Morphology of Inner Magnetospheric low-energy ions M. Yamauchi, et al. Swedish Institute of Space Physics (IRF), Kiruna.

Slides:



Advertisements
Similar presentations
Locations of Boundaries of the Outer and Inner Radiation Belts during the Recent Solar Minimum, as Observed by Cluster and Double Star Natalia Ganushkina.
Advertisements

Solar flare hard X-ray spikes observed by RHESSI: a statistical study Jianxia Cheng Jiong Qiu, Mingde Ding, and Haimin Wang.
Electron Acceleration in the Van Allen Radiation Belts by Fast Magnetosonic Waves Richard B. Horne 1 R. M. Thorne 2, S. A. Glauert 1, N. P. Meredith 1.
1 FIREBIRD Science Overview Marcello Ruffolo Nathan Hyatt Jordan Maxwell 2 August 2013FIREBIRD Science.
U N C L A S S I F I E D Operated by the Los Alamos National Security, LLC for the DOE/NNSA Pitch angle evolution of energetic electrons at geosynchronous.
Evidence at Saturn for an Inner Magnetospheric Convection Pattern, Fixed in Local Time M. F. Thomsen (1), R. L. Tokar (1), E. Roussos (2), M. Andriopoulou.
Seminar S 3, IMPRS, MPAeJanuary 9, 2003 N. Krupp Planetary Magnetospheres: Global Configuration and Dynamics of the Jovian Magnetosphere N. Krupp Solar.
Fate of sub-keV ring current ions observed by Viking Viking 20 years Yamauchi and Lundin * Superposed epoch analyses * Viking Ion data + AE (and Dst) 
ESS 7 Lecture 14 October 31, 2008 Magnetic Storms
Sudden appearance of sub- keV structured ions in the inner magnetosphere within one hour: drift simulation M. Yamauchi 1, Y. Ebihara 2, I. Dandouras 3,
Budget and Roles of Heavy Ions in the Solar System M. Yamauchi, I. Sandahl, H. Nilsson, R. Lundin, and L. Eliasson Swedish Institute of Space Physics (IRF)
Auxiliary slides. ISEE-1 ISEE-2 ISEE-1 B Locus of  = 90 degree pitch angles Will plot as a sinusoid on a latitude/longitude projection of the unit.
Space Weather Workshop, Boulder, CO, April 2013 No. 1 Ionospheric plasma irregularities at high latitudes as observed by CHAMP Hermann Lühr and.
PLASMA TRANSPORT ALONG DISCRETE AURORAL ARCS A.Kullen 1, T. Johansson 2, S. Buchert 1, and S. Figueiredo 2 1 Swedish Institute of Space Physics, Uppsala.
1 Geomagnetic/Ionospheric Models NASA/GSFC, Code 692 During the early part of April 6, 2000 a large coronal “ejecta” event compressed and interacted with.
Tuija I. Pulkkinen Finnish Meteorological Institute Helsinki, Finland
Cusp O+ H+ e- "SPI" event #1 event #2 MLT energy ratio = 15~20 O+ H+ 68°CGLat66°CGLat 63°CGLat #1) Mono-energetic ion injection with O+ faster.
Magnetospheric ULF wave activity monitoring based on the ULF-index OLGA KOZYREVA and N. Kleimenova Institute of the Earth Physics, RAS.
Does Fermi Acceleration of account for variations of the fluxes of radiation belt particles observations at low altitudes during geomagnetic storms? J.
Finite Gyroradius Effect in Space and Laboratory 1. Radiation belt (Ring current) 2. Auroral phenomena (Substorm current) 3. Shock acceleration and upstream.
STB CIR events #17,19,20,22 are from period Dec 2007-Feb 2008 (Bucik et al., AnGeo, 2009) these two bursts periods show an excess in number of counts beyond.
1 Cambridge 2004 Wolfgang Baumjohann IWF/ÖAW Graz, Austria With help from: R. Nakamura, A. Runov, Y. Asano & V.A. Sergeev Magnetotail Transport and Substorms.
© 2008 The Aerospace Corporation Workshop on Coupling of Thunderstorms and Lightning to Near-Earth Space University of Corsica, June 2008 SAMPEX.
Fate of cold ions in the inner magnetosphere: energization and drift inferred from morphology and mass dependence M. Yamauchi 1, I. Dandouras 2, H. Reme.
Magnetosphere-Ionosphere coupling processes reflected in
Hot He + events in the inner magnetosphere observed by Cluster M. Yamauchi 1, I. Dandouras 2, H. Reme 2, H. Nilsson 1 (1) Swedish Institute of Space Physics.
9 May MESSENGER First Flyby Magnetospheric Results J. A. Slavin and the MESSENGER Team BepiColombo SERENA Team Meeting Santa Fe, New Mexico 11 May.
PAPER I. ENA DATA ANALYSIS RESULTS. The Imager for Magnetopause-to- Aurora Global Exploration (IMAGE) missionis the first NASA Mid-size Explorer (MIDEX)
Initial Measurements of O-ion and He-ion Decay Rates Observed from the Van Allen Probes RBSPICE Instrument Andrew Gerrard, Louis Lanzerotti et al. Center.
Large electric fields near the nightside plasmapause observed by the Polar spacecraft K.-H. Kim 1, F. Mozer 2, and D.-H. Lee 1 1 Department of Astronomy.
Sub-keV Ring Current Ions: Source, Transport, and O+/H+ difference M. Yamauchi, R. Lundin, H. Nilsson, S. Arvelius (IRF-Kiruna), Y. Ebihara (NIPR), and.
