Resonant acceleration and diffusion of outer zone electrons in an asymmetric geomagnetic field

By S. Elkington, M. Hudson, A. Chan. 2003

403 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f970a65d1c8e261c0f4e8b92fb3bed1eeeab10d3

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In Astronomy and Astrophysics

Citations in the corpus

Van Allen Probes observation of localized drift resonance between poloidal mode ultra‐low frequency waves and 60 keV electrons (2013, background): “We emphasize however, that when such drift-resonant interactions are aggregated over a long time interval and over many drift orbits, and occur at multiple isolated locations along the drift orbit, the net effect could produce radial diffusion [e.g., Elkington et al., 2003].”
The Electric and Magnetic Field Instrument Suite and Integrated Science (EMFISIS) on RBSP (2013, background): “Theoretical calculations suggest that ULF acceleration mechanisms should be substantially reduced in efficiency at lower L, compared to geosynchronous orbit (Fälthammar and Walt 1969; Elkington et al. 2003).”
Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era (2019, methodology): “Elkington et al. (2003) followed guiding center test particles in the equatorial plane of a compressed dipole analytic model with poloidal mode ultralow frequency (ULF) wave fields (Hughes, 2013) of order 1 mHz, comparable to the drift period of MeV electrons at geosynchronous orbit.”
Space Weather Effects in the Earth’s Radiation Belts (2018, methodology): “Extensions to the pure azimuthal drift based radial diffusion framework have been pursued more recently by Elkington et al. (1999, 2003) through inclusion of drift-resonant electron interactions with ULF toroidal and/or poloidal wave modes in a manner that inherently accommodates an asymmetric…”
Time dependent radial diffusion modeling of relativistic electrons with realistic loss rates (2004, background): “Leading mechanisms for acceleration to relativistic energies include radial diffusion driven by ULF waves [e.g., Elkington et al., 2003 ] and local stochastic acceleration by VLF waves [Horne and Thorne, 1998; Summers et al., 1998, 2002].”
Radiation Belt Environment model: Application to space weather nowcasting (2008, background): “Elkington et al. [2003] investigated the effects of”
A review of interplanetary discontinuities and their geomagnetic effects (2011, background): “7) demonstrate that the directionality of the interplanetary magnetic field (IMF) is not a factor for this mechanism (Hudson et al., 1997, 2004; Elkington et al., 2003, 2004).”
The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere (2017, methodology): “This process can adiabatically accelerate inner-magnetosphere charged particles and significantly enhance their radial diffusion (e.g., Elkington et al. 2003; Loto’aniu et al. 2006).”
Acceleration mechanism responsible for the formation of the new radiation belt during the 2003 Halloween solar storm (2006, background): “Leading mechanisms for acceleration to relativistic energies include radial diffusion driven by ULF waves [e.g., Elkington et al., 2003], local stochastic acceleration driven by VLF waves [Horne and Thorne, 1998; Summers et al., 1998; Horne et al., 2005a], and rapid shock induced acceleration [Li…”
On the storm‐time evolution of relativistic electron phase space density in Earth's outer radiation belt (2013, background): “…a source at the outer boundary, inward transport and energization is enabled by ULF waves in the Pc5 frequency range, which break the third adiabatic invariant and provide the random displacements in L* necessary for diffusion [e.g., Hudson et al., 2000; Elkington et al., 2003; Mann et al., 2004].”
Quantification of relativistic electron microburst losses during the GEM storms (2004, background): “Specifically, Reeves et al. argued that the net outer radiation belt response to a magnetic storm was a ‘‘delicate and complicated balance between the effects of particle acceleration and loss.’’ [3] The two most promising acceleration processes are enhanced radial diffusion caused by drift resonanc”
Relativistic electrons in the outer radiation belt: Differentiating between acceleration mechanisms (2004, background): “The diffusion rate is set by the coefficient D which is a function of L* as well as the amplitude of magnetic and electric field perturbations and can take various forms [e.g., Elkington et al., 2003 ].”
Timescale for MeV electron microburst loss during geomagnetic storms (2005, background): “[21] Enhanced radial diffusion [e.g., Elkington et al., 2003 ] and local stochastic acceleration during resonant interactions with chorus [e.g., Horne et al., 2005] are leading candidates to explain the observed relativistic electron flux enhancements during the storm recovery phase.”
Parameterization of radiation belt electron loss timescales due to interactions with chorus waves (2007, methodology): “…processes may also be used in radial diffusion codes [e.g., Shprits and Thorne, 2004; Barker et al., 2005], and particle tracing codes [e.g., Elkington et al., 2003; Ukhorskiy et al., 2005], which require additional specification of processes that violate the first and second adiabatic…”
Event‐specific chorus wave and electron seed population models in DREAM3D using the Van Allen Probes (2014, background): “The acceleration of radiation belt electrons can be due to inward radial diffusion [Hudson et al., 2000; Elkington et al., 2003] and/or local heating by Very Low Frequency (VLF) waves, such as whistler mode chorus [Horne and Thorne, 1998; Horne et al.”
Excitation of poloidal standing Alfvén waves through drift resonance wave‐particle interaction (2013, background): “The resonance associated with the drift motion is considered important for dynamics of the ring current [Southwood, 1976; Sibeck et al., 2012] and radiation belt particles [Schulz and Lanzerotti, 1974; Elkington et al., 2003].”