INNER MAGNETOSPHERE PLASMA DENSITIES. Bodo W. Reinisch and Xueqin Huang
|
|
- Nelson Lawrence
- 5 years ago
- Views:
Transcription
1 XA INNER MAGNETOSPHERE PLASMA DENSITIES Bodo W. Reinisch and Xueqin Huang Environmental, Earth, and Atmospheric Sciences Department, Centerfor Atmospheric Research, University of Massachusetts Lowell, MA 01854, USA Abstract: The radio plasma imager (RPI) on the IMAGE satellite performs radio sounding in the magnetosphere, transmitting coded signals stepping through the frequency range of interest and receiving the returned echoes. The measurements provide the echo amplitude as a function of frequency and echo delay time on a so-called plasmagram. A newly developed algorithm inverts THE echo traces on a plasmagram to electron density spatial distributions. Based on these observed density distributions, an empirical model is constructed to describe the twodimensional density distribution in the inner magnetosphere. INTRODUCTION The radio plasma imager (RPI) on the Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) satellite (Burch et al., 2001) performs sounding in the frequency range from 3 khz to 3 MHz using three orthogonal antennas, two 500-m long dipoles in the spin plane, and a 20-m dipole along the spin axis. IMAGE is on an elliptical polar orbit with an altitude of 7.2 R E at apogee, and 1,200 km at perigee. When the RPI is sounding inside or close to the plasmapause there are often discrete echo traces with virtual ranges of up to 7 RE The virtual range is the time delay of an echo multiplied by half of the speed of light. Reinisch et al. (2001) have shown that the waves producing these discrete traces have propagated along the magnetic field lines. A newly developed profile inversion algorithm calculates the electron density distribution along the direct path from the spacecraft along the magnetic field line that intersects the spacecraft. The RPI sounding observations of the field aligned propagation echoes make it possible to measure the density profile in a large range of distance along the field line. A single measurement is typically completed within two minutes. This paper first gives a brief description of the inversion technique, then shows examples of the density profiles, and finally presents an empirical model of electron density distribution in the plasmasphere during one pass. PLASMAGRAMS AND INVERSION TECHNIQUE Coded radio signals are transmitted from the RPI into all directions, and they are reflected at places where the wave frequency equals a plasma cut-off frequency. The echo delay
2 106 times are transformed into the so-called virtual ranges by multiplying them with half the speed of light, and the echo amplitudes are displayed in plasmagrams as function of virtual range in units of Earth radii R E and frequency hi khz. Measurements are typically made about every 2 minutes during which tune the satellite travels about 500 km along its trajectory. Figure 1 shows an example of RPI plasmagrams when IMAGE was inside the plasmasphere. 05»f.« Frequency (khz) 2001 June 08,20:40:56 UT Magnetic Latitude Ο Fig. 1. (a) Plasmagram recorded inside the plasmasphere displaying the echo amplitude as function of frequency and virtual range. The thin red lines on top of the two strongest traces are echo traces predicted according to the density profile shown in (b). The insert shows the orbit (red line) and location (red square) of IMAGE at the time of the sounding. The field lines of L=4 are shown in black lines, (b) The density profile, as function of magnetic latitude, inverted from the plasmagram shown in (a). The two strongest traces have been identified as X mode echoes (Reinisch et al., 2001). The virtual range, P, for a point on a trace must satisfy the integral where c is the speed of light in free space, and V g (f) is the group velocity of the wave with frequency/, traveling from the spacecraft along the path F f to the reflection point, assuming the
3 107 wave travels back to the spacecraft on the same path at the same speed as to the reflection point. With the cold plasma and geometric optics approximations we can write P(/)= jvcosacfc (2) r/ where n'=3(n/)/9/is the so-called group refractive index with η the refractive index for the extraordinary mode, and ctis the angle between the group velocity and the wave normal. In an earlier paper, Muldrew (1963) suggested that the echoes are traveling along the magnetic field line intersecting the spacecraft. The multiple echo traces on the plasmagram in Figure la are the result of waves propagating to the local and conjugate hemispheres. The echoes from the local (northern) hemisphere produce the trace with smaller virtual ranges, while the longer virtual ranges result from reflections in the conjugate hemisphere. The trace at ~8 R E (not used for the inversion) propagates first to one hemisphere, then to the conjugate one, and then back to the spacecraft. For propagation along the field line, the deviation angle a becomes zero, and the wave normal is parallel to the group velocity, simplifying (2) to P(f}=\n\fJ P,f B )ds (3) r/ The group refractive index n' is a function of the wave frequency/, the electron plasma frequency/p, and the electron gyro-frequency^. A new algorithm, based on the method used to invert the topside ionograms (Huang and Reinisch, 1982), was developed to solve the integral equation (3) numerically for the true reflection distance. The integration is carried out along the field line using a global magnetic field model (Tsyganenko and Stern, 1996). The X mode traces in Figure la extend from/= 350 khz to