42 research outputs found
Locations of boundaries of outer and inner radiation belts as observed by Cluster and Double Star
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95464/1/jgra21211.pd
Inner magnetosphere currents during the CIR/HSS storm on July 21â23, 2009
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94920/1/jgra21817.pd
Lowâenergy electrons (5â50 keV) in the inner magnetosphere
Transport and acceleration of the 5â50 keV electrons from the plasma sheet to geostationary orbit were investigated. These electrons constitute the lowâenergy part of the seed population for the highâenergy MeV particles in the radiation belts and are responsible for surface charging. We modeled one nonstorm event on 24â30 November 2011, when the presence of isolated substorms was seen in the AE index. We used the Inner Magnetosphere Particle Transport and Acceleration Model (IMPTAM) with the boundary at 10 R E with moment values for the electrons in the plasma sheet. The output of the IMPTAM modeling was compared to the observed electron fluxes in 10 energy channels (from 5 to 50 keV) measured on board the AMC 12 geostationary spacecraft by the Compact Environmental Anomaly Sensor II with electrostatic analyzer instrument. The behavior of the fluxes depends on the electron energy. The IMPTAM model, driven by the observed parameters such as Interplanetary Magnetic Field (IMF) B y and B z , solar wind velocity, number density, dynamic pressure, and the Dst index, was not able to reproduce the observed peaks in the electron fluxes when no significant variations are present in those parameters. We launched several substormâassociated electromagnetic pulses at the substorm onsets during the modeled period. The observed increases in the fluxes can be captured by IMPTAM when substormâassociated electromagnetic fields are taken into account. Modifications of the pulse front velocity and arrival time are needed to exactly match the observed enhancements. Key Points Electron flux peaks due to substorm activity Solar wind driven inner magnetosphere model does not work for quiet times Substormâassociated fields to explain electron flux peaksPeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/106068/1/jgra50735.pd
Evolution of the proton ring current energy distribution during 21â25 April 2001 storm
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/95267/1/jgra18324.pd
Event-specific chorus wave and electron seed population models in DREAM3D using the Van Allen Probes
Abstract The DREAM3D diffusion model is applied to Van Allen Probes observations of the fast dropout and strong enhancement of MeV electrons during the October 2012 double-dip storm. We show that in order to explain the very different behavior in the two dips, diffusion in all three dimensions (energy, pitch angle, and Lo) coupled with data-driven, event-specific inputs, and boundary conditions is required. Specifically, we find that outward radial diffusion to the solar wind-driven magnetopause, an event-specific chorus wave model, and a dynamic lower-energy seed population are critical for modeling the dynamics. In contrast, models that include only a subset of processes, use statistical wave amplitudes, or rely on inward radial diffusion of a seed population, perform poorly. The results illustrate the utility of the high resolution, comprehensive set of Van Allen Probes\u27 measurements in studying the balance between source and loss in the radiation belt, a principal goal of the mission. Key Points DREAM3D uses event-specific driving conditions measured by Van Allen Probes Electron dropout is due to outward radial diffusion to compressed magnetopause Event-specific chorus and seed electrons are necessary for the enhancement
FORESAIL-1 cubesat mission to measure radiation belt losses and demonstrate de-orbiting
Abstract Today, the near-Earth space is facing a paradigm change as the number of new spacecraft is literally sky-rocketing. Increasing numbers of small satellites threaten the sustainable use of space, as without removal, space debris will eventually make certain critical orbits unusable. A central factor affecting small spacecraft health and leading to debris is the radiation environment, which is unpredictable due to an incomplete understanding of the near-Earth radiation environment itself and its variability driven by the solar wind and outer magnetosphere. This paper presents the FORESAIL-1 nanosatellite mission, having two scientific and one technological objectives. The first scientific objective is to measure the energy and flux of energetic particle loss to the atmosphere with a representative energy and pitch angle resolution over a wide range of magnetic local times. To pave the way to novel model - in situ data comparisons, we also show preliminary results on precipitating electron fluxes obtained with the new global hybrid-Vlasov simulation Vlasiator. The second scientific objective of the FORESAIL-1 mission is to measure energetic neutral atoms (ENAs) of solar origin. The solar ENA flux has the potential to contribute importantly to the knowledge of solar eruption energy budget estimations. The technological objective is to demonstrate a satellite de-orbiting technology, and for the first time, make an orbit manoeuvre with a propellantless nanosatellite. FORESAIL-1 will demonstrate the potential for nanosatellites to make important scientific contributions as well as promote the sustainable utilisation of space by using a cost-efficient de-orbiting technology.Peer reviewe
