Energetic electron (&gt;10 keV) microburst precipitation, ~5–15 s X‐ray pulsations, chorus, and wave‐particle interactions: A review

Tsurutani, B. T.; Lakhina, G. S.; Verkhoglyadova, O. P.

doi:10.1002/jgra.50264

Cited by 93 publications

(107 citation statements)

References 113 publications

(220 reference statements)

Supporting

Mentioning

105

Contrasting

Order By: Relevance

“…Chorus waves can interact strongly with electrons over a wide energy range from a few hundred electron volts up to several megaelectron volts via Doppler shifted cyclotron resonance [ Horne and Thorne , ]. These cyclotron resonant interactions result in pitch angle diffusion of electrons into the loss cone and, hence, due to the bursty nature of the waves, they have been associated with bursts of precipitation observed by balloons and satellites at low altitudes [ Rosenberg et al , ; Imhof et al , ; Lorentzen et al , ; Saito et al , ; Tsurutani et al , ] and the loss of electrons from the radiation belts into the atmosphere. Pitch angle scattering by chorus is also largely responsible for both the diffuse aurora [ Thorne et al , ; Ni et al , ] and pulsating aurora [ Nishimura et al , ; Miyoshi et al , ].…”

Section: Introductionmentioning

confidence: 99%

A new diffusion matrix for whistler mode chorus waves

et al. 2013

View full text Add to dashboard Cite

[1] Global models of the Van Allen radiation belts usually include resonant wave-particle interactions as a diffusion process, but there is a large uncertainty over the diffusion rates. Here we present a new diffusion matrix for whistler mode chorus waves that can be used in such models. Data from seven satellites are used to construct 3536 power spectra for upper and lower band chorus for 1.5 Ä L * Ä 10 MLT, magnetic latitude 0 ı Ä | m | Ä 60 ı and five levels of K p . Five density models are also constructed from the data. Gaussian functions are fitted to the spectra and capture typically 90% of the wave power. The frequency maxima of the power spectra vary with L * and are typically lower than that used previously. Lower band chorus diffusion increases with geomagnetic activity and is largest between 21:00 and 12:00 MLT. Energy diffusion extends to a few megaelectron volts at large pitch angles > 60 ı and at high energies exceeds pitch angle diffusion at the loss cone. Most electron diffusion occurs close to the geomagnetic equator (< 12 ı ). Pitch angle diffusion rates for lower band chorus increase with L * and are significant at L * = 8 even for low levels of geomagnetic activity, while upper band chorus is restricted to mainly L * < 6. The combined drift and bounce averaged diffusion rates for upper and lower band chorus extend from a few kiloelectron volts near the loss cone up to several megaelectron volts at large pitch angles indicating loss at low energies and net acceleration at high energies.

show abstract

Section: Introductionmentioning

confidence: 99%

A new diffusion matrix for whistler mode chorus waves

et al. 2013

View full text Add to dashboard Cite

show abstract

“…The energetic electron component creates electromagnetic chorus waves through the loss cone instability (Tsurutani and Smith, 1977;Meredith et al, 2001;Tsurutani et al, 2013). Then the chorus accelerates the high-energy electrons to relativistic energies by resonant interactions (Inan et al, 1978;Horne and Thorne, 1998;Thorne et al, 2005Thorne et al, , 2013Summers et al, 2007;Reeves et al, 2013;Boyd et al, 2014;Hajra et al, 2015a).…”

Section: F L Guarnieri Et Al: a Correlation Study Regarding The Aementioning

confidence: 99%

A correlation study regarding the AE index and ACE solar wind data for Alfvénic intervals using wavelet decomposition and reconstruction

Guarnieri

Tsurutani

Vieira

et al. 2018

Nonlin. Processes Geophys.

Self Cite

View full text Add to dashboard Cite

Abstract. The purpose of this study is to present a wavelet interactive filtering and reconstruction technique and apply this to the solar wind magnetic field components detected at the L1 Lagrange point ∼ 0.01 AU upstream of the Earth. These filtered interplanetary magnetic field (IMF) data are fed into a model to calculate a time series which we call AE * . This model was adjusted assuming that magnetic reconnection associated with southward-directed IMF B z is the main mechanism transferring energy into the magnetosphere. The calculated AE * was compared to the observed AE (auroral electrojet) index using cross-correlation analysis. The results show correlations as high as 0.90. Empirical removal of the high-frequency, short-wavelength Alfvénic component in the IMF by wavelet decomposition is shown to dramatically improve the correlation between AE * and the observed AE index. It is envisioned that this AE * can be used as the main input for a model to forecast relativistic electrons in the Earth's outer radiation belts, which are delayed by ∼ 1 to 2 days from intense AE events.

show abstract

“…The same general feature is expected for ∼10-100 keV electron microbursts. The interaction time scales between the energetic electrons and chorus subelements are ∼3 ms [Tsurutani et al, , 2013b. But again, the chorus subelement scale sizes are irregular and thus the microburst substructures will be as well.…”

Section: Final Commentsmentioning

confidence: 99%

Electromagnetic cyclotron waves in the dayside subsolar outer magnetosphere generated by enhanced solar wind pressure: EMIC wave coherency

et al. 2015

View full text Add to dashboard Cite

Electromagnetic ion (proton) cyclotron (EMIC) waves and whistler mode chorus are simultaneously detected in the Earth's dayside subsolar outer magnetosphere. The observations were made near the magnetic equator 3.1°–1.5° magnetic latitude at 1300 magnetic local time from L = 9.9 to 7.0. It is hypothesized that the solar wind external pressure caused preexisting energetic 10–100 keV protons and electrons to be energized in the T⊥ component by betatron acceleration and the resultant temperature anisotropy (T⊥>T∥) formed led to the simultaneous generation of both EMIC (ion) and chorus (electron) waves. The EMIC waves had maximum wave amplitudes of ∼6 nT in a ∼60 nT ambient field B0. The observed EMIC wave amplitudes were about ∼10 times higher than the usually observed chorus amplitudes (∼0.1–0.5 nT). The EMIC waves are found to be coherent to quasi‐coherent in nature. Calculations of relativistic ∼1–2 MeV electron pitch angle transport are made using the measured wave amplitudes and wave packet lengths. Wave coherency was assumed. Calculations show that in a ∼25–50 ms interaction with an EMIC wave packet, relativistic electron can be transported ∼27° in pitch. Assuming dipole magnetic field lines for a L = 9 case, the cyclotron resonant interaction is terminated ∼±20° away from the magnetic equator due to lack of resonance at higher latitudes. It is concluded that relativistic electron anomalous cyclotron resonant interactions with coherent EMIC waves near the equatorial plane is an excellent loss mechanism for these particles. It is also shown that E > 1 MeV electrons cyclotron resonating with coherent chorus is an unlikely mechanism for relativistic microbursts. Temporal structures of ∼30 keV precipitating protons will be ∼2–3 s which will be measurable at the top of the ionosphere.

show abstract

Energetic electron (>10 keV) microburst precipitation, ~5–15 s X‐ray pulsations, chorus, and wave‐particle interactions: A review

Cited by 93 publications

References 113 publications

A new diffusion matrix for whistler mode chorus waves

A new diffusion matrix for whistler mode chorus waves

A correlation study regarding the AE index and ACE solar wind data for Alfvénic intervals using wavelet decomposition and reconstruction

Electromagnetic cyclotron waves in the dayside subsolar outer magnetosphere generated by enhanced solar wind pressure: EMIC wave coherency

Contact Info

Product

Resources

About