Cold plasma: a previously hidden solar system particle population Mats André and Chris Cully Swedish Institute of Space Physics, Uppsala.
Oxygen Injection Events observed by Freja Satellite M. Yamauchi 1, L. Eliasson 1, H. Nilsson 1, R. Lundin 1, and O. Norberg 2 1.Swedish Institute of Space.
Equatorial signatures of an auroral bulge and a filamentation/demarcation of a transpolar arc observed by Cluster M. Yamauchi 1, I. Sandahl 1, R. Lundin.
1 THEMIS Inner Magnetosphere Review, Dec 20, 2008 Summary of THEMIS results in the inner magnetosphere Future mission operations discussion: –Science targets.
M. Yamauchi 1, H. Nilsson 1, I. Dandouras 2, H. Reme 2, R. Lundin 3, Y. Ebihara 4 (1) Swedish Institute of Space Physics (IRF), Kiruna, Sweden (2) CNRS.
Energy conversion at Saturn’s magnetosphere: from dayside reconnection to kronian substorms Dr. Caitríona Jackman Uppsala, May 22 nd 2008.
Escaping ions over polar cap. Inner magnetosphere, Bow shock/Foreshock, and Ancient magnetosphere.
A. Vaivads, M. André, S. Buchert, N. Cornilleau-Wehrlin, A. Eriksson, A. Fazakerley, Y. Khotyaintsev, B. Lavraud, C. Mouikis, T. Phan, B. N. Rogers, J.-E.
Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University.
NASA NAG Structure and Dynamics of the Near Earth Large-Scale Electric Field During Major Geomagnetic Storms P-I John R. Wygant Assoc. Professor.
Substorm-origin sub-keV ring current ions: wedge-like structure ICS-9, Graz, ~7 Substorm : production of plasma Sub-keV ring current : fossil of.
Global Structure of the Inner Solar Wind and it's Dynamic in the Solar Activity Cycle from IPS Observations with Multi-Beam Radio Telescope BSA LPI Chashei.
Hot He + events in the inner magnetosphere observed by Cluster 1 Yamauchi, et al. (2014), JGR, doi: /2013JA Inner magnetosphere: Majority.
The large scale convection electric field, ring current energization, and plasmasphere erosion in the June 1, 2013 storm Scott Thaller Van Allen Probes.
Morphology of Inner Magnetospheric low- energy ions M. Yamauchi 1, I. Dandouras 2, H. Reme 2, R. Lundin 3, L.M. Kister 4, F. Mazouz 5, Y. Ebihara 6 (1)
MULTI-INSTRUMENT STUDY OF THE ENERGY STEP STRUCTURES OF O + AND H + IONS IN THE CUSP AND POLAR CAP REGIONS Yulia V. Bogdanova, Berndt Klecker and CIS TEAM.
© Research Section for Plasma and Space Physics UNIVERSITY OF OSLO Daytime Aurora Jøran Moen.
Swedish Institute of Space Physics, Kiruna M. Yamauchi 1 Different Sun-Earth energy coupling between different solar cycles Acknowledgement:
Particle energization at Saturn C. Paranicas 1, E. Roussos 2, P. Kollmann 2, N. Krupp 2, J. F. Carbary 1, D. G. Mitchell 1, S. M. Krimigis 1, B. H. Mauk.
Oxygen Injection Events observed by Freja M. Yamauchi IRF-Kiruna * Motivation / Examples * Distribution (mainly in nightside) * Unusual events (dayside)
Lecture 15 Modeling the Inner Magnetosphere. The Inner Magnetosphere The inner magnetosphere includes the ring current made up of electrons and ions in.
On-Line Visualization Ring Current / Radiation Belt.
Modulation of chorus wave intensity by ULF waves from Van Allen Probes Observation Lunjin Chen 1, Zhiyang Xia 1, Lei Dai 2 1 Physics Dept., The University.
Magnetospheric Solitary Structure maintained by 3000 km/s ions and its relation to Auroral Bulge after a Substorm M. Yamauchi1, H. Nilsson1, I. Dandouras2,
Plasma Wave Excitation Regions in the Earth’s Global Magnetosphere
Disturbance Dynamo Effects in the Low Latitude Ionosphere
M. Yamauchi1, I. Dandouras2, H. Reme2,
Sub-keV Phenomena of Dayside Ring Current
Oxygen Injection Events observed by Freja Satellite
Source Location of the Wedge-like Dispersed (sub-keV) Ring Current in the Morning Sector During a Substorm M. Yamauchi (IRF-Kiruna), P.C. Brandt, Y. Ebihara,
M. Yamauchi1, H. Nilsson1, R. Lundin1, I. Dandouras2, H. Reme2, H
Sources of < 10 keV ring current ions: supply mechanism?
Magnetospheric solitary structure maintained by 3000 km/s ions as a cause of westward moving auroral bulge at 19 MLT M. Yamauchi1, I. Dandouras2, P.W.
Yama's works Using geomagnetic data
Yuki Takagi1*, Kazuo Shiokawa1, Yuichi Otsuka1, and Martin Connors2  
Debye-like shielding effect on low-cloud electricity by the radioactive aerosol after Fukushima nuclear accident M. Yamauchi1, M. Takeda2, M. Makino3,
Swedish Institute of Space Physics (IRF), Kiruna
M. Yamauchi1, T. Sergienko1, C. -F. Enell2, A. Schillings1, R
Past cusp researches: (potentially) missing facts
Presentation transcript:

