overview of energgp()etic particle precipitation (epp ... of energgp()etic particle precipitation...

Overview of Energetic Particle Precipitation (EPP) g p ( )

Effects on the Earth's Atmosphere

Charles JackmanNASA Goddard Space Flight Center Greenbelt MDNASA Goddard Space Flight Center, Greenbelt, MD

October 9, 2012

Acknowledgments:Cora Randall

University of Colorado, Boulder, CO

Daniel Marsh, Francis Vitt, and Rolando GarciaNational Center for Atmospheric Research, Boulder, CO

Eric FlemingNASA Goddard Space Flight Center, Greenbelt, MD

Sh h i WShuhui WangJPL, California Institute of Technology, Pasadena, CA

Pekka VerronenPekka Verronen Finnish Meteorological Institute, Helsinki, FINLAND

Bernd FunkeInstituto de Astrofisica de Andalucia, CSIC, Granada, SPAIN

OutlineI. Introduction

II. EPP-caused HOx and Ozone Change

III. EPP-caused NOx, NOy, and Ozone Change

IV. Conclusions

I IntroductionI. Introduction

Ulti t i i f t E ti P ti lUltimate origin of most Energetic Particlesis the Sun

Galactic Cosmic Rays (GCRs)originate outside the Solar System

and will not be discussed

I IntroductionI. Introduction

Ulti t i i f t E ti P ti lUltimate origin of most Energetic Particlesis the Sun

Galactic Cosmic Rays (GCRs)Stay tuned f Jó E ill K i tjá ’ T lkoriginate outside the Solar System

and will not be discussed for Jón-Egill Kristjánsson’sTalk

at 11:10 Tomorrow about GCR impacts

Overview ofEnergetic Particle Precipitation

Electrons and Protonscomprise most (~90% or so) of these Particles

Higher flux of particles associated with:Higher flux of particles associated with:1) Solar flares, 2) Coronal mass ejections (CMEs),3) Geomagnetic storms

Animation ofC l M Ej tiCoronal Mass Ejection

Electron PrecipitationLower energy

Auroral electrons auroral zone [~62-75o geomag. lat.]

50o60o

70o 80o 90oN geomagnetic

40o

50

Medium & high energy electrons subauroral zone [~55-65o geom. lat.]

Each zone is ~9% of Earth area.

Protons also come via CMEs

Earthand enter through the magnetosphere

“S l P t E t (SPE)”

Earthnear the poles and precipitate there

“Solar Proton Event (SPE)”

GOES

Sun

GOES Geostationary Operational Environmental SatellitesGOES - Geostationary Operational Environmental Satellites

Proton PrecipitationS l tSolar protons

60o70o 80o 90oN geomagnetic

Polar Caps >~60o geomag. lat.

40o

50o60

Very intense solar events push polar cap boundaries Equatorward

About 14% of Earth is affectedduring solar proton events.during solar proton events.

125Thermosphere

100

m)

MesosphereMesopause

75

tude

(km Mesosphere

Middl

25

50

Alti

t

Stratosphere

StratopauseMiddleAtmosphere

0

25

TroposphereTropopause

Atmospheric Structure

1 keV electron

125Thermosphere 1 MeV proton

10 keV electron

100

m)

MesosphereMesopause

10 MeV proton100 keV electron

75

tude

(km Mesosphere p

Middl

1 MeV electron

25

50

Alti

t

Stratosphere

Stratopause100 MeV protonMiddleAtmosphere

Bremsstrahlungpenetrate further

0

25

TroposphereTropopause

Atmospheric Structure

Atmospheric Influences ofAtmospheric Influences ofEnergetic Particle Precipitation

M t (70 80%) f th E D it dMost (70-80%) of the Energy Deposited creates Ion Pairs:

free Electron & positive Ion

Energetic Particle Precipitation

Medium & High Energy Electrons

Solar Protons

What are the dates of some large Solar Proton Events?Solar Proton Events?

Largest 15 Solar Proton Events (SPEs) in Past 50 YearsDate of Computed Rank Date of Computed Rank

SPEs (Total Ion Pair Production) October 1989 1

Note that seven

August 1972 2July 2000 3October 28-31, 2003 4

of the largest SPEsoccurred in 2000-2005!

November 5-7, 2001 5November 2000 6September 2001 7

Note that two

pAugust 1989 8November 23-25, 2001 9March 2012 10 Note that two

of the largest SPEsoccurred in 2012!