higher frequencies with virtual ranges increasing from 0 to ~2.5 RE for the local trace, and 4-6 RE for the conjugate trace. The local trace determines the electron density distribution along the field line (L=3.0) from the satellite position (MLAT=12.9o) to higher latitudes. The conjugate trace with echoes reflected in the southern hemisphere does not start at 0 range. The waves must propagate across the equator region where the densities are lower than at the satellite location. The first conjugate echo at the lowest frequency is reflected at the point approximately conjugate to the spacecraft location. For f close to and slightly above 350 khz, the group velocities are very small in the whole region near the equator, producing very large virtual ranges of ~6 RE. Higher frequencies, on the other hand, have higher group velocities across the equator, and low group velocities occur only for a relatively short distance near the reflection point at higher latitudes. Combining these two effects, the virtual ranges are shorter for higher frequencies although the echoes actually travel longer distances. No echoes return from the equatorial region of the path from the spacecraft to its conjugate point. However, the total electron content in this region is known from the time delay of the first conjugate echo. The equatorial densities are interpolated assuming that the density gradients are continuous in this region. When the satellite flies through the equator, sometimes echo traces can be received near the equator. The quality of the interpolation of the equatorial densities can be assessed by comparing the profiles
4 108 from the interpolated densities with the directly measured ones. As will be seen later in this paper, the uncertainty due to the interpolation is much smaller than the inherent variations of the plasma structures. After subtraction of the virtual range to the satellite's conjugate point from the left side of (3), the inversion procedure is applied to the adjusted conjugate trace. The inversion results for the plasmagram in Figure la are shown in Figure Ib. Using the derived density profile, the time delays for each frequency can be calculated. The thin red lines marked on each of the two strongest traces show the calculated traces using the electron density profile in Figure Ib. EMPIRICAL MODEL Since the launch of IMAGE in March 2000, RPI has continuously recorded plasmagrams in the plasmasphere. The inversion technique described above has been applied to process plasmagrams with echo traces of good quality. The profile inverted from a single plasmagram gives the density distribution along the field line, and it can be regarded as an instantaneous measurement over a large region. Combining the profiles obtained from different L-values, it is possible to construct an empirical model showing the global density distribution in the plasmasphere. In this paper, we demonstrate, as the first step, the possibility to derive a 2-D plasma density model. On June 8, 2001, IMAGE passed through L = 2.22 to L = 3.23 in the morning sector as shown in Figure 2. During this pass within 22 minutes, 7 plasmagrams were obtained with good discrete traces, a rare opportunity. I 1 I I I I Fig. 2. Trajectory of IMAGE on June 8, The meridian cut is near 0800 MLT. The red dots on the trajectory indicate where plasmagrams were made. The black lines show the field lines from the empirical field model.
5 June 08, MLT = 8.0 έ* η w fi Magnetic Latitude Π Fig 3. Density profiles on June 8,2001. The solid black lines are inverted from measurements, and the red dashed lines are the empirical model. The 7 inverted density profiles are shown in Figure 3. The densities vary as functions of latitude λ and L-value. After experimenting with many different possible functional forms, noting that a single functional form has to describe the intrinsic properties of all 7 profiles, we choose the following form: D-L ''INV β(ι-) η αλ where Xjn V is the invariant latitude of the L shell. Parameter No(L) is the equatorial density. Parameter γ describes the asymmetry of the north-south distribution around the equator, γ < 0 meaning that the density in the southern hemisphere is higher than at the conjugate points in the northern hemisphere, and visa versa. Careful inspection of Figure 3 shows the asymmetry. The power index β(ί,) defines the steepness of the profile at high latitudes. Parameter α specifies the flatness of the profile at low latitudes. Parameter Β roughly gives the location of the plasmapause. From a multi-variant best fit, we obtain A=4833 cm" 3, 5=3.64, C=0.2, D=0.03, γ=-0.14, and a=1.25 for the morning sector on June 8 The two-dimensional distribution of density in magnetic local time 0800 on June 8, 2001 can then be determined as shown in Figure 4. A similar model was used to describe the refilling process after the March 31, 2001 storm (Reinisch et al., 2003). For the equinox period, the asymmetry factor γ was found to be zero. To illustrate the seasonal asymmetry, Figure 5 shows the vertical plasmaspheric total electron content (TEC) at equinox (left) and solstice 'INV _ (4)
6 110 (right). In June, the plasmaspheric TEC in the southern hemisphere is -10% higher than in the northern hemisphere *? Εu CO ο D Ο «t * u <ΰ Hi Geocentric Distance (RE) Fig. 4. Empirical model for the June 8, 2001 event. 30 Before the storm on 2001 March 31, MLT= MAGNETIC LATITUDE Π MAGNETIC LATITUDE ( ) Fig. 5. Vertical plasmaspheric electron content above 1 RE altitude at equinox (left) and solstice (right). At 30 latitude, the relative TEC difference ATEC is -10%.
