Effects of Solar Energetic Effects of Solar Energetic Particles and Radiation Belt Particles and Radiation Belt Precipitation on the Middle Precipitation on the Middle Atmosphere and the Global Atmosphere and the Global

Electric CircuitElectric CircuitEdgar A. Bering, III, Michael Kokorowski, Edgar A. Bering, III, Michael Kokorowski,

Robert H. Holzworth, Mark J. Engebretson, Robert H. Holzworth, Mark J. Engebretson, Jennifer L. Posch, John G. Sample, David M. Jennifer L. Posch, John G. Sample, David M. Smith, Akira Kadokura, Brandon D. Reddell, Smith, Akira Kadokura, Brandon D. Reddell,

and Hisao Yamagishiand Hisao Yamagishi

Outline of TalkOutline of Talk

IntroductionIntroduction PPB CampaignPPB Campaign Jan 27, 2003 EventJan 27, 2003 Event

Conductivity perturbationConductivity perturbation Pc1 event, Proton PrecipitationPc1 event, Proton Precipitation

MINIS CampaignMINIS Campaign Jan 20, 2005 SEP eventJan 20, 2005 SEP event

Vertical field responseVertical field response Convection responseConvection response

Global CircuitGlobal Circuit Generators:Generators:

Tropospheric Tropospheric ThunderstormsThunderstorms

Cross-Polar Cap Cross-Polar Cap PotentialPotential

Quiet day Ionospheric Quiet day Ionospheric Dynamo (Dynamo (SSqq))

and other possible and other possible unknown sourcesunknown sources

Return Path Through Return Path Through Ionosphere, Fair Ionosphere, Fair Weather AtmosphereWeather Atmosphere

Model Rests on Very Model Rests on Very Meager Data BaseMeager Data Base

Geophysics Balloon ClusterGeophysics Balloon Cluster

Balloon LocationsBalloon Locations

Range: 450 km

Conjugate PathsConjugate Paths

Solar Wind, IMF, Solar Wind, IMF, GOESGOES

Canopus Magnetometer DataCanopus Magnetometer Data

Wave EventWave Event

σσ increase at one increase at one balloon appears to balloon appears to correlate with large correlate with large scale ULF wave eventscale ULF wave event

Global Pc 1 Global Pc 1 EventEvent

Seen in both Seen in both hemisphereshemispheres

Seen at P2, A80, Seen at P2, A80, A81, A84A81, A84

PolarPolarS.PoleS.Pole

Conductivity PerturbationConductivity PerturbationRange: 450 km

Other DataOther Data No X-ray counts, but…No X-ray counts, but… E-field invertsE-field inverts

electrified stormelectrified storm Strange Riometer DataStrange Riometer Data

DiscussionDiscussion

What caused of the factor of 2 σ increase observed by PPB #8 on 27 January 2003? Electrons and X-rays ruled out by the absence of any X-ray counts in the on-board detector. Two ideas are: precipitating energetic protons, or the nearby tropospheric storm .

Proton EvidenceProton Evidence

IMAGE SIP Proton Auroral Images

FUV proton auroral images from the IMAGE spacecraft for 17:48 to 18:05 UT on 27 January 2003.

Proton EvidenceProton Evidence Energetic proton

count rates from the RDM detector on Akebono and the >16 MeV channel from the POES/MEPOmni detector on NOAA-15,-16 and -17 plotted in an L-shell vs. UT spectrogram format for 27 January 2003.

Proton EvidenceProton Evidence

Proton SummaryProton Summary•An MeV proton event was seen in the outer belt at the right time/place•IMAGE FUV proton aurora images show arc near balloon location.•Event was initiated by SI and IMF orientation change•Pc1 waves with f near equatorial fc,H were seen with same time envelope as σ bump.

Jan 27, 2003 ConclusionJan 27, 2003 Conclusion•It appears to us that precipitating energetic protons are the leading candidate explanation.•This conclusion points to the fact that MeV protons sometimes contribute to the post-noon proton hotspot. •Major reasons are the better temporal agreement and the lack of known mechanism for the storm explanation. •The observation of an electrified extra-tropical cyclone at this latitude is unusual and significant.

MINIS: The Balloon FlightsMINIS: The Balloon Flights

Small, hand-launched Small, hand-launched balloonsballoons 300,000 ft300,000 ft33

70 lb payload70 lb payload 8 day flights8 day flights 35 km (115,000 ft) 35 km (115,000 ft)

float altitudefloat altitude

MINIS: The InstrumentsMINIS: The Instruments X ray scintillation counterX ray scintillation counter

Detailed, broad energy Detailed, broad energy spectrumspectrum

10 MeV maximum10 MeV maximum Electric field, 3 axisElectric field, 3 axis Magnetic field, 3 axisMagnetic field, 3 axis

Dc-0.5hz, both fieldsDc-0.5hz, both fields VLF wave power (1-30 VLF wave power (1-30

kHz)kHz) One axis each electric and One axis each electric and

magnetic fieldmagnetic field Ambient temperatureAmbient temperature

MINIS: The PlaceMINIS: The Place

SANAESANAE

Flare X-rays were Flare X-rays were detected by the balloon at detected by the balloon at the same time RHESSI the same time RHESSI sees main high energy sees main high energy portion of flare.portion of flare.