Morphology of Inner Magnetospheric low-energy ions M. Yamauchi, et al. Swedish Institute of Space Physics (IRF), Kiruna

Ion drift under strong B-field (e.g. inner magnetosphere) Magnetic drift (Energy dependent) * gradient-B drift * curvature drift ⇒ dominant for > 10 keV ExB drift (Energy independent) * co-roration E-field * external E-field ⇒ dominant for < 0.1 keV

Ion drift Energy dependent for magnetic drift and Energy independent for ExB drift/corotation external E-field

Ion drift Westward drift for high energy/evening and Eastward drift for low-energy/morning

Ion drift Variation in the source and E-field makes the ion population a zoo of various patterns

Characteristic of Cluster Perigee * North-South symmetric * Quick scan of all latitude

The examined ion signatures (1) (b) Wedge-like energy-latitude dispersed ions at sub-keV range: predominantly found in the morning sector some hours after a substorm. The source population is much colder than the plasma sheet. (both symmetric/asymmetric) (e) Internal asymmetry of (b)

(c) Vertical stripes: similar to the wedge-like structure but dispersion is weak (nearly vertical in the spectrogram). The energy extends from the about 10 keV to sub-keV. (both symmetric/asymmetric) The examined ion signatures (2)

The examined ion signatures (3) (d) Short bursts of low-energy ions isolated from the above structures: a peak energy flux less than 100 eV but not thermal. (both symmetric/asymmetric)

The examined ion signatures (4) (f) Warm trapped ions confined near equator: ~ tens eV to a few hundred eV.

(b) Wedge-like energy-latitude dispersed ions at sub-keV range: predominantly found in the morning sector some hours after a substorm. The source population is much colder than the plasma sheet. (c) Vertical stripes: similar to the wedge-like structure but dispersion is weak (nearly vertical in the spectrogram). The energy extends from the about 10 keV to sub-keV. (d) Short bursts of low-energy ions isolated from the above structures: a peak energy flux less than 100 eV but not thermal. (e) Internal asymmetry of (b) (f) Warm trapped ions confined near equator: tens eV to a few hundred eV. The examined ion signatures (1)-(4)

Characteristic of Cluster Perigee * North-South symmetric * Quick scan of all latitude + north-south symmetric nature of trapped ions (due to bouncing)  Distribution must be north-south symmetric

Where? Inner Magnetosphere at 4~6 R E (Cluster perigee) Species? H + of 10 eV ~ 10 keV (CIS/CODIF energy range) Distribution? Intense ion population (except plasma sheet) In this work: (a) Statistics distribution, (b) 1-2 hour scale evolution/decay (using inbound-outbound asymmetry), (c) relation to substorms (using elapsed time from high AE), (d) modeling (using Ebihara’s simulation code). We examined all SC-4 perigee pass during (about 670 traversals, with relatively clean data of 460 traversals). Analyses

Before analyses, we have to examine possible “biases” such as Instrument Degradation or Solar Cycle phase Database quality check  We examine both “inbound-outbound” symmetric & asymmetric cases

Decrease of “wedge-like” is not due to solar cycle ! Occurrence of substorm is rather constant 

The same for “low-energy burst” Occurrence of substorm is rather constant 

But “vertical stripes” show some solar cycle effect

Rather, the decrease is due to instrumental effect  Rapid degradation of the sensor Occurrence of substorm is rather constant 

Impossible to take statistics during because of radiation dose. Otherwise large decrease. How about warmed trapped ions?  Rapid degradation of the sensor Occurrence of substorm is rather constant 

(1) Both & show morning peak  We can safely use data together. (2) Very high observation frequency in the morning (> 80%) Next check: Is Local Time distribution affected by this bias?