7 Nsumei et al. (2003) have analyzed RPI plasmagrams in the northern polar cap and have derived an empirical polar cap density model for high sunspot activity: Ill N e (R,Kp)[cm- 3 ] = 3433(R/R E )~ 5 09 e ' 229Kp. (5) The density decreases with height as a power law with exponent of approximately -5. The analysis of one year of data in showed a strong dependence of the density on the magnetic activity. The exponential Kp dependence indicates that magnetospheric energetic precipitated particles and electromagnetic energy deposited during disturbed geomagnetic conditions are important sources for additional ionization. SUMMARY The basic techniques have been described for the development of an empirical model of the inner magnetospheric electron density distribution based on IMAGE/RPI measurements. The electron density distribution is determined from ~0.5 R E to ~5 R E. ACKNOWLEDGMENTS This work was supported by NASA under subcontract from Southwest Research Institute. REFERENCES Burch, J. L., S. B. Mende., D. G. Mitchell, T. E., Moore., C. J. Pollock, B. W. Reinisch, B. R. Sandel, S. A. Fuselier, D. L. Gallagher, J. L. Green, J. D. Perez, and P. H. Reiff, Views of the Earth's magnetosphere with the IMAGE satellite, Science, 291, 5504,2001. Huang, X. and B.W. Reinisch, Automatic Calculation of Electron Density Profiles from Digital lonograms. 2. True Height Inversion of Topside lonograms with the Profile-fitting Method. Radio ScL, 17,4, Muldrew, D.B., Radio Propagation along Magnetic Field-aligned Sheets of lonization Observed by the Alouette Topside Sounder, J. Geophys. Res., 68,19, Nsumei, P., X. Huang, B.W. Reinisch, P. Song, V.M. Vsyliunas, J.L. Green, S.F, Fung, R.F. Benson, and D.L. Gallagher, Electron density distribution over the northern polar region deducted from IMAGE/radio plasma imager sounding, J. Geophys. Res., 108(A2), 1078, doi: /2002ja009616,2003 Reinisch, B.W., X. Huang, P. Song, G.S. Sales, S.F. Fung, J.L. Green, D.L. Gallagher, and V.M. Vasyliunas, Plasma Density Distribution Along the Magnetospheric Field: RPI Observations From IMAGE. Geophys. Res. Lttrs., 28, 24, Reinisch, B.W., X. Huang, P. Song, S. F. Fung, J. L. Green, V. M. Vasyliunas, D. Gallagher, and B. R. Sandel, Plasmaspheric Mass Loss and Refilling as a Result of a Magnetic Storm, J. Geophys. Res., submitted, Tsyganenko, N.A. and D.P. Stern, Modeling the global magnetic field and the large-scale Birkeland current systems, J. Geophys. Res., 101, ,1996.
IMAGE and DMSP observations of a density trough inside the plasmasphere
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja015104, 2010 IMAGE and DMSP observations of a density trough inside the plasmasphere H. S. Fu, 1,2,3 J. Tu, 1 J.
More informationElectron density images of the middle- and high-latitude magnetosphere in response to the solar wind
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 110,, doi:10.1029/2005ja011328, 2005 Electron density images of the middle- and high-latitude magnetosphere in response to the solar wind Jiannan Tu, 1 Paul Song,
More informationDistribution of density along magnetospheric field lines
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111,, doi:10.1029/2005ja011414, 2006 Distribution of density along magnetospheric field lines R. E. Denton, 1 K. Takahashi, 2 I. A. Galkin, 3 P. A. Nsumei, 3 X. Huang,
More informationTHE FIRST TWO YEARS OF IMAGE
THE FIRST TWO YEARS OF IMAGE J. L. BURCH Southwest Research Institute San Antonio, TX 78228-0510, U.S.A. Abstract. The Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) is the first satellite
More informationRotation of the Earth s plasmasphere at different radial distances
Available online at www.sciencedirect.com Advances in Space Research 48 (2011) 1167 1171 www.elsevier.com/locate/asr Rotation of the Earth s plasmasphere at different radial distances Y. Huang a,b,, R.L.
More informationWhat Processes Influence Plasmaspheric Refilling?
What Processes Influence Plasmaspheric Refilling? (Really, I d like to know) D.L. Gallagher, NASA/MSFC Unsolved Problems in Magnetospheric Physics, Scarborough, UK September 6-12, 2015 l Not so much new
More informationMagnetospheric electron density model inferred from Polar plasma wave data
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A11, 1386, doi:10.1029/2001ja009136, 2002 Magnetospheric electron density model inferred from Polar plasma wave data R. E. Denton, 1 J. Goldstein, 2 J. D.
More informationIn-Situ vs. Remote Sensing
In-Situ vs. Remote Sensing J. L. Burch Southwest Research Institute San Antonio, TX USA Forum on the Future of Magnetospheric Research International Space Science Institute Bern, Switzerland March 24-25,
More informationELECTROSTATIC AND ELECTROMAGNETIC EMISSIONS NEAR THE PLASMASPHERE. A CASE EVENT: 27 MAY 2003
ELECTROSTATIC AND ELECTROMAGNETIC EMISSIONS NEAR THE PLASMASPHERE. A CASE EVENT: 7 MAY 3 1 F. El-Lemdani Mazouz (1), S. Grimald (1), J.L. Rauch (1), P.M.E. Décréau (1), G. Bozan (1), G. Le Rouzic (1),
More informationSub-Auroral Electric Fields: An Inner Magnetosphere Perspective
Sub-Auroral Electric Fields: An Inner Magnetosphere Perspective Bob Spiro Rice University 2005 GEM/CEDAR Tutorial 1 Introduction/Outline Introduction/Outline Importance of Sub-Auroral E-Fields Early Models
More informationElectromagnetic Fields Inside the Magnetoshpere. Outline
