Impact of Solar X-ray Flares on the Earth lower ionosphere

relating LYRA – GOES - VLF data

Vida Žigman, UNG, Nova Gorica,SloveniaDavorka Grubor, UB, Belgrade, Serbia

Desanka Šulić, IP, Belgrade, SerbiaCraig Rodger, James Brundell, Department of Physics,

University of Otago, Dunedin, New ZealandMark Clilverd, British Antarctic Survey, Cambridge,UK

ESWW9 / PROBA2 splinter

JOINT WORKING GROUP

GOES

SDO

In Space:

Observe and

measure

Flares!

LYRA?

SOHO

OBSERVATIONS

• Observations of the effects of Solar X-ray flares from Earth –VLF transmission

• How we correlate with space based measurements – GOES

• How we model: N(t,h), LWPM• Can we exploit LYRA data? • Results• Summary

OUTLINE

74 km

On Earth:

D-region

Radiowavepropagation(Supported by NOSC LWPC)

Tx:NWC

Rx:AbsPAL,AwesomeBeograd

Solar Lyman Alpha (121.6 nm)during flares: Solar X-rays measure

AMPLITUDE& PHASE

DISTURBANCESVLF

f < 30 kHz

OBSERVATIONS:

Radiowave propagation

TRANSMITTER Tx:Harold E. HoltNorth West CapeNWC (21.S ;114.2 E)

RECEIVERs Rx:Beograd (44.85 N; 20.38 E)

AbsPAL

AWESOME

View from ArcticNAA/24.0 kHz

Antarctic-ArcticRadiation-belt Dynamic) Deposition –VLF Atmospheric Research Konsortia

e.g.Tx: :NAA/24.0 kHz :(44.65 N; 67.3 W)

GQD/22.1 kHz :(54.72 N; 02.88 W) ICV/20.3 kHz:(40.92 N;9.73W)NWC/19.8 kHz:(21.8S; 114.2 E)

BGAbsPAL

Rx:

Scott

Gde je NPM?

Casey Scott B.

NWC/19.8 kHz

SCIENCE TOPICS

• SPE• REP• SOLAR FLARES

NPM/21.4 kHz

00:00 04:00 08:00 12:00 16:00 20:00 24:00

1E-6

1E-5

1E-4

-68

-66

-64

-62

-60

-58

-100

0

100

200

10-3

time UT

0200 UTC4.7

I x [w

/m-2]

0353 M6.3

0.1-0.8 nm GOES15_20120309

0128 UTC2

NWC20120309_Casey_1min

ampl

itude

[dB

]

0350.5 UT0350.5 UT

NWC - Casey : VLF Amplitude & Phase

I [W

/m2 ]

0357 UT 6-20 nm + X ray

1E-6

1E-5

1E-4

1E-3

-96

-90

-84

-78

-72

-66

00:00 04:00 08:00 12:00 16:00 20:00 24:00

10-3

-450

0

450

0348 UT

I [w

/m-2]

I x

[w/m

-2]

0353 UTM6.3

0.1-0.8 nm GOES15_20120309VLF NPM20120309_Casey

ampl

itude

[dB

]

0357 UT ch2-4(Zr); 6-20 nm + X ray

time UT

NPM - Casey : VLF Amplitude & Phase

pha

se [d

eg]

0349 UT

OBSERVATIONS

NPM/21.4 kHz

VLF: AMPLITUDEPHASEat

CASEY

Flare – active 9March 2012

Solar Irradiance

GOES 15 LYRA

NWC/19.8 kHz

Maine NAA/24.0 kHz at BELGRADE Flare – active 17July 2004

-1 5 0-1 0 0

-5 00

5 01 0 0

4 04 55 05 56 06 5

1 0 -71 0 -6

1 x 1 0 -51 x 1 0 -4

NAA/24.0 kHz

phas

e (d

eg)

t ime UT

1 7 0 7 20 0 4

1 7 0 7 20 0 4

1 9 5 016 5 01 3 5 01 0 5 0

NAA/24.0 kHz

ampl

itude

(r

elat

ive

dB)

0 7 50

GO ES-120.1-0.8 nm

I (W

/m2 )

1 7 0 7 20 0 4

X1.1 0757 UT 110µW/m2

C7.3 1137 UT 7.3µW/m2

M2.5 1651 UT 25.4µW/m2

dB5min3

=∆=∆

At

M2.5

dB3min2

=∆=∆

At

C7.3

56

58

60

62

64

1639 1659 1719 1739 1759

10-6

1x10-5

50

100

150

200GOES-12 0.1-0.8 nm

1654 UT

1651 UT

ampl

itude

(re

lativ

e d

B)

17072004

NAA/24.0 kHz

I (W

/m2 )

time UT

phas

e (d

eg)

LWPC model

For quiet ionosphereInitial concentration N(t=0, h)

Wait model of the quiet ionosphere (1970)

-sharpness, H’ – reflection heightβ

NOSC: Computer programme for the assessment of long wave Propagation Long Wavelength Propagation Capability,