September 1966 11January 2012 12January 2005 13January 2005 13Sep. 29 – Oct. 3, 1989 14Jan. 28 – Feb. 1, 1967 15

Large SPE – GOES Proton Flux Data (March 6-11, 2012)

Note the large (>100X)

> 10 MeV104

-1 103

enhancement !

> 10 MeV

m-2

s-1sr

- 103

102

101

rtic

les c

m 10100

10-1

6 7 8 9 10 11 12Day in March 2012

Par

10-2

Day in March 2012

Ionization Rates (#cm-3 s-1) – March 6-11, 2012

500

Mesosphere

200

500

100 Stratosphere

Day in March

P t f 1 300 M V i l d d

Contour levels: 100, 200, 500, 1000, & 2000 (#cm-3 s-1)

Protons from 1-300 MeV included

Energetic Particles also ProduceEnergetic Particles also Produce HOx (H,OH,HO2) & NOx (N,NO,NO2)

Both of which can destroy Ozone

II EPP caused HO andII. EPP-caused HOx andOzone ChangeOzone Change

EPPs Enhance HO (H OH HO )HOx (H, OH, HO2)

• HOx constituents are produced through waterHOx constituents are produced through water cluster ion formation & neutralization– Primarily short-term effects as HOx lifetime is short

(~hours) in the atmosphere

HO d i b EPP b h h• HOx production by EPPs to be shown here:

– For Solar Proton Event in March 2012

– For Electron Precipitation in April 2006

Solar Proton HOx Production

Ionization RatesIonization Rates (top) &

HO Production

f

HOx Production Rates (bottom)

100200

500

for March 6-11, 2012 Day in March 2012

Contour levels: 100, 200, 500, 1000,

2000 & 5000 (#cm-3 s-1)200

500

2000, & 5000 (#cm s ) 100

Aura MLS(Microwave Limb Sounder)(M c o a e b Sou de )

measures HO2 and Ozone

MLS and 2D Model HO2 Polar NH (60-82.5o)March 6-11, 2012

HO2(ppbv) change for 60-82.5oN Latitude Band

HO2 average for0.5Feb.14-Mar.5 (3 weeks)

is subtractedfrom Mar. 6-11 values

0.10.2

from Mar. 6 11 values

Top: MLS DataDay in March 2012Day in March 2012

Bottom: ComputedHO P d tiHOx Production

100

200500

100

Ozone ImpactOzone Impact– March 2012 SPE

Aura MLS observations

MLS and 2D Model Ozone Polar NH (60-82.5o)March 6-11, 2012 Ozone(%) change for 60-82.5oN Latitude BandOzone & HO2 change for 60-82.5oN Lat. Band

Average forFeb 14 Mar 5 (3 weeks)-20

-40-60

Feb.14-Mar.5 (3 weeks) is subtracted

from Mar. 6-11 values-10

20

Day in March 2012Top: MLS Ozone Data

2D ModelDay in March 2012

Bottom: 0.5

MLS HO2 Data0.1

0.2

Day in March 2012

OH ProductionOH Production– Precipitating Electrons in April 2006

Aura MLS - OH observations

Adapted from Verronen et al. [2011]

OH J 15 (b f SPE)

Aura MLS OH Measurements (71-78 km) vs.Medium Energy Electron Flux (100-300 keV)

1610

5OH on Jan. 15 (before SPE)

C C f 0 93

for geomagnetic latitudes 55-65oN

12

14

m-3

] x

1

April 2006i d

Corr. Coef. = 0.93

Larger OH correlated withHigher Electron Flux

10

12

atio

n [c

m periodHigher Electron Flux

8

once

ntra

Adapted from

4

6

OH

co Verronen et al. [2011]

10-1

Electron Count Rate (s-1)100 101 102 103 104

III. EPP-caused NOx , NOy, and Ozone Change

EPPs EnhanceNO (N NO NO )NOx (N, NO, NO2)

• NO constituents are produced by primary electrons• NOx constituents are produced by primary electrons and protons and associated secondary electrons dissociating N2g 2– Short- and long-term effects as NOx constituents can last

for weeks

• SCISAT-1 ACE (Atmospheric Chemistry Experiment) NO (NO NO ) tit tmeasures NOx (NO+NO2) constituents

Adapted from Randall et al. [2006]