Electromagnetic Fields Inside the Magnetoshpere P. K. Toivanen Finnish Meteorological Institute, Space Research Outline Introduction to large-scale electromagnetic fields Magnetic field geometry Modelling
More information2 Preliminary Results Achieved by the Meridian Project
Space Science Activities in China cycle peak year ( ), magnetic storm activities increased significantly, the Meridian Project has repeatedly observed the responses of the space environment to solar storms
More informationThe occurrence of ionospheric signatures of plasmaspheric plumes over different longitudinal sectors
Digital Commons@ Loyola Marymount University and Loyola Law School Physics Faculty Works Seaver College of Science and Engineering 8-1-2008 The occurrence of ionospheric signatures of plasmaspheric plumes
More informationDavid versus Goliath 1
David versus Goliath 1 or A Comparison of the Magnetospheres between Jupiter and Earth 1 David and Goliath is a story from the Bible that is about a normal man (David) who meets a giant (Goliath) Tomas
More informationGEOPHYSICAL RESEARCH LETTERS, VOL. 37, L20107, doi: /2010gl045199, 2010
GEOPHYSICAL RESEARCH LETTERS, VOL. 37,, doi:10.1029/2010gl045199, 2010 A comparison of ionospheric O + /light ion transition height derived from ion composition measurements and the topside ion density
More informationThe CARISMA Array of Fluxgate and Induction Coil Magnetometers
The CARISMA Array of Fluxgate and Induction Coil Magnetometers David Milling CARISMA Project Manager dmilling@ualberta.ca Ian Mann CARISMA PI Canada Research Chair in Space Physics ian.mann@ualberta.ca
More informationparticipation in magnetopause reconnection: first results
Structure of plasmaspheric plumes and their participation in magnetopause reconnection: first results from THEMIS 0 J. P. McFadden, C. W. Carlson, D. Larson, J. Bonnell, F. S. Mozer, V. Angelopoulos,,
More informationIMF B Y and the seasonal dependences of the electric field in the inner magnetosphere
Annales Geophysicae, 23, 2671 2678, 2 SRef-ID: 143276/ag/2-23-2671 European Geosciences Union 2 Annales Geophysicae IMF B Y and the seasonal dependences of the electric field in the inner magnetosphere
More informationUsage of IGS TEC Maps to explain RF Link Degradations by Spread-F, observed on Cluster and other ESA Spacecraft
Usage of IGS TEC Maps to explain RF Link Degradations by Spread-F, observed on Cluster and other ESA Spacecraft J. Feltens, J. Dow, G. Billig, D. Fornarelli, S. Pallaschke, B. Smeds, H.-J. Volpp, P. Escoubet,
More informationTools of Astronomy Tools of Astronomy
Tools of Astronomy Tools of Astronomy The light that comes to Earth from distant objects is the best tool that astronomers can use to learn about the universe. In most cases, there is no other way to study
More informationOn the relationship of SAPS to storm-enhanced density
Journal of Atmospheric and Solar-Terrestrial Physics 69 (07) 3 313 www.elsevier.com/locate/jastp On the relationship of SAPS to storm-enhanced density J.C. Foster a,, W. Rideout a, B. Sandel b, W.T. Forrester
More informationChapter 8 Geospace 1
Chapter 8 Geospace 1 Previously Sources of the Earth's magnetic field. 2 Content Basic concepts The Sun and solar wind Near-Earth space About other planets 3 Basic concepts 4 Plasma The molecules of an
More informationcos 6 λ m sin 2 λ m Mirror Point latitude Equatorial Pitch Angle Figure 5.1: Mirror point latitude as function of equatorial pitch angle.
Chapter 5 The Inner Magnetosphere 5.1 Trapped Particles The motion of trapped particles in the inner magnetosphere is a combination of gyro motion, bounce motion, and gradient and curvature drifts. In
More informationVania K. Jordanova Los Alamos National Laboratory, Los Alamos, NM 87545, USA
Vania K. Jordanova Los Alamos National Laboratory, Los Alamos, NM 87545, USA What is the contribution from different ion species to inner magnetosphere dynamics:» Simulations of ring current H +, He +,
More informationLocations of chorus emissions observed by the Polar Plasma Wave Instrument
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja014579, 2010 Locations of chorus emissions observed by the Polar Plasma Wave Instrument K. Sigsbee, 1 J. D. Menietti,
More informationInterplanetary magnetic field control of afternoon-sector detached proton auroral arcs
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A9, 1251, doi:10.1029/2001ja007554, 2002 Interplanetary magnetic field control of afternoon-sector detached proton auroral arcs J. L. Burch, 1 W. S. Lewis,
More informationThe Magnetic Sun. CESAR s Booklet
The Magnetic Sun CESAR s Booklet 1 Introduction to planetary magnetospheres and the interplanetary medium Most of the planets in our Solar system are enclosed by huge magnetic structures, named magnetospheres
More informationCluster and DEMETER Satellite Data. Fabien Darrouzet (Belgian Institute for Space Aeronomy (IASB-BIRA))
Cluster and DEMETER Satellite Data Fabien Darrouzet (Belgian Institute for Space Aeronomy (IASB-BIRA)) 1 Outline Magnetosphere Plasmasphere Cluster Mission WHISPER Instrument and Data DEMETER Mission ISL
More informationMagnetosphere-Ionosphere Coupling as Revealed in Ground and Space-Based Observations of Total Electron Content
Magnetosphere-Ionosphere Coupling as Revealed in Ground and Space-Based Observations of Total Electron Content A. J. Mannucci Jet Propulsion Laboratory, California Institute of Technology Collaborator:
