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1 edition of Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index found in the catalog.

Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index

Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index

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Published by Storming Media .
Written in English

    Subjects:
  • SCI042000

  • The Physical Object
    FormatSpiral-bound
    ID Numbers
    Open LibraryOL11846395M
    ISBN 101423519205
    ISBN 109781423519201

      The first model to do this was the two‐way coupling of the Polar Wind Outflow Model (PWOM), a classical polar wind model, and BATS‐R‐US [Glocer et al., a, b]. Welling et al. [ ] demonstrated that this model exhibits a positive feedback loop where electron heating from region 2 currents enhances the PWOM outflows, enhances the Cited by:   The main findings are as follows: (1) In local winter, the maximum auroral energy flux over the oval is located in the premidnight sector (– magnetic local time) under geomagnetically quiet condition (Kp = 1) and moves toward the postmidnight sector (– magnetic local time) as the Kp index by: 1.

    Discover Book Depository's huge selection of Keith Anderson books online. Free delivery worldwide on over 20 million titles. Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index. Keith A Anderson. 20 Sep Paperback. US$ US$ Save US$ Add . Akasofu, The topology of the auroral oval as seen by the Isis 2 scanning auroral photometer, Journal of Geophysical Research, 80, 13, (), (). Wiley Online Library Robert H. Eather, Advances in magnetospheric physics: Aurora, Reviews of Geophysics, 13, 3, (), ().

      An aurora is a natural light display in the sky (from the Latin word aurora, “sunrise” or the Roman goddess of dawn), especially in the high latitude (Arctic and Antarctic) regions, caused by the collision of solar wind and magnetospheric charged particles with the high altitude atmosphere (thermosphere).Most auroras occur in a band known as the auroral zone, which is typically 3° to 6. Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index Author: Keith A. Anderson, Air Force Institute of Technology (U.S.) (Creator).


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Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index Download PDF EPUB FB2

DERIVATION OF A SELF-CONSISTENT AURORAL OVAL MODEL USING THE AURORAL BOUNDARY INDEX THESIS Presented to the Faculty Department of Engineering Physics Graduate School of Engineering and Management Air Force Institute of Technology Air University Air Education and Training Command In Partial Fulfillment of the Requirements for the.

Thus, the current work represents a move toward a more self-consistent--and presumably more accurate--climatological representation of the auroral oval boundaries.

This was accomplished by recreating the process performed by Hardy et al., substituting the ABI for the Kp index and deriving an entirely new set of auroral ovals based on almost 11 years of DMSP data from the F8 and F9 : Keith A.

Anderson. Download Citation | Derivation of a Self-Consistent Auroral Oval Model Using the Auroral Boundary Index | The position and intensity of the auroral oval has many implications for the Air Force Author: Keith A. Anderson. the equatorial boundary of the auroral oval on the mid- night side corresponds the inner edge of the plasma sheet, the distance to which decreases slightly with i n.

Statistical and functional representations of the pattern of auroral energy flux, number flux, and conductivity Use of the Auroral Boundary Index for potential forecasting of ionospheric scintillation, Radio Science, 47, 4, ().

Including auroral oval boundaries in the IRI model, Advances in Space Research, 16, 1. Using global riometer network we test the method performance for stations in the middle of auroral zone (at corrected geomagnetic latitudes of 65–67°) where generally the absorption amplitude is largest.

In this paper we use the midlatitude positive bay index, recently developed by X. Chu and R. McPherron, to drive the : V. Sergeev, M. Shukhtina, N. Stepanov, N.

Stepanov, D. Rogov, A. Nikolaev, E. Span. [1] A new self‐consistent version of a time‐dependent magnetospheric paraboloid model is presented and tested on the 24–27 September magnetic storm interval (minimum Dst = − nT).

The model uses DMSP satellite data to identify the location of the inner boundary of the magnetotail current sheet and the magnetic flux in the lobes and their variations with by: () Open Magnetosphere and the Auroral Oval.

In: Physics of Magnetospheric Substorms. Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Reviews), vol Author: Syun-Ichi Akasofu.

aurora that moved poleward to near the poleward boundary of the auroral oval, and seven of these onsets were pseudo-breakups. For all the pseudobreakups, the region of active expansion phase aurora did not move poleward of the field of view of the Gillam ASI.

The dates and UT’s of the 11 onsets are given in Table 1, and each onset is labeled as. Knowledge of the spatial distribution of auroral precipitation and its associated ionospheric effects is important both to scientific studies of the Earth's environment and successful operation of defense and communication systems.

Observations with the best spatial and temporal coverage are obtained through remote sensing from space-based by: 1] The auroral oval can serve as both a representation and a prediction of space weather on a global scale, so a competent model of the oval as a function of a geomagnetic index could conveniently.

AOP (auroral oval precipitation) is the region of structured precipitation, which has equatorward and poleward boundaries statistically coincident with the borders of the auroral oval; SDP (soft diffuse precipitation) is the region of soft diffuse precipitation just poleward of by: auroral oval.

We interpret the double oval morphology as being due to the plasma sheet boundary layer becoming active in the later stages of the substorm process. ff the disturbance engulfs the nightside low-latitude boundary layers, then the double oval configuration extends into the dayside ionospheric region.

The usual rule for calculating a derivative of an explicit function, which is given by equations (5), yields a full system of canonical equations of motion Aco where an important relativistic factor of the velocity- dependence of the electron mass ^=(-Dl|c'l)-l/l ^ = 2^c \-Nl+2^m' Aco Auroral kilometric radiation KI = - (6) where decreases Cited by: 3.

The phenomenon named poleward boundary intensification (PBI) is a brightening of aurora at the poleward edge of the auroral : Robert Mcpherron. The objectives of this paper are the following: (1) to investigate the general trends of the H + and O + ion outflows in the polar wind and auroral zone by using Barghouthi model, (2) to explain.

This is the first study in which a physical ionospheric model (time-dependent ionospheric model (TDIM)) has been driven through a substorm using self-consistent magnetospheric convection electric field and auroral electron precipitation by: The magnetic field increases by 5% from the upper boundary to the lower boundary.

On the field-aligned scale length of the V-shaped auroral potential structure 93 convergence of 10% over Debye lengths). These parameters model the auroral environment under Cited by: 5. • “Derivation of a Self-Consistent Auroral Oval Model using the Auroral Boundary Index” • “Spacecraft Charging at Geosynchronous Altitudes: Critical Temperature Analysis for Non-Maxwellian Distributions” • “Validation and Assessment of DMSP Electron Temperatures in the Topside Ionosphere”.

the Hardy Auroral Oval Boundary model 5. The Hardy model requires only a local time and a Kp value to The Hardy model requires only a local time and a Kp value to generate its output. It is known that the equatorward boundary of the auroral oval has a fairly good correlation with the intensity of the associated magnetic storms.

Yokoyama et al. () studied the time variation of the equatorward boundary of the auroral oval and the intensity (Dst value) of storms between and (their Figure 3).

In a quiet auroral arc a disturbance may occur e.g. due to Kelvin-Helmholz instability associated with a convection shear along the arc. Also, a vortex of plasma flow can arise due to some kind of the Rayleigh-Taylor instability [6].Figure 1 presents a sketch of wave-like distortions in the field-aligned currents and plasma flows connected to an auroral arc.Determination of auroral heat fluxes and thermal ion outflows using a numerical ionospheric model and incoherent-scatter radar data Q.-L.

Min x and B. J. Watkins Geophysical Institute, University of Alaska, Fairbanks Abstract. A comprehensive one-dimensional model of the polar ionosphere has.