Evolution of CIR storm on 22 July 2009

Perez, J. D.; Grimes, E. W.; Goldstein, J.; McComas, D. J.; Valek, P. W.; Billor, Nedret

doi:10.1029/2012ja017572

Cited by 29 publications

(79 citation statements)

References 42 publications

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“…Prior to extracting the ion distribution, the TWINS images are statistically smoothed using a technique described in detail in Appendix A of McComas et al . [] and previously applied successfully to ENA images from IBEX [ McComas et al ., ] and TWINS [ Valek et al ., ; Grimes et al ., ; Perez et al ., ].…”

Section: Data Sourcesmentioning

confidence: 99%

Comparison of TWINS and THEMIS observations of proton pitch angle distributions in the ring current during the 29 May 2010 geomagnetic storm

et al. 2013

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[1] The first comparison between energy-dependent ion pitch angle distributions in the ring current deconvolved from Two Wide-angle Imagining Neutral-atom Spectrometers (TWINS) energetic neutral atom (ENA) images and measured by Time History of Events and Macroscale Interactions during Substorms (THEMIS) D and E during a magnetic storm on 29 May 2010 is shown. The ion intensities and energy spectra along the THEMIS path are also compared with those deconvolved from the TWINS ENA images. The global plots of the ion intensities show an asymmetric ring current in the early recovery phase consistent with the ASY/H index. The comparison between the in situ pitch angle distributions observed by THEMIS and those obtained here from TWINS ENA images lends credence to the global plots of pitch angle anisotropy provided by the TWINS data. The spatial dependence of the pitch angle anisotropy provides information relevant to ion precipitation and lifetimes of trapped ring current ions not available from in situ measurements.

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Section: Data Sourcesmentioning

confidence: 99%

Comparison of TWINS and THEMIS observations of proton pitch angle distributions in the ring current during the 29 May 2010 geomagnetic storm

et al. 2013

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“…They showed that the ring current ion intensities were more asymmetric at the main phase while less asymmetric at the recovery phase, and at the main phase the peak of ion intensities located at~23:00 MLT for <30 keV ions and gradually moved to~21:00 MLT for >50 keV ions. If we simply use the ring current energy density distribution pattern similar to 22.5-67.5 keV ion intensity distribution shown in Perez et al [2012] at the main phase of July 2009 storm, the ring current energy content decreases by~30% compared to the energy content calculated using MLT symmetry assumption. However, it is worth mentioning that for higher energy ions the energy density distribution should be more MLT symmetric, and those higher energy ions still account for a large portion of the ring current energy content, thus the influence of MLT asymmetry to the ring current energy content should be smaller.…”

Section: The Contribution Of Ring Current Heavy Ionsmentioning

confidence: 99%

“…Perez et al [2012], using Two Wide-Angle Imaging Neutral-Atom Spectrometers ENA images, derived the global image of equatorial ion intensities for a moderate storm on July 2009. They showed that the ring current ion intensities were more asymmetric at the main phase while less asymmetric at the recovery phase, and at the main phase the peak of ion intensities located at~23:00 MLT for <30 keV ions and gradually moved to~21:00 MLT for >50 keV ions.…”

Section: The Contribution Of Ring Current Heavy Ionsmentioning

confidence: 99%

The evolution of ring current ion energy density and energy content during geomagnetic storms based on Van Allen Probes measurements

et al. 2015

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Enabled by the comprehensive measurements from the Magnetic Electron Ion Spectrometer (MagEIS), Helium Oxygen Proton Electron mass spectrometer (HOPE), and Radiation Belt Storm Probes Ion Composition Experiment (RBSPICE) instruments onboard Van Allen Probes in the heart of the radiation belt, the relative contributions of ions with different energies and species to the ring current energy density and their dependence on the phases of geomagnetic storms are quantified. The results show that lower energy (<50 keV) protons enhance much more often and also decay much faster than higher‐energy protons. During the storm main phase, ions with energies <50 keV contribute more significantly to the ring current than those with higher energies; while the higher‐energy protons dominate during the recovery phase and quiet times. The enhancements of higher‐energy proton fluxes as well as energy content generally occur later than those of lower energy protons, which could be due to the inward radial diffusion. For the 29 March 2013 storm we investigated in detail that the contribution from O+ is ~25% of the ring current energy content during the main phase and the majority of that comes from <50 keV O+. This indicates that even during moderate geomagnetic storms the ionosphere is still an important contributor to the ring current ions. Using the Dessler‐Parker‐Sckopke relation, the contributions of ring current particles to the magnetic field depression during this geomagnetic storm are also calculated. The results show that the measured ring current ions contribute about half of the Dst depression.

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“…The features of the ion energy spectrum and intensity in the main phase and the early recovery phase during a storm driven by a CIR on 22 July 2009 have been studied with TWINS ENA images and THEMIS in situ measurements (Perez et al 2012). However, to the best of our knowledge, inadequate research has been done in studying the energy transport during the storms using data from simultaneous observations using multiple satellites moving in different regions of the magnetotail.…”

Section: Introductionmentioning

confidence: 98%

Multi-satellite observations of energy transport during an intense geomagnetic storm

Yang

Duan

et al. 2016

Astrophys Space Sci

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Energy transport during a geomagnetic substorm is a very important process for solar wind-magnetosphere energy coupling and the energy cycle in the magnetotail. In this paper, we use magnetotail data from the five THEMIS probes and two Cluster satellites on the dayside to investigate the energy transport of one intense storm during the period from 08 March to 11 March 2008 at large spatial-temporal scales. Simultaneous observations of the five THEMIS probes indicate that there is a stronger and earlier duskward energy flux density in the near-Earth magnetotail than that in the mid-tail in the initial phase. Low energy particles inject earthward from the dusk flank. Stronger and more variable earthward energy flux density is observed in the mid-tail compared to that near Earth in the main phase; mainly caused by high-speed flow. Tailward energy flux was observed in the near-Earth and mid-tail regions during the recovery phase. Dayside data observed by two Cluster satellites show that the duskward energy flux may be related to stable solar wind input. Tailward energy flux on the dayside should experience some energy conversion process in the magnetotail before it can provide the earthward energy flux in the magnetotail for this intense storm. The strongest energy transport observed by the nightside probes occurs in the main phase. However, the strongest energy measured by the dayside satellites is in the recovery phase without intense activities, two hours later. Different features of the energy transport in the three phases of the storm may be closely

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Evolution of CIR storm on 22 July 2009

Cited by 29 publications

References 42 publications

Comparison of TWINS and THEMIS observations of proton pitch angle distributions in the ring current during the 29 May 2010 geomagnetic storm

Comparison of TWINS and THEMIS observations of proton pitch angle distributions in the ring current during the 29 May 2010 geomagnetic storm

The evolution of ring current ion energy density and energy content during geomagnetic storms based on Van Allen Probes measurements

Multi-satellite observations of energy transport during an intense geomagnetic storm

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