More informationA Survey of Spacecraft Charging Events on the DMSP Spacecraft in LEO
A Survey of Spacecraft Charging Events on the DMSP Spacecraft in LEO Phillip C. Anderson Space Science Applications Laboratory The Aerospace Corporation PO Box 92957 M2/260 Los Angeles, CA 90009-2957 ph:
More informationExploring the ionosphere of Mars
Exploring the ionosphere of Mars This hazy region contains the atmosphere and ionosphere of Mars Paul Withers Boston University (withers@bu.edu) Department of Physics and Astronomy, University of Iowa,
More informationSimultaneous Observations of E-Region Coherent Backscatter and Electric Field Amplitude at F-Region Heights with the Millstone Hill UHF Radar
Simultaneous Observations of E-Region Coherent Backscatter and Electric Field Amplitude at F-Region Heights with the Millstone Hill UHF Radar J. C. Foster and P. J. Erickson MIT Haystack Observatory Abstract
More informationGlobal Monitoring of the Terrestrial Ring Current
Global Monitoring of the Terrestrial Ring Current Stefano Orsini Istituto di Fisica dello Spazio Interplanetario, CNR ROMA, Italy with the fruitful help of Anna Milillo and of all other colleagues of the
More informationCOMPARISON OF THERMAL PLASMA OBSERVATIONS ON SCATHA AND GEOS
57 COMPARISON OF THERMAL PLASMA OBSERVATIONS ON SCATHA AND GEOS R. C. Olsen The University of Alabama,Huntsville, AL., USA P. M. E. Decreau LPCE, Orleans, France J. F. E. Johnson Department of Physics,
More informationStormtime Dynamics of the Magnetosphere near Geosynchronous Altitudes
Stormtime Dynamics of the Magnetosphere near Geosynchronous Altitudes William J. Burke 1, Meg A. Noah 2 and Jun Yang 2 4 November 214 1. Boston College/ISR 2. University of Massachusetts, Lowell Stormtime
More informationThe influence of hemispheric asymmetries on field-aligned ion drifts at the geomagnetic equator
GEOPHYSICAL RESEARCH LETTERS, VOL. 39,, doi:10.1029/2012gl053637, 2012 The influence of hemispheric asymmetries on field-aligned ion drifts at the geomagnetic equator A. G. Burrell 1,2 and R. A. Heelis
More information1.2 Coordinate Systems
1.2 Coordinate Systems 1.2.1 Introduction One of the critical factors in the development of the AE9/AP9/SPM model was the selection of coordinate systems for mapping particle flux measurements and the
More informationOrbit and Transmit Characteristics of the CloudSat Cloud Profiling Radar (CPR) JPL Document No. D-29695
Orbit and Transmit Characteristics of the CloudSat Cloud Profiling Radar (CPR) JPL Document No. D-29695 Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 26 July 2004 Revised
More informationEarth s Magnetosphere
Earth s Magnetosphere General Description of the Magnetosphere Shape Pressure Balance The Earth s Magnetic Field The Geodynamo, Magnetic Reversals, Discovery Current Systems Chapman Ferraro Cross Tail
More informationMagnetospherically-Generated Ionospheric Electric Fields
Magnetospherically-Generated Ionospheric Electric Fields Stanislav Sazykin Rice University sazykin@rice.edu June 26, 2005 Sazykin--Ionospheric E-Fields--CEDAR Student Workshop 1 Overall Magnetospheric
More informationVisualization of ion cyclotron wave and particle interactions in the inner magnetosphere via THEMIS-ASI observations
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117,, doi:10.1029/2012ja018180, 2012 Visualization of ion cyclotron wave and particle interactions in the inner magnetosphere via THEMIS-ASI observations K. Sakaguchi,
More informationThe Physics of Space Plasmas
The Physics of Space Plasmas Magnetic Storms, Substorms and the Generalized Ohm s Law William J. Burke 27 November 2012 University of Massachusetts, Lowell Lecture 10 Geomagnetic Storms: (continued ) Large
More informationIonospheric Tomography II: Ionospheric Tomography II: Applications to space weather and the high-latitude ionosphere
Ionospheric Tomography II: Ionospheric Tomography II: Applications to space weather and the high-latitude ionosphere Why tomography at high latitudes? Why tomography at high latitudes? Magnetic field railway
More informationThe Physics of Space Plasmas
The Physics of Space Plasmas Magnetic Storms and Substorms William J. Burke 14 November 2012 University of Massachusetts, Lowell Lecture 9 Course term-paper topics Geomagnetic Storms: (continued ) Volland-Stern
More informationObservations of the warm plasma cloak and an explanation of its formation in the magnetosphere
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 113,, doi:10.1029/2007ja012945, 2008 Observations of the warm plasma cloak and an explanation of its formation in the magnetosphere C. R. Chappell, 1 M. M. Huddleston,
More informationEstimates of the Suprathermal O + outflow characteristic energy and relative location in the auroral oval
Estimates of the Suprathermal O + outflow characteristic energy and relative location in the auroral oval L. Andersson, W. K. Peterson and K. M. McBryde Laboratory for Atmospheric and Space Physics, University
More informationNASA Future Magnetospheric Missions. J. Slavin & T. Moore Laboratory for Solar & Space Physics NASA GSFC
NASA Future Magnetospheric Missions J. Slavin & T. Moore Laboratory for Solar & Space Physics NASA GSFC Future Magnetospheric Missions Strategic Missions Radiation Belt Storm Probes (LWS/2011) Magnetospheric
More informationWhy Study Magnetic Reconnection?