Overview of Solar WindâMagnetosphereâIonosphereâAtmosphere Coupling and the Generation of Magnetospheric Currents
Energyâlatitude dispersion patterns near the isotropy boundaries of energetic protons
Non-adiabatic motion of plasma sheet protons causes
pitch-angle scattering and isotropic precipitation to the
ionosphere, which forms the proton auroral oval. This mechanism
related to current sheet scattering (CSS) provides a specific
energyâlatitude dispersion pattern near the equatorward boundary
of proton isotropic precipitation (isotropy boundary, IB), with
precipitation sharply decreasing at higher (lower) latitude for
protons with lower (higher) energy. However, this boundary maps to
the inner magnetosphere, where wave-induced scattering may
provide different dispersion patterns as recently demonstrated by
Liang et al. (2014). Motivated by the potential usage of the IBs
for the magnetotail monitoring as well as by the need to better
understand the mechanisms forming the proton IB, we investigate
statistically the details of particle flux patterns near the
proton IB using NOAA-POES polar spacecraft observations made
during September 2009. By comparing precipitated-to-trapped flux
ratio (<i>J</i><sub>0</sub>/<i>J</i><sub>90</sub>) at >30 and >80 keV proton energies, we
found a relatively small number of simple CSS-type dispersion events
(only 31 %). The clear reversed (wave-induced) dispersion patterns
were very rare (5 %). The most frequent pattern had nearly
coinciding IBs at two energies (63 %). The structured precipitation with multiple IBs was very frequent (60 %), that is, with two
or more significant <i>J</i><sub>0</sub>/<i>J</i><sub>90</sub> dropouts. The average latitudinal
width of multiple IB structures was about 1°. Investigation
of dozens of paired auroral zone crossings of POES satellites showed
that the IB pattern is stable on a timescale of less than 2 min (a few
proton bounce periods) but can evolve on a longer (several
minutes) scale, suggesting temporal changes in some mesoscale
structures in the equatorial magnetosphere.
<br><br>
We discuss the possible role of CSS-related and wave-induced
mechanisms and their possible coupling to interpret the emerging
complicated patterns of proton isotropy boundaries
Conditions of Loss Cone Filling by Scattering on the Curved Field Lines for 30Â keV Protons During Geomagnetic Storm as Inferred From Numerical Trajectory Tracing
The rate of pitch angle scattering on the curved magnetic field lines is well parameterized by the ratio of the minimum field line curvature radius to the maximum effective particle gyroradius (K = RC/rg). The critical value of this ratio (Kcr) corresponding to the loss cone filling is of special interest since it corresponds to the low altitude isotropic boundaries (IBs). The early theoretical estimates gave Kcr = 8, whereas recent estimations of the K parameter on the field lines corresponding to the observed IBs during the geomagnetic storms revealed KIB values in the range of 3â30. We numerically trace the trajectories of the 30 keV protons in the magnetic field of the global magnetohydrodynamic simulation of the intense storm in order to infer statistical distribution of Kcr. The electric field and effects of nonstationarity are neglected in this study. It is found that although the Kcr values do show some variations during the course of the storm, its range is rather narrow 4 < Kcr < 8. The result suggests that higher KIB values found in the observational studies, if not caused by the magnetosphereâionosphere mapping error, should be attributed to some other mechanism of pitch angle scattering. The Kcr values tend to be lower (4â6) during the main phase because the region of low K values approaches the Earth and the equatorial loss cone size becomes larger due to a larger equatorial magnetic field in the nearâearth region. The remaining variation of Kcr is explained by the presence of the guide component of the magnetic field.Key Points30 keV proton trajectories are traced to model the loss cone filling by scattering on the curved field lines during geomagnetic stormCritical value of adiabaticity parameter (Kcr) corresponding to the loss cone filling varies in the range of 4â8This Kcr variation is due to variations of the equatorial loss cone size and the guide component of magnetic field in the current sheetPeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/163828/1/jgra56124_am.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/163828/2/2020JA028490-sup-0001-Text_SI-S01.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/163828/3/jgra56124.pd