Electric fields and large-scale undulations in the evening sector of the diffuse auroral zone

Baishev, D. G.; Barkova, E. S.; Степанов, А. А.; Rich, F. J.; Yumoto, K.

doi:10.1134/s0016793210010056

Cited by 5 publications

(11 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…[] report amplitudes of 40–400 km in the atmosphere, Kelley [] report amplitudes of 30–300 km in the atmosphere, and Biashev et al . [] report amplitudes of 100–150 km in the atmosphere. The smaller of these amplitudes correspond to ~0.1–0.2 R E radial displacements in the equatorial plane.…”

Section: Potential Sources Of the Long‐lived Plasmaspheric Plumesmentioning

confidence: 99%

Long‐lived plasmaspheric drainage plumes: Where does the plasma come from?

et al. 2014

View full text Add to dashboard Cite

Long-lived (weeks) plasmaspheric drainage plumes are explored. The long-lived plumes occur during long-lived high-speed-stream-driven storms. Spacecraft in geosynchronous orbit see the plumes as dense plasmaspheric plasma advecting sunward toward the dayside magnetopause. The older plumes have the same densities and local time widths as younger plumes, and like younger plumes they are lumpy in density and they reside in a spatial gap in the electron plasma sheet (in sort of a drainage corridor). Magnetospheric-convection simulations indicate that drainage from a filled outer plasmasphere can only supply a plume for 1.5-2 days. The question arises for long-lived plumes (and for any plume older than about 2 days): Where is the plasma coming from? Three candidate sources appear promising: (1) substorm disruption of the nightside plasmasphere which may transport plasmaspheric plasma outward onto open drift orbits, (2) radial transport of plasmaspheric plasma in velocity-shear-driven instabilities near the duskside plasmapause, and (3) an anomalously high upflux of cold ionospheric protons from the tongue of ionization in the dayside ionosphere, which may directly supply ionospheric plasma into the plume. In the first two cases the plume is drainage of plasma from the magnetosphere; in the third case it is not. Where the plasma in long-lived plumes is coming from is a quandary: to fix this dilemma, further work and probably full-scale simulations are needed.

show abstract

Section: Potential Sources Of the Long‐lived Plasmaspheric Plumesmentioning

confidence: 99%

Long‐lived plasmaspheric drainage plumes: Where does the plasma come from?

et al. 2014

View full text Add to dashboard Cite

show abstract

“…The performed theoretical studies (e.g., (Kelley, 1986;Yamamoto et al, 1993Yamamoto et al, , 1994Goldstein et al, 2005)) indicate that SAPS is of paramount importance in the development of the instability at the plasmapause or at the plasma sheet inner edge. Below, we will briefly analyze the experimental studies illustrated in several works (Kelley, 1986;Zhang et al, 2005;Henderson et al, 2010;Baishev et al, 2010) in order to support this hypothesis. No.…”

Section: Resultsmentioning

confidence: 91%

“…In the LAU event studied in (Baishev et al, 2010) based on the DMSP data, considerable ion drift veloc ity gradients in the luminosity undulation generation region were, on the contrary, related to an unexpected appearance of a "standstill" band (the convection velocity Vc ≈ 0) near the poleward edge of intense elec tron and ion precipitation rather than to an enhanced convection stream. Such a behavior of the drift veloc ity and auroral precipitation characteristics can corre spond to the transition from the diffuse luminosity region to bright discrete auroras at the poleward edge of this region.…”

Section: Resultsmentioning

confidence: 97%

“…Such a behavior of the drift veloc ity and auroral precipitation characteristics can corre spond to the transition from the diffuse luminosity region to bright discrete auroras at the poleward edge of this region. In this case we should take into account that a substantial longitudinal difference exists between the DMSP satellite trajectory and the loca tion of Tiksi observatory, the optical observations at which were used in (Baishev et al, 2010).…”

Section: Resultsmentioning

confidence: 99%

“…It is insufficiently clear whether sub storm activity substantially affects the generation of luminosity undulations. Thus, Baishev et al (2010) considered the LAU event on December 12, 2004, when the ground based all sky camera registered eight lumi nosity undulations with a 100-150 km amplitude and a wavelength of 200-300 km at Tiksi observatory. This event lasted ~1 h during a relatively quiet period Polar Geophysical Institute, Apatity Division, Kola Scientific Center, Russian Academy of Sciences, ul.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Large amplitude undulations of evening site diffuse aurorae. Optical characteristics and conditions of generation

2015

View full text Add to dashboard Cite

Optical characteristics of large amplitude undulations (LAU) of diffuse aurorae observed by all sky cameras at Kola Peninsula on December 28, 2010 were examined. Both interplanetary medium condi tions and characteristics of magnetic activity before and during LAU were analyzed. It was shown that the development of undulations could be activated by sharp short living of ~20 minutes solar wind dynamic pres sure impulse and existence of the undulations during about two hours was supported by electric field of sta tionary magnetospheric convection originated from large smoothly changed southward IMF Bz component of about -12nT. The altitude of undulation luminosity determined by triangulation method was 120 ± 10 km. The undulations amplitude changed from about 100 to 300 km and the average wavelength was ~250 km. The undulations were observed moving westward with the average phase velocity of ~0.7 km/s. The pass of DMSP F16 spacecraft just along "the tongue" of undulations showed that the wave of luminosity was located in the region of the predominantly ion (proton) precipitation with the average energy of particles of ~18 keV. Rayed auroral structures were observed continuously in the region of diffuse aurorae during time interval of LAU existence. These structures were observed moving westward with the velocity of about 2 km/s that corresponds to the northward electric field of ~100 mV/m.

show abstract

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

Horvath

Lovell

2021

JGR Space Physics

View full text Add to dashboard Cite

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 (

show abstract

Electric fields and large-scale undulations in the evening sector of the diffuse auroral zone

Cited by 5 publications

References 7 publications

Long‐lived plasmaspheric drainage plumes: Where does the plasma come from?

Long‐lived plasmaspheric drainage plumes: Where does the plasma come from?

Large amplitude undulations of evening site diffuse aurorae. Optical characteristics and conditions of generation

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

Contact Info

Product

Resources

About