Why Study Magnetic Reconnection? Fundamental Process Sun: Solar flares, Flare loops, CMEs Interplanetary Space Planetary Magnetosphere: solar wind plasma entry, causes Aurora Ultimate goal of the project
More informationEXTREMELY QUIET 2009 STATE OF GEOMAGNETIC FIELD AS A REFERENCE LEVEL FOR AMPLITUDE OF THE LOCAL GEOMAGNETIC DISTURBANCES
EXTREMELY QUIET 2009 STATE OF GEOMAGNETIC FIELD AS A REFERENCE LEVEL FOR AMPLITUDE OF THE LOCAL GEOMAGNETIC DISTURBANCES A.E. Levitin, L.I. Gromova, S.V. Gromov, L.A. Dremukhina Pushkov Institute of Terrestrial
More informationAdvanced modeling of low energy electrons responsible for surface charging
Advanced modeling of low energy electrons responsible for surface charging Natalia Ganushkina (1, 2), Stepan Dubyagin (1), Ilkka Sillanpää (1), Jean-Charles Matéo Vélez (3), Dave Pitchford (4) (1) Finnish
More informationOUTLINE. HISTORY CAUSES AURORA SPECTRUM AURORAL OVAL AURORA OCCURRENCE AURORAL SUBSTORM PROTON AURORA EXPERIMENTS AURORA ON OTHER PLANETS References
The Aurora OUTLINE HISTORY CAUSES AURORA SPECTRUM AURORAL OVAL AURORA OCCURRENCE AURORAL SUBSTORM PROTON AURORA EXPERIMENTS AURORA ON OTHER PLANETS References HISTORY China ~ Flying Dragons (2000 ac) Bible
More informationCluster observations of a magnetic field cavity in the plasma sheet
Cluster observations of a magnetic field cavity in the plasma sheet N.C. Draper a, M. Lester a, S.W.H. Cowley a, J.-M. Bosqued b, A. Grocott a, J.A. Wild a, Y. Bogdanova c, A.N. Fazakerley c, J.A. Davies
More informationJOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. A11, 1398, doi: /2003ja010011, 2003
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. A11, 1398, doi:10.109/003ja010011, 003 Locations of auroral kilometric radiation bursts inferred from multispacecraft wideband Cluster VLBI observations.
More informationLATITUDINAL PLASMA DISTRIBUTION IN THE DUSK PLASMASPHERIC BULGE: REFILLING PHASE AND QUASI-EQUILIBRIUM STATE
LATITUDINAL PLASMA DISTRIBUTION IN THE DUSK PLASMASPHERIC BULGE: REFILLING PHASE AND QUASI-EQUILIBRIUM STATE P. M. E. Decreau, 1,2, D. Carpenter, 3 C. R. Chappell, 1 R. H. Comfort, 4 J. Green, 1 R. C.
More informationOUTLINE. Polar cap patches: Polar Cap Patches. Core instrumentation for UiO patch studies:
Polar Cap Patches islands of high electron density, form on the day side and drift towards night side across the polar cap OUTLINE Background on polar cap patches 630 nm airglow observations in the - MLT
More informationStorm-time distortion of the inner magnetosphere: How severe can it get?
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. A5, 1209, doi:10.1029/2002ja009808, 2003 Storm-time distortion of the inner magnetosphere: How severe can it get? N. A. Tsyganenko Universities Space Research
More informationResonant scattering of plasma sheet electrons by whistler-mode chorus: Contribution to diffuse auroral precipitation
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 35, L11106, doi:10.1029/2008gl034032, 2008 Resonant scattering of plasma sheet electrons by whistler-mode chorus: Contribution to diffuse
More informationRemote sensing of magnetospheric processes: Lesson 1: Configura7on of the magnetosphere
Remote sensing of magnetospheric processes: Lesson 1: Configura7on of the magnetosphere AGF-351 Optical methods in auroral physics research UNIS, 24.-25.11.2011 Anita Aikio Dept. Physics University of
More informationChapter S1 Celestial Timekeeping and Navigation. How do we define the day, month, year, and planetary time periods?
Chapter S1 Celestial Timekeeping and Navigation S1.1 Astronomical Time Periods Our goals for learning:! How do we define the day, month, year, and planetary time periods?! How do we tell the time of day?!
More informationPlasma Observations at the Earth's Magnetic Equator
Plasma Observations at the Earth's Magnetic Equator R. C. OLSEN, S. D. SHAWHAN, D. L. GALLAGHER, J. L. GREEN, C. R. CHAPPELL, AND R. R. ANDERSON The magnetic equator provides a unique location for thermal
More informationIon heating during geomagnetic storms measured using energetic neutral atom imaging. Amy Keesee
Ion heating during geomagnetic storms measured using energetic neutral atom imaging Amy Keesee Outline Motivation Overview of ENA measurements Charge exchange MENA and TWINS ENA instruments Calculating
More informationLow Hanging Fruit. Large-Scale Dynamics & Structure
Low Hanging Fruit Large-Scale Dynamics & Structure Global Models We plan to try to run DREAM-RB continuously with both SWx data and science data. This will be a limited model (1D, T89...) For events we
More informationModeling Interactions between the Magnetosphere, Ionosphere & Thermosphere. M.Wiltberger NCAR/HAO
Modeling Interactions between the Magnetosphere, Ionosphere & Thermosphere M.Wiltberger NCAR/HAO Outline Overview of MIT circuit Modeling Magnetospheric impacts on the Ionosphere Energetic Particle Fluxes
More informationStorm-dependent radiation belt electron dynamics
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114,, doi:10.1029/2008ja013480, 2009 Storm-dependent radiation belt electron dynamics Weichao Tu, 1 Xinlin Li, 1 Yue Chen, 2 G. D. Reeves,
More informationSources and sinks of equatorially mirroring energetic charged particles in the earth s inner magnetosphere
Sources and sinks of equatorially mirroring energetic charged particles in the earth s inner magnetosphere M. M. Klida and T. A. Fritz Center for Space Physics, Boston University, Boston, MA 02215, USA
More informationTracking Solar Eruptions to Their Impact on Earth Carl Luetzelschwab K9LA September 2016 Bonus
Tracking Solar Eruptions to Their Impact on Earth Carl Luetzelschwab K9LA September 2016 Bonus In June 2015, the Sun emitted several M-Class flares over a 2-day period. These flares were concurrent with
More informationRelative contribution of electrons to the stormtime total ring current energy content
GEOPHYSICAL RESEARCH LETTERS, VOL. 32, L311, doi:1.129/24gl21672, 25 Relative contribution of electrons to the stormtime total ring current energy content S. Liu, 1 M. W. Chen, 2 J. L. Roeder, 2 L. R.
