The Characteristic Response of Whistler Mode Waves to Interplanetary Shocks

Yue, Chao; Chen, Lunjin; Bortnik, J.; Ma, Q.; Thorne, R. M.; Angelopoulos, V.; Li, Jinxing; An, Xin; Zhou, Chen; Kletzing, C. A.; Reeves, G. D.; Spence, H. E.

doi:10.1002/2017ja024574

Cited by 34 publications

(50 citation statements)

References 72 publications

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“…The comparatively weaker presence/impact of stochastic effects at L < 5-5.5 than near L = 6.6 probably explains the higher correlation of SampEn(P * ) with SampEn(ap) than with SampEn(AE) in Figures 5 and 6. The significant correlation between SampEn(P * ) and SampEn(ap) also agrees with recent studies showing that fast streams in the solar wind correspond to high Kp intervals (Denton et al, 2006) and are strong drivers of ∼10-day periods of strongly regulated particle dynamics at L ∼ 3.5-5 in the heart of the outer radiation belt (Li et al, 2015;Mourenas et al, 2019;Yue et al, 2017).…”

Section: Entropy Correlations Between Geomagnetic Indices and Energetsupporting

confidence: 90%

Dynamical Properties of Peak and Time‐Integrated Geomagnetic Events Inferred From Sample Entropy

2020

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We provide a comprehensive statistical analysis of the sample entropy of peak and time‐integrated geomagnetic events in 2001–2017, considering different measures of event strength, different geomagnetic indices, and a simplified solar wind‐magnetosphere coupling function P*. Our investigations reveal the existence of significant correlations between the entropies of Dst, ap, and P*, and between such entropies and event strengths, as well as good correlations between peak levels of solar wind‐magnetosphere coupling and ring current ( Dst) and ap entropies, suggesting a potential predictability of significant Dst and ap events on the basis of appropriate functions of P*. Sensibly weaker correlations are found with AE entropy. We further show the presence of several significant entropy correlations between geomagnetic indices, solar wind‐magnetosphere coupling, and trapped or precipitated energetic electron and ion fluxes measured by geostationary and low Earth orbit satellites in the outer radiation belt during the same periods. Entropy correlations between Dst and trapped or precipitated 30‐ to 80‐keV ion fluxes at low L and between AE and trapped 40‐keV electron fluxes at geostationary orbit correspond well with ring current properties and substorm‐induced injections, respectively. Entropy correlations between ap and precipitation rates of energetic ion and electron fluxes demonstrate the sensibility of ap index entropy to both low‐energy (5–30 keV) electron injections and ring current. The stronger entropy correlation between solar wind‐magnetosphere coupling and ap than AE likely stems from the more stochastic behavior of electron injections and fast losses near geostationary orbit.

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Section: Entropy Correlations Between Geomagnetic Indices and Energetsupporting

confidence: 90%

Dynamical Properties of Peak and Time‐Integrated Geomagnetic Events Inferred From Sample Entropy

2020

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“…All these global characteristics agree with the results of ray‐tracing codes that show a possible generation of hiss through inward propagation of chorus waves (Bortnik et al, ; Chen et al, ; Meredith et al, ). Similarly, close relationships between chorus and hiss have also been found by analyzing the global response of these waves to interplanetary disturbances in recent event (Liu et al, ; Liu et al, ; Su et al, ) and statistical studies (Yue et al, ).…”

Section: Spatial Scales Of the Generation Regions Of Chorus And Hissmentioning

confidence: 72%

Spatial Extent and Temporal Correlation of Chorus and Hiss: Statistical Results From Multipoint THEMIS Observations

et al. 2018

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The spatial localization of whistler mode waves, determined by their generation process, propagation, and damping, is important for assessing the efficiency of wave-particle interactions and the dynamics of the radiation belts. We use 11 years of multipoint wave measurements in 2007-2017 from five Time History of Events and Macroscale Interactions during Substorms (THEMIS) spacecraft covering L = 2-10 at low magnetic latitudes over all magnetic local times (MLTs) to characterize both the instantaneous spatial extent of chorus and hiss active regions and their wave amplitude distribution in the vicinity of their respective generation regions, making use of the time domain correlation technique. The correlation of lower band chorus wave power dynamics from two spacecraft measurements remains significant up to 250-800 km transverse to the background magnetic field, in agreement with the typical scale of a chorus element, with a shorter correlation length for higher peak wave power. Additionally, a coordinated analysis of average chorus amplitudes at separate locations shows that the radial extent of the chorus active region varies from 0.2 R E on the nightside to 1 R E on the dayside, with an azimuthal width of 1 MLT. The wave power correlation scale of hiss has no fine structure and is generally larger (1,500-3,000 km); its correlation remains nonnegligible up to 1.5 R E . Such observations are consistent with chorus generation by localized electron injections and subsequent hiss amplification at lower L shells from seed chorus waves having propagated and spread over a wider region inside the plasmasphere. The connection between hiss and chorus is further explored statistically through the correlation between their respective wave power variations, suggesting a significant link between them.

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“…The intense magnetosonic waves were observable only in the period from 03:33 UT to 05:24 UT with the enhanced solar wind dynamic pressure. Other interesting features of Figure S3 are the dramatic responses of whistler mode hiss and chorus waves to the solar wind dynamic pressure variations, which have been studied recently in detail Liu, Su, Gao, Reeves, et al, 2017;Yue et al, 2017). For the electromagnetic ion cyclotron waves destabilized by the comparable energy protons to those for the magnetosonic wave excitation, the solar wind compression has long been recognized as an important trigger (e.g., Anderson & Hamilton, 1993;Cho et al, 2017;McCollough et al, 2010;Usanova et al, 2008).…”

Section: Conclusion and Discussionmentioning

confidence: 89%

Prompt Disappearance and Emergence of Radiation Belt Magnetosonic Waves Induced by Solar Wind Dynamic Pressure Variations

Liu

Zheng

et al. 2018

Geophysical Research Letters

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Magnetosonic waves are highly oblique whistler mode emissions transferring energy from the ring current protons to the radiation belt electrons in the inner magnetosphere. Here we present the first report of prompt disappearance and emergence of magnetosonic waves induced by the solar wind dynamic pressure variations. The solar wind dynamic pressure reduction caused the magnetosphere expansion, adiabatically decelerated the ring current protons for the Bernstein mode instability, and produced the prompt disappearance of magnetosonic waves. On the contrary, because of the adiabatic acceleration of the ring current protons by the solar wind dynamic pressure enhancement, magnetosonic waves emerged suddenly. In the absence of impulsive injections of hot protons, magnetosonic waves were observable even only during the time period with the enhanced solar wind dynamic pressure. Our results demonstrate that the solar wind dynamic pressure is an essential parameter for modeling of magnetosonic waves and their effect on the radiation belt electrons.

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The Characteristic Response of Whistler Mode Waves to Interplanetary Shocks

Cited by 34 publications

References 72 publications

Dynamical Properties of Peak and Time‐Integrated Geomagnetic Events Inferred From Sample Entropy

Dynamical Properties of Peak and Time‐Integrated Geomagnetic Events Inferred From Sample Entropy

Spatial Extent and Temporal Correlation of Chorus and Hiss: Statistical Results From Multipoint THEMIS Observations

Prompt Disappearance and Emergence of Radiation Belt Magnetosonic Waves Induced by Solar Wind Dynamic Pressure Variations

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