NOx in the Northern Hemisphere (50-85oN) Use ACE – started Feb. 18, 2004

1000 No Measurements

2004January February March

10Stratopause 100

January February March

Year 2004:– Significant EPP (electrons) in 2004

Al U l M l– Also, Unusual Meteorology- Sudden Stratospheric Warming (SSW) in January- Enhanced descent


NOx in the Northern Hemisphere (50-85oN) Use ACE – started Feb. 18, 2004

1000 No Measurements


10100Stratopause 100

January February March

Downward transport of NOxfrom the Mesosphere to the Upper Stratosphere

Year 2004:– Significant EPP (electrons) in 2004

Al U l M l– Also, Unusual Meteorology- Sudden Stratospheric Warming (SSW) in January- Enhanced descent


NOx descent in Northern Hem. Use ACE (50-85oN)

2004 1000

Years 2004, 2006, 2009:

2004 10100

1000

Stratopause– Unusual Meteorology descent

10

1000

100Stratopause

200610

1000

Stratopause

200910100

1000

Stratopause2009

January February MarchAdapted from Randall et al. [2009]

NOx descent in Northern Hem. Use ACE (50-85oN)Also, note that:

Years 2005, 2007, 2008, 2010, & 2011 2004 1000

, , , ,did not show enhanced descent

Years 2004, 2006, 2009:

2004 10100

1000

100Stratopause– Unusual Meteorology descent

10

1000

100100Stratopause

200610

1000

Stratopause

However: Yrs 2006 and 2009 did t h h

200910100

1000

100Stratopause

did not show much NOx descent to stratosphere



Now back to Year 2004:

How did the electron-produced NOximpact Ozone?impact Ozone?

Use data from POAM (Polar Ozone and Aerosol Measurement) instrumentsand Aerosol Measurement) instruments

Adapted from Randall et al. (2005)

POAM II & IIIobs (54-71oN)obs. (54-71 N)

NO2 at 40 km2

Ozone at 40 km

Column Ozone(35 50 km)(35-50 km)

-1.5 to 3 D.U. (~0.5-1%)


( 0.5 1%)

POAM II & IIIobs (54-71oN)obs. (54-71 N)

NO2 at 40 km2

Year 2004 appears to be very Ozone at 40 kmexceptional for EPP (electron)

NO transport to the StratosphereColumn Ozone

(35 50 km)

NOx transport to the Stratosphere

(35-50 km)-1.5 to 3 D.U.

(~0.5-1%)


( 0.5 1%)

Does the electron-caused Ozone change impact Climate?

Stay tuned for Annika Seppälä’sTalkfor Annika Seppälä sTalk

at 16:30 Todayat 16:30 Today for more information

Date of Computed Rank

Largest 15 Solar Proton Events (SPEs) in Past 50 YearsDate of Computed Rank

SPEs (Total Ion Pair Production) October 1989 1August 1972 2July 2000 3October 28-31, 2003 4

“Halloween” SPEof Oct. 2003

November 5-7, 2001 5November 2000 6September 2001 7

of Oct. 2003 was Very Large

pAugust 1989 8November 23-25, 2001 9March 2012 10September 1966 11January 2012 12January 2005 13January 2005 13Sep. 29 – Oct. 3, 1989 14Jan. 28 – Feb. 1, 1967 15

In memory of:ESA Envisat

(1 March 2002 8 April 2012)(1 March, 2002 – 8 April, 2012) Over 10 years of Earth observations

MIPAS, SCIAMACHY, & GOMOS Instruments provided greatInstruments provided great

measurements of EPP impact th At hon the Atmosphere

MIPAS provided measurements ofpmost NOy constituents:

NO, NO2, N2O5, HNO3 , HO2NO2, ClONO2

Only missing N, NO3, BrONO2, which are minuscule in the middle atmospherewhich are minuscule in the middle atmosphere.

NOy lifetime can be long (~months) NOy lifetime can be long ( months)

MIPAS NOy (NO+NO2+2N2O5+HNO3+ClONO2+HNO4)observations (40-90oN) in 2003( )

0.1

Changes with respect to October 26 20031 to October 26, 20031

10

Adapted from Funke et al. (2011)

Model

• Whole Atmosphere Community Climate Model p y(WACCM) – NCAR Model

- Domain [90oS – 90oN, 0 - 145 km] Ground to

Lower Thermosphere!