Input :Tx and Rx coordinates Time Angle of magnetic inclination Conductivity

For solar-flare conditions:N(h),

To validate the N(t,h) model

β H’

Output :VLF amplitude and phase along the trace, from Tx to Rx

0 2000 4000 6000 8000 10000 1200030

60

90

120

am

plitu

de [d

B]

D [km] along GCP

LWPC quiet

NPM-Cas 07/03/12; LWPC for X1.4 at 01:15 UT

-400

-200

0

200

400

pha

se [d

eg]

NPM-Cas 07/03/12; LWPC for X1.4 at 01:15 UT

0 2000 4000 6000 8000 10000 12000

D [km] along GCP

NAA/24.0 kHz 17July 2004, 1651 UT

OBSERVATIONS - MODELLING:

Time delay (Appleton,1953, Journal of Atm. Terrestrial Physics JATP, 3, 282) “slugishness”(time shift of maximum N with respect to regular diurnal fluxat χ=0)

Amax , Imax ,, I(Amax) , A(Imax)

maxmax IAttt −=∆

KEY parameters:MEASUREMENTS:2004 -2007…2010...2012I(t), A(t), P(t)

maxmax NAtt ≡

)()( maxmax N IA I ≡

Assumption:

56

58

60

62

64

1639 1659 1719 1739 1759

10-6

1x10-51654 UT

1651 UT

ampl

itude

[dB

]

17072004 NAA/24 [kHz]

I X x

106

[W/m

2 ]

time UT

t∆ > 0A∆ > 0A∆ < 0

300 , 250 events

Multicomponent hydrodynamics N,N+,N-

q = (C/eH )I

q( t ) = k I (t)

q - rate of electron productionC –number of electrons per unit of energyH - scale height– solar zenith angle e –base of natural logarithm

?,αk

2Nqdt

dN α−=

χcos

χcoseH

Ck ≡

( )λλα

λ +−−

+=

1

1

)1(2

dt

dNN

q

dt

dN

Continuity equationelementary process kinetics

- effective electron recombination coefficient

MODELLING:

time dependence!

11.4 11.5 11.6 11.7 11.8 11.9 12

1× 109

2× 109

3× 109

4× 109

5× 109

6× 109

7× 109

Time UT

I (t)

from NOAAwww.sec.noaa.gov

From LWPC or IRI:preflare N(t=0)

α

χ

Why not LYRA?

Time delay , but for the active ionosphere:

tIN

∆=

α21

)( max ),,,( maxmaxmax IktNN α∆= (1)

α)(

)( maxmaxNkI

N DE =2Nqdt

dN α−= (2)

Agreement of (1) i (2) yields:

.constk =αq( t ) = k I (t), χcos

eH

Ck ≡

5× 1012

1× 1013

1.5× 1013

2× 1013

5× 10-13

1× 10-12

1.5× 10-12

2× 10-12

0

1

2

3

4

5

5× 1012

1× 1013

1.5× 1013

5× 101× 10-12

1.5× 10-12

2× 10

1/Jm][k

min][t∆

]sm[ -13α

5× 10121× 1013

1.5× 1013

2× 1013

5× 10-13

1× 10-12

1.5× 10-12

2× 10-12

0

1

2

3

4

5

5× 101× 10-12

1.5× 10-12

2×

0

1

2

3

4

]sm[ -13α1/Jm][k

min][t∆

0 5× 1012 1× 1013 1.5× 1013 2× 10130

5× 10-13

1× 10-12

1.5× 10-12

2× 10-12

.constk =αFriedrich et al. 1999, Adv. Space Res. Osepian et al. 2009 ,

Ann.Geophys

RECENT advances - extension to different heights

170704_1137 C7.3

e.g.

min)',( tt ∆∆(2, 1.92)

= 8.75 10-13 m3 s-1

q(t) = 3.73 1012 I(t) [m-3 s-1]

11.4 11.5 11.6 11.7 11.8 11.9 12

1× 109

2× 109

3× 109

4× 109

5× 109

6× 109

7× 109

Time UT

N [m

-3],

I x

1015

[Wm

-2]

17072004_1137 C7.3

Nmax= 5.23 109 m-3

N(Imax)= 4.86 109 m-3Height: 74km,

N(t=0):2.18 x 108 m-3

RESULTS

NAA/24.0 KHz

Žigman et al., 2007, Grubor et al., 2008,Journal of Atm. Solar-Terrestrial Physics Ann. Geophys

α

60 65 70 75 80 85 90

108

109

1010

1011

1012

X3.9X1.1M2.5M1.6C8.8C2.5M1.0X1.4

Nm

ax [m

-3]

height [km]

C2.5_70705_1228 ibid, Osepian et al. r.c. C8.8_50510_1152 M1.0_180211_1408 M1.6_160505_908 M2.5_60706_836 X1.1_170704_757 X3.9_170105_952 X1.4_70312_115 LWPM

Nmax height profile from N(t,h): t∆ from X flux 0.1-0.8 nm

How to apply the N(t,h) model to Lyra data ?