Local Time distribution symmetric + asymmetric enhanced within traversal Wedge-like: high-occurrence (morning) peak is not midnight enhance > symmetric > decay Vertical stripe: midnight phenomena enhance (midnight) decay ~ enhance (other LT) Low-energy burst: all local time enhance ~ decay  time scale ~ 1 hour enhance/decay  factor 3 change

Is enhancement related to substorm? AL AU AL AU

eastward drift Viking 14 MLT poleward 6 MLT 9 MLT 12 MLT 15 MLT 18 MLT For the wedge-like dispersion, the relation to substorm has already been studied: After AE>400 nT activity, (1) Moves eastward (2) Decay in time hr from substorm cf. Viking

Relation to AE activities Local Time distribution * Strong preference during |AL|>300 nT activity * Outstanding at midnight  Related to substorm-related injction * Optimum at 300 nT threshold (cf. 200, 400 nT) Vertical stripes

Relation to AE activities Local Time distribution * Same result as Viking (morning~0h, afternoon>5h) * Less enhancement with elapsed time  stagnation * Yet, enhancements after 5h & aftrnoon  ??? Wedge-like dispersion

Relation to AE activities Local Time distribution * slight decrease of “change” with time * but  stagnation Low-energy burst

The inner magnetospheric low-energy ion populations (1)-(3) below show significant changes within 1-2 hours. (1) Wedge-like energy-latitude dispersed ions (< a few keV), (2) Vertical stripes (< 10 keV), (3) Short-lived low-energy ion burst (< few hundred eV). For all three patterns, asymmetric cases (large inbound- outbound difference) are found more often than symmetric cases at almost all LT. For vertical stripes, majority of local midnight pass show large inbound-outbound difference when AL<300 nT. For low-energy burst, the lifetime is estimated as short as 1 hour Summary 1

Where? Inner Magnetosphere at 4~6 R E (Cluster perigee) Species? H + of 10 eV ~ 10 keV (CIS/CODIF energy range) Distribution? Intense ion population (except plasma sheet) In this work: (a) Statistics distribution, (b) 1-2 hour scale evolution/decay (using inbound-outbound asymmetry), (c) relation to substorms (using elapsed time from high AE), (d) modeling (using Ebihara’s simulation code). We examined all SC-4 perigee pass during (about 670 traversals, with relatively clean data of 460 traversals). Next

Relation to AE activities Local Time distribution * Same result as Viking (morning~0h, afternoon>5h) * Less enhancement with elapsed time  stagnation * Yet, enhancements after 5h & aftrnoon  ??? Wedge-like dispersion

Why inbound-outbound difference of “wedge” at Noon-Afternoon sector so often? ⇒ We examine using numerical simulation (Ebihara’s code)

The ion drift alone can re-produce significant inbound-outbound difference ! 0.1 keV t ≈ 15 hr

Another example: sub-keV (dispersion asymmetry) and a few keV (ion band) 0.1 keV t ≈ 6 hr t ≈ 4 hr

The significant changes of the “ Wedge-like dispersed sub-keV ions within only 1-2 hours can be explained by the drift motion even in the noon-afternoon sector. But some signatures are yet naturally explained by the local inflow from ionosphere, that also has short time scale. For both sources, the ion energy is very low (< 0.1 keV) but not cold. Summary 2

Future work: * Mass dependence * Pitch-angle dependence

note: // >> ⊥ does not necessarily mean ionospheric source but mirroring ions

Next

equator Confined near equator = Only  direction spin axis SC motion sectors ≈ PA E(H + ) << E(He + ) : new

equator All Local time All AE conditions Energy-time dispersion = new Appearing in 40 min = new! statistics & dynamics

Summary 3 We also studied the “equatorially-trapped warm ions” which are basically symmetric between inbound and outbound The energy of He + is often higher than that for H +. Some events show a non-thermal ring distribution rather than superthermal pancake distribution. Some events show energy-time dispersion, indicating drifts from different local times. The time scale of the development is again about 1 hour. At about R E, the observation probability is about 1/3 (night-dawn) to 1/2 (noon-dusk). The He + /H + ratio is variable and is much less than 5% for the majority of the cases.

Future work: (2) (n+(1/2))f ce wave is accompanied * relation to wave

Future work: * relation to wave * compare different SC