More informationMission to Understand Electron Pitch Angle Diffusion and Characterize Precipitation Bands and Spikes. J. F. Fennell 1 and P. T.
Mission to Understand Electron Pitch Angle Diffusion and Characterize Precipitation Bands and Spikes J. F. Fennell 1 and P. T. O Brien 2 1 The Aerospace Corporation, MS:M2-260, P.O.Box 92957, Los Angeles,
More informationAURORA: GLOBAL FEATURES
AURORA: GLOBAL FEATURES Jean-Claude Gérard LPAP Université de Liège OUTLINE - collisional processes involved in the aurora - remote sensing of auroral electron energy - Jupiter - Saturn MOP meeting - 2011
More informationCharacteristics of the storm-induced big bubbles (SIBBs)
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111,, doi:10.1029/2006ja011743, 2006 Characteristics of the storm-induced big bubbles (SIBBs) Hyosub Kil, 1 Larry J. Paxton, 1 Shin-Yi Su, 2 Yongliang Zhang, 1 and
More informationMagnetopause reconnection impact parameters from multiple spacecraft magnetic field measurements
Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 36, L20108, doi:10.1029/2009gl040228, 2009 Magnetopause reconnection impact parameters from multiple spacecraft magnetic field measurements
More informationLETTERS. The unexpected origin of plasmaspheric hiss from discrete chorus emissions. Jacob Bortnik 1, Richard M. Thorne 1 & Nigel P.
Vol 2 March 2008 doi:10.1038/nature01 The unexpected origin of plasmaspheric hiss from discrete chorus emissions Jacob Bortnik 1, Richard M. Thorne 1 & Nigel P. Meredith 2 Plasmaspheric hiss 1 is a type
More informationSubauroral electron temperature enhancement in the nighttime
Ann. Geophys., 24, 1871 1885, 2006 European Geosciences Union 2006 Annales Geophysicae Subauroral electron temperature enhancement in the nighttime ionosphere G. W. Prölss Argelander Institut für Astronomie,
More informationCHAPTER 2 DATA. 2.1 Data Used
CHAPTER DATA For the analysis, it is required to use geomagnetic indices, which are representatives of geomagnetic activity, and Interplanetary Magnetic Field (IMF) data in addition to f F,which is used
More informationIon multi-nose structures observed by Cluster in the inner Magnetosphere
Ann. Geophys., 25, 171 190, 2007 European Geosciences Union 2007 Annales Geophysicae Ion multi-nose structures observed by Cluster in the inner Magnetosphere C. Vallat 1,3, N. Ganushkina 2, I. Dandouras
More informationYearly variations in the low-latitude topside ionosphere
Ann. Geophysicae 18, 789±798 (2000) Ó EGS ± Springer-Verlag 2000 Yearly variations in the low-latitude topside ionosphere G. J. Bailey 1,Y.Z.Su 1, K.-I. Oyama 2 1 Department of Applied Mathematics, The
More informationModeling the wave normal distribution of chorus waves
JOURNAL OF GEOPHYSICAL RESEARCH: SPACE PHYSICS, VOL. 8, 74 88, doi:.9/ja8343, 3 Modeling the wave normal distribution of chorus waves Lunjin Chen, Richard M. Thorne, Wen Li, and Jacob Bortnik Received
More informationTime Series of Images of the Auroral Substorm
ESS 7 Lecture 13 October 27, 2010 Substorms Time Series of Images of the Auroral Substorm This set of images in the ultra-violet from the Polar satellite shows changes that occur during an auroral substorm.
More informationMAE 180A: Spacecraft Guidance I, Summer 2009 Homework 2 Due Tuesday, July 14, in class.
MAE 180A: Spacecraft Guidance I, Summer 2009 Homework 2 Due Tuesday, July 14, in class. Guidelines: Please turn in a neat and clean homework that gives all the formulae that you have used as well as details
More informationThe Structure of the Magnetosphere
The Structure of the Magnetosphere The earth s magnetic field would resemble a simple magnetic dipole, much like a big bar magnet, except that the solar wind distorts its shape. As illustrated below, the
More informationMass density inferred from toroidal wave frequencies and its comparison to electron density
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111,, doi:10.1029/2005ja011286, 2006 Mass density inferred from toroidal wave frequencies and its comparison to electron density Kazue Takahashi, 1 Richard E. Denton,
More information2-1-4 Preceding Monitoring of Solar Wind Toward the Earth Using STEREO
2-1-4 Preceding Monitoring of Solar Wind Toward the Earth Using STEREO NAGATSUMA Tsutomu, AKIOKA Maki, MIYAKE Wataru, and OHTAKA Kazuhiro Acquisition of solar wind information before it reaches the earth
More informationMagnetic Reconnection
Magnetic Reconnection? On small scale-lengths (i.e. at sharp gradients), a diffusion region (physics unknown) can form where the magnetic field can diffuse through the plasma (i.e. a breakdown of the frozenin
More informationPoloidal ULF wave observed in the plasmasphere boundary layer
JOURNAL OF GEOPHYSICAL RESEARCH: SPACE PHYSICS, VOL. 118, 4298 4307, doi:10.1002/jgra.50427, 2013 Poloidal ULF wave observed in the plasmasphere boundary layer W. Liu, 1,2 J. B. Cao, 1,2 X. Li, 3 T. E.