- Atmospheric physics & photochemistry - Specified dynamics from measurements for 2003

• Perturbed: Simulation ‘With’ SPEs

D. Marsh et al.

NOy (40-90oN) in 2003MIPAS WACCM

0.1 0.1

1 1

Changes with respect

1 1

10 10

g pto October 26, 2003

Adapted from Funke et al. (2011)

More WACCM Simulations

• Perturbed (1963-2004): Four realizations ‘With’ SPEs

Interactive dynamics

Perturbed (1963 2004): Four realizations With SPEs

• Base (1963-2004): Four realizations ‘Without’ SPEs

• Difference mean of Perturbed and Base results to compute SPE-caused change

Look at Averagegfor Years 2000-2004

Perturbed – Base (2000-2004 average)

50

100

-5

-2

10

20

50

5

10-2

5

2

Very Large SPEs in 2000, 2001, & 2003From Jackman et al. (2009)


C l d R iFrom Jackman et al. (2009)

Colored Regions are Statistically Significant to 95% (Student’s t-test)


Large stratospheric areawith statistically significant

Some stratospheric areawith statistically significantwith statistically significant

NOy increasewith statistically significant Ozone decrease (mainly NH)

Ozone decreaseOzone decrease more NOy-induced O3 loss

Ozoneiincrease

Interference of NOy with Cl/Br O3 loss

C l d R iFrom Jackman et al. (2009)

Colored Regions are Statistically Significant to 95% (Student’s t-test)

Do Solar Proton Events impact Total Ozone?impact Total Ozone?

Predicted Impact (GSFC 2D Model) of Solar Protons on Total Ozone (%)of Solar Protons on Total Ozone (%)

% Ozone-1

0 2-0.5

-0.1-0.20 5

% Ozonechange

-0.2

-0.5 -1

0 10 1

-0.2-0.2

-0.2

-0.5-0.5-1-3

-0.1-0.1

-0.1-0.1-0.2

-0.1-0.1-0.1-0.1 -0.1 -0.2

-0.2-0.2

0 5 0 5

-1 -1-1

-0.1

-0.1 -0.2-0.2-0.5 -0.5

-0.2

From Jackman et al. (2008)


% Ozone-1

0 2-0.5

-0.1-0.20 5

% Ozonechange

-0.2

-0.5 -1

0 10 1

-0.2-0.2

-0.2

-0.5

Larger decreases in NH caused by1989, 2001, & 2003 SPEs

-0.5-1-3

-0.1-0.1

-0.1-0.1-0.2

-0.1-0.1-0.1-0.1 -0.1 -0.2

-0.2-0.2

0 5 0 5Larger decreases in SH caused by

1972 1989 & 2000 SPEs

-1 -1-1

-0.1

-0.1 -0.2-0.2-0.5 -0.5

-0.2

1972, 1989, & 2000 SPEs



% Ozone-1

0 2-0.5

-0.1-0.20 5

% Ozonechange

-0.2

-0.5 -1

0 10 1

-0.2-0.2

-0.2

-0.5

Larger decreases in NH caused by1989, 2001, & 2003 SPEs

Computed Total Ozone decreasesfrom SPEs are <3% -0.5

-1-3

-0.1-0.1

-0.1-0.1-0.2from SPEs are <3%.

These can be compared -0.1-0.1-0.1

-0.1 -0.1 -0.2-0.2-0.2

0 5 0 5Larger decreases in SH caused by

1972 1989 & 2000 SPEs

with measured interannual variability of up to ~10%, thus are not observable

-1 -1-1

-0.1

-0.1 -0.2-0.2-0.5 -0.5

-0.2

1972, 1989, & 2000 SPEso up to 0%, t us a e ot obse ab e


IV. Conclusions• Both electrons & protons influence the polar

mesosphere/stratosphere – mainly in certain years e.g., near solar max, large Ap, unusual meteorology

• EPP produces HO which is short-livedEPP produces HOx, which is short lived Mesospheric Ozone depletion can be large (>20%)

• EPP produces long-lived NOy (1972,’89, 2000, ‘01, ‘03,’04, ‘06?)

Stratospheric Ozone impacts can last for months Computed total ozone changes are small (<3%)

Addendum:Addendum:EPP also impacts other constituents (e g HNO N O HO NO N O ClONO(e.g., HNO3,N2O5,HO2NO2,N2O,ClONO2,

ClO,HOCl,HCl,CO,H2O2) & T

Th k f tt ti !Thank you for your attention!

overview of energgp()etic particle precipitation (epp ... of energgp()etic particle precipitation...

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