Relativistic Electron Microburst Events: Modeling the Atmospheric Impact

Seppälä, Annika; Douma, Emma; Rodger, Craig J.; Verronen, Pekka T.; Clilverd, Mark A.; Bortnik, J.

doi:10.1002/2017gl075949

Cited by 28 publications

(35 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using these spectra, we calculate how many microbursts it would take to reduce the flux tube population of any given energy (in the range 100 keV to 7 MeV) to 1%. We then apply the statistically average microburst occurrence rate of three microbursts per minute (discussed in greater detail in Seppälä et al, 2018) and the extreme microburst occurrence rate of 50 microbursts per minute (based on an extreme case that will be discussed in a future study) to estimate the time taken to reduce the total flux tube population at any given energy down to 1%.…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Characteristics of Relativistic Microburst Intensity From SAMPEX Observations

et al. 2019

Self Cite

View full text Add to dashboard Cite

Relativistic electron microbursts are an important electron loss process from the radiation belts into the atmosphere. These precipitation events have been shown to significantly impact the radiation belt fluxes and atmospheric chemistry. In this study we address a lack of knowledge about the relativistic microburst intensity using measurements of 21,746 microbursts from the Solar Anomalous Magnetospheric Particle Explorer (SAMPEX). We find that the relativistic microburst intensity increases as we move inward in L, with a higher proportion of low‐intensity microbursts (<2,250 [MeV cm2 sr s]−1) in the 03–11 magnetic local time region. The mean microburst intensity increases by a factor of 1.7 as the geomagnetic activity level increases and the proportion of high‐intensity relativistic microbursts (>2,250 [MeV cm2 sr s]−1) in the 03–11 magnetic local time region increases as geomagnetic activity increases, consistent with changes in the whistler mode chorus wave activity. Comparisons between relativistic microburst properties and trapped fluxes suggest that the microburst intensities are not limited by the trapped flux present alongside the scattering processes. However, microburst activity appears to correspond to the changing trapped flux; more microbursts occur when the trapped fluxes are enhancing, suggesting that microbursts are linked to processes causing the increased trapped fluxes. Finally, modeling of the impact of a published microburst spectra on a flux tube shows that microbursts are capable of depleting <500‐keV electrons within 1 hr and depleting higher‐energy electrons in 1–23 hr.

show abstract

Section: Discussionmentioning

confidence: 99%

“…Based on these relatively new studies, Breneman et al (2017), Greeley et al (2019), and Seppälä et al (2018), we now know that relativistic microbursts are not only a significant loss process from the electron radiation belts but also a significant driver of chemical changes and subsequently ozone loss in the atmosphere.…”

Section: Introductionmentioning

confidence: 99%

Characteristics of Relativistic Microburst Intensity From SAMPEX Observations

et al. 2019

Self Cite

View full text Add to dashboard Cite

show abstract

“…Atmospheric effects of solar D protons and auroral electrons (energy < 30 keV) have been studied extensively over the last few decades (Crutzen, 1979;Funke et al, 2011;Jackman et al, 1995;Jackman & McPeters, 2004;Jackman et al, 2008;Jackman et al, 2009;López-Puertas et al, 2005;Orsolini et al, 2005;Roble & Rees, 1977). Particularly in the past several years, more attention has been paid to medium energy electron (MEE,~30-1,000 keV) and high-energy electron (HEE, >1 MeV) precipitation influences on the atmosphere (Andersson et al, 2018;Clilverd et al, 2013;Newnham et al, 2018;Seppälä et al, 2018;Verronen et al, 2015). Evaluating two different energetic electron precipitation (EEP) data sets for inclusion in global climate models, both of which include MEE precipitation inferred from the Medium Energy Proton and Electron Detector (MEPED) instruments, is the focus of this paper.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric Effects of >30‐keV Energetic Electron Precipitation in the Southern Hemisphere Winter During 2003

Pettit

Randall

Peck³

et al. 2019

JGR Space Physics

Self Cite

View full text Add to dashboard Cite

The atmospheric effects of precipitating electrons are not fully understood, and uncertainties are large for electrons with energies greater than ~30 keV. These electrons are underrepresented in modeling studies today, primarily because valid measurements of their precipitating spectral energy fluxes are lacking. This paper compares simulations from the Whole Atmosphere Community Climate Model (WACCM) that incorporated two different estimates of precipitating electron fluxes for electrons with energies greater than 30 keV. The estimates are both based on data from the Polar Orbiting Environmental Satellite Medium Energy Proton and Electron Detector (MEPED) instruments but differ in several significant ways. Most importantly, only one of the estimates includes both the 0° and 90° telescopes from the MEPED instrument. Comparisons are presented between the WACCM results and satellite observations poleward of 30°S during the austral winter of 2003, a period of significant energetic electron precipitation. Both of the model simulations forced with precipitating electrons with energies >30 keV match the observed descent of reactive odd nitrogen better than a baseline simulation that included auroral electrons, but no higher energy electrons. However, the simulation that included both telescopes shows substantially better agreement with observations, particularly at midlatitudes. The results indicate that including energies >30 keV and the full range of pitch angles to calculate precipitating electron fluxes is necessary for improving simulations of the atmospheric effects of energetic electron precipitation.

show abstract

“…4.2), which find their closure through ionospheric horizontal currents in the ionosphere (e.g. Sergeev et al, 1996), which is a resistive medium as neutral and charged particles undergo collisions. Ultimately, the power density dissipated by JH is according to Poynting's theorem j • E, where j is the electric current density and E the electric field in the frame of the neutral gas.…”

Section: Joule Heatingmentioning

confidence: 99%

Lower-thermosphere–ionosphere (LTI) quantities: current status of measuring techniques and models

et al. 2021

Self Cite

View full text Add to dashboard Cite

Abstract. The lower-thermosphere–ionosphere (LTI) system consists of the upper atmosphere and the lower part of the ionosphere and as such comprises a complex system coupled to both the atmosphere below and space above. The atmospheric part of the LTI is dominated by laws of continuum fluid dynamics and chemistry, while the ionosphere is a plasma system controlled by electromagnetic forces driven by the magnetosphere, the solar wind, as well as the wind dynamo. The LTI is hence a domain controlled by many different physical processes. However, systematic in situ measurements within this region are severely lacking, although the LTI is located only 80 to 200 km above the surface of our planet. This paper reviews the current state of the art in measuring the LTI, either in situ or by several different remote-sensing methods. We begin by outlining the open questions within the LTI requiring high-quality in situ measurements, before reviewing directly observable parameters and their most important derivatives. The motivation for this review has arisen from the recent retention of the Daedalus mission as one among three competing mission candidates within the European Space Agency (ESA) Earth Explorer 10 Programme. However, this paper intends to cover the LTI parameters such that it can be used as a background scientific reference for any mission targeting in situ observations of the LTI.

show abstract

Relativistic Electron Microburst Events: Modeling the Atmospheric Impact

Cited by 28 publications

References 28 publications

Characteristics of Relativistic Microburst Intensity From SAMPEX Observations

Characteristics of Relativistic Microburst Intensity From SAMPEX Observations

Atmospheric Effects of >30‐keV Energetic Electron Precipitation in the Southern Hemisphere Winter During 2003

Lower-thermosphere–ionosphere (LTI) quantities: current status of measuring techniques and models

Contact Info

Product

Resources

About