More informationTitan s Atomic and Molecular Nitrogen Tori
s Atomic and Molecular Nitrogen Tori H.T. Smith a, R.E. Johnson a, V.I. Shematovich b a Materials Science and Engineering, University of Virginia, Charlottesville, VA 9 USA b Institute of Astronomy, RAS,
More informationFeatures of the F3 layer occurrence over the equatorial location of Trivandrum
Ann. Geophys., 28, 1741 1747, 2010 doi:10.5194/angeo-28-1741-2010 Author(s) 2010. CC Attribution 3.0 License. Annales Geophysicae Features of the F3 layer occurrence over the equatorial location of Trivandrum
More informationCorrelations between low-frequency and high-frequency auroral kilometric radiation plasma wave intensity bursts and X rays in the auroral zone
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 109,, doi:10.1029/2003ja010357, 2004 Correlations between low-frequency and high-frequency auroral kilometric radiation plasma wave intensity bursts and X rays in
More informationSingle particle motion and trapped particles
Single particle motion and trapped particles Gyromotion of ions and electrons Drifts in electric fields Inhomogeneous magnetic fields Magnetic and general drift motions Trapped magnetospheric particles
More informationHow is Earth s Radiation Belt Variability Controlled by Solar Wind Changes
How is Earth s Radiation Belt Variability Controlled by Solar Wind Changes Richard M. Thorne Department of Atmospheric and Oceanic Sciences, UCLA Electron (left) and Proton (right) Radiation Belt Models
More informationON THE PERIODIC MODULATION OF ENERG TitleELECTRONS IN THE MAGNETOSPHERIC SKI REGION.
ON THE PERIODIC MODULATION OF ENERG TitleELECTRONS IN THE MAGNETOSPHERIC SKI REGION Author(s) SAKURAI, Kunitomo Citation Special Contributions of the Geophy University (1967), 7: 15-21 Issue Date 1967-12
More informationMagnetospheric Model Performance during Conjugate Aurora
18 Magnetospheric Model Performance during Conjugate Aurora William Longley 1, Patricia Reiff 1, Jone Peter Reistad 2, and Nikolai Østgaard 2 Video of Yosemite Talk, URL: http://dx.doi.org/10.15142/t3h01c
More informationPlasma refilling rates for L = flux tubes
Click Here for Full Article JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 115,, doi:10.1029/2009ja014191, 2010 Plasma refilling rates for L = 2.3 3.8 flux tubes Yuki Obana, 1,2 Frederick W. Menk, 1 and Ichiro
More informationMagnetosphere-Ionosphere-Thermosphere Coupling During Storms and Substorms
Magnetosphere-Ionosphere-Thermosphere Coupling During Storms and Substorms Bill Lotko Bin Zhang Oliver Brambles Sheng Xi John Lyon Tian Luo Roger Varney Jeremy Ouellette Mike Wiltberger 2 3 4 CEDAR: Storms
More informationG. Balasis (1), I. A. Daglis (1,2), M. Georgiou (1,2), C. Papadimitriou (1,2), E. Zesta (3), I. Mann (4) and R. Haagmans (5)
G. Balasis (1), I. A. Daglis (1,2), M. Georgiou (1,2), C. Papadimitriou (1,2), E. Zesta (3), I. Mann (4) and R. Haagmans (5) (1) IAASARS-National Observatory of Athens; (2) University of Athens; (3) NASA;
More informationLow energy electrons at MEO during observed surface charging events
Low energy electrons at MEO during observed surface charging events N. Ganushkina (1, 2), I. Sillanpää (1), Jean-Charles Matéo-Vélez (3), S. Dubyagin (1), Angélica Sicard-Piet (3), S. Claudepierre (4),
More informationAtmospheric Structure
Atmospheric Structure The gaseous area surrounding the planet is divided into several concentric strata or layers. About 99% of the total atmospheric mass is concentrated in the first 20 miles (32 km)
More informationStatistical analysis of plasmaspheric plumes with Cluster/WHISPER observations
Ann. Geophys., 26, 23 217, 28 www.ann-geophys.net/26/23/28/ European Geosciences Union 28 Annales Geophysicae Statistical analysis of plasmaspheric plumes with Cluster/WHISPER observations F. Darrouzet
More informationObserving SAIDs with the Wallops Radar
Observing SAIDs with the Wallops Radar Raymond A. Greenwald, Kjellmar Oksavik, J. Michael Ruohoniemi, and Joseph Baker The Johns Hopkins University Applied Physics Laboratory SuperDARN-Storms New Technologies--Antenna
More informationA New Equatorial Plasma Bubble Prediction Capability
A New Equatorial Plasma Bubble Prediction Capability Brett A. Carter Institute for Scientific Research, Boston College, USA, http://www.bc.edu/research/isr/, RMIT University, Australia, www.rmit.edu.au/space
More informationAdvanced Technology Center, Lockheed Martin Space Systems Company, Palo Alto, California, USA
1 Solar wind control of Earth s H + and O + outflow rates in the 15-eV to 33-keV energy range O.W. Lennartsson and H.L. Collin Advanced Technology Center, Lockheed Martin Space Systems Company, Palo Alto,
More information