characteristics and the formation and evolution processes of the planets, moons, comets, asteroids and other minor bodies of the solar system, the exoplanets, and the planetary systems. Planetary scientific research mainly depends on deep space exploration, and it is highly interdisplinary and is built from Earth science, space science, astronomy and other relevant disciplines. Planetary space, a critical region of mass and energy exchange between the planet and the interplanetary space, is an integral part of the planetary multi-layer coupling system. Atmospheres of different compositions and plasmas of different densities and energies exist in planetary space, where mass transportation at different temporal and spatial scales and various energy deposition and dissipation processes occur. Optical remote sensing overcomes the difficulties of capturing global views and distinguishing spatiotemporal variations in in-situ particle and field detections. This chapter introduces the principles and applications of optical remote sensing in planetary science. The first ground-based planetary observatory in China, the Lenghu Observation Center for Planetary Sciences, will be introduced in detail. Future development of optical remote sensing platforms in Chinese planetary exploration program will also be introduced.

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Plasmapause surface wave oscillates the magnetosphere and diffuse aurora

Cited by 44 publications

References 77 publications

Subauroral Flow Channel Structures and Auroral Undulations Triggered by Kelvin‐Helmholtz Waves

Subauroral Flow Channel Structures and Auroral Undulations Triggered by Kelvin‐Helmholtz Waves

Generation of Subauroral Longitudinally Extended Emissions Following Intensifications of the Poleward Boundary of the Substorm Bulge and Streamer Production

Optical Remote Sensing of Planetary Space Environment

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