Ohshio M, et al. 1966Height distribution of local ionization efficiency,Journal of the Radio Research Laboratories, 13, no 70, 245- 261

Local ionization efficiencies ?

How they change with:

•Wavelength

•Height

from: J.K.Hargreaves,1992, The solar-terrestrial environment

Production rate / irradiance for vertical incidenceat 90 km for 6-20 nm

1210≅k [mJ]

-112

-104

-96

-88

-80

-72

-450

0

450

00:00 04:00 08:00 12:00 16:00 20:00 24:00

10-6

1x10-5

1x10-4

10-3

10-2

10-3

10-20118 UT

0020 UT

0115 UTX1.4

ch2-4(Zr); 6-20 nm + X ray

I [W

/m2 ]

VLF NPM20120307_Casey

ampl

itude

[dB

]

0028 UT p

hase

[deg

]

time UT

0.1-0.8 nm GOES15_20120307

0024 UTX5.4

Ix [

W/m

2 ]

data missing

data missing

2012_03_07

time UT1.2 1.4 1.6 1.8

2× 1011

4× 1011

6× 1011

8× 1011

-120

-100

-80

-600

0

600

00:00 02:00

10-6

1x10-5

1x10-4

10-3

10-2

10-3

10-2

0117.5 UT

0020 UT

0115 UTX1.4

ch2-4(Zr); 6-20 nm + X ray

I [W

/m2 ]

VLF NPM20120307_Casey

ampl

itude

[dB

]

0028 UT p

hase

[deg

]

time UT

0.1-0.8 nm GOES15_20120307

0024 UTX5.4

I x [W

/m2 ]

2012_03_07_0115_X1.4 H=90 km : I(t), N(t) GOES - LYRA

GOES LYRA

Nmax [m-3]: AMP 8.30 ×1011 7.66 × 1011

t(Imax ) UT 0115 0115

(∆t ∆t ′) [min] (2.5, 2.52) (2.5, 2.36)

Nmax [m-3]: PHA 8.82 × 1011

N(t) according to LYRA decreases slower than N(t) according to GOES

N [m-3], I x 1015 [Wm-2]

I x 1014 [Wm-2]

Nmax [m-3]: LWPM 1.13 × 1012

1E-6

1E-5

1E-4

1E-3

-96

-90

-84

-78

-72

-66

00:00 04:00 08:00 12:00 16:00 20:00 24:00

10-3

-450

0

450

0348 UT

I [w

/m-2]

I x

[w/m

-2]

0353 UTM6.3

0.1-0.8 nm GOES15_20120309VLF NPM20120309_Casey

ampl

itude

[dB

]

0357 UT ch2-4(Zr); 6-20 nm + X ray

time UT

pha

se [d

eg]

0349 UT

2012_03_09

5 10 15 20

0.00001

0.00002

0.00003

0.00004

0.00005

0.00006

1.8 1.9 2 2.1 2.2 2.3

1× 10-6

2× 10-6

3× 10-6

4× 10-6

5 10 15 20

0.0015

0.002

0.0025

0.003

0.0035

0.004

1.8 1.9 2 2.1 2.2 2.3 2.4

0.0002

0.0004

0.0006

0.0008

0.001

LYRA ch(2- 4) 6 - 20 nm +XrayLyra peaks at 0201 UT

Irr [W/m2] on 2012_03_09GOES15 0.1- 0.8 nm; 0200 UT_C4.7

Time UT Time UT

1.8 1.9 2 2.1 2.2 2.3

2× 1010

4× 1010

6× 1010

8× 1010

GOES15 LYRA

2012_03_09_0200_C4.7 H=90 km : I(t), N(t)

I scaled 1014I scaled 2 x 1016

1.9 2 2.1 2.2 2.3 2.4

1.2× 1011

1.4× 1011

1.6× 1011

1.8× 1011

2× 1011

Nmax [m-3]: 4.22×1010 1.17× 1011

t(Imax ) UT 0200 0201

t(Nmax ) UT (ev) 2.079 2.08

(∆t ∆t ′) [min] (4.5, 4.6) (3.5, 3.8)

Ns according to both GOES and LYRA peak simultaneously

Time UT Time UT

N [m-3], N [m-3],

Nmax [m-3]: LWPM 3.92 ×1010

X-ray flare ionization is efficient in the range 60-90km, more efficient than any other radiation in the lower D-region.

At the D-region upper limit Ly-Alpha and EUV are mo re efficient.

The diagnostics by Lyra time delay is more approp riate for the D-region upper limit, and is expected to give more realistic N estimates.

Apparently there is no reason to retrieve N from GO ES at 90 km height.But GOES time delay will give more realistic values of N for 74 km height and below.

VLF data A and P give N ( 60- 90 km) independetly o f the particular radiation. A na P bear the integral signature of th e event.

REMARKS

To estimate D- region electron density enhancements during Solar X-ray flares, as diagnostic tools use:

For the lower D-region limit and its vicinity - GOES X-ray data

For the upper D-region limit - LYRA data

For the whole D-region - VLF data

Summary

Thanks to

Proba2 Science Centre

LYRA team Ingolf