Counting rates jump Counting rates jump rapidly about 15 min after rapidly about 15 min after x-ray flare, saturating x-ray flare, saturating detector and creating detector and creating severe dead-time effects.severe dead-time effects.

Class X7.1 Flare, 20 Jan 2005Class X7.1 Flare, 20 Jan 2005

Mo Dy Begin Max End Reg# Lat CMD X-classMo Dy Begin Max End Reg# Lat CMD X-class

Jan 20 0227 0636 0701 0726 N14 W61 X 7.1 Ion Storm, Ground Level EnhancementJan 20 0227 0636 0701 0726 N14 W61 X 7.1 Ion Storm, Ground Level Enhancement

Raw X-ray spectra from 2S for the interval 0600-0900 UT on 20 Jan 2005, showing details of the flare onset.

X-ray flare Ion Storm

Flare X-rays were Flare X-rays were detected by the balloon at detected by the balloon at the same time RHESSI the same time RHESSI sees main high energy sees main high energy portion of flare.portion of flare.

Counting rates jump Counting rates jump rapidly about 15 min after rapidly about 15 min after x-ray flare, saturating x-ray flare, saturating detector and creating detector and creating severe dead-time effects.severe dead-time effects.

Class X7.1 Flare, 20 Jan 2005Class X7.1 Flare, 20 Jan 2005

Mo Dy Begin Max End Reg# Lat CMD X-classMo Dy Begin Max End Reg# Lat CMD X-class

Jan 20 0227 0636 0701 0726 N14 W61 X 7.1 Ion Storm, Ground Level EnhancementJan 20 0227 0636 0701 0726 N14 W61 X 7.1 Ion Storm, Ground Level Enhancement

Raw X-ray spectra from 2S for the interval 0600-0900 UT on 20 Jan 2005, showing details of the flare onset.

X-ray flare Ion Storm

1-8 Å

0.5-3 Å

> 2 MeV e-

> 100 MeV H+

> 1 MeV H+

150-250 MeV

300-500 300-500 MeV MeV

Hp (perp to orbit plane)noon

midnight

X2.622:25 15 Jan

Fast CME1850 km/s

X3.807:02 17 JanFast CME2400 km/s

X1.308:03 19 JanHalo CME1960 km/s

X7.106:36 20 JanHalo CME

Ground level event

GOES Summary PlotGOES Summary Plot

Ground Level EventGround Level Event Observed neutron Observed neutron

monitor increases for monitor increases for GLE 69. GLE 69.

Top: Polar stations with Top: Polar stations with cutoff rigidity < 1 GV.cutoff rigidity < 1 GV.

Bottom: Stations with Bottom: Stations with cutoff rigidity > 1 GV.cutoff rigidity > 1 GV.

(Highest Rigidity (Highest Rigidity displayed: Hermanus, Rc displayed: Hermanus, Rc = 4.4 GV, ~7%)= 4.4 GV, ~7%)

(Highest Rigidity (Highest Rigidity recorded: Athens, Rc recorded: Athens, Rc = 8.4 GV, ~2%)= 8.4 GV, ~2%)

14 15 16 17 18 19 20 21 22

10-1

101

103

January 2005

Four separate solar proton events in time period.

>10 MeV >50 MeV >100 MeV

Proton Flux Measurements by GOES 11Proton Flux Measurements by GOES 11 (Particles cm (Particles cm-2-2 s s-1-1 sr sr-1-1))

X 7.1/2b Solar Proton Flare at 0636X 7.1/2b Solar Proton Flare at 0636

Jumps

Jumps Followed By Proton PeaksJumps Followed By Proton Peaks

Global Current FlowsGlobal Current Flows

Each Jump Each Jump preceded by preceded by ΔΔBBXX>0 spike in >0 spike in

auroral zoneauroral zone

Details of the Electric fieldDetails of the Electric field

Horizontal Electric FieldHorizontal Electric Field

Convection Convection disappears at disappears at the time of the the time of the SEP eventSEP event

Magnetic ActivityMagnetic Activity

Magnetic Magnetic activity already activity already lowlow

Absent for 6 Absent for 6 hours following hours following flareflare

SuperDarn SummarySuperDarn Summary

Potential estimate was Model not Data Potential estimate was Model not Data DrivenDriven

Data Points ~0 for 2 Hours after flareData Points ~0 for 2 Hours after flare

ConclusionsConclusions

Solar protons strongly Solar protons strongly affect global circuit.affect global circuit.

Changes of Changes of stratospheric stratospheric conductivityconductivity

Major changes in Major changes in vertical fieldvertical field

Short out the Short out the magnetosphere?magnetosphere?

Stay tuned. Exciting Stay tuned. Exciting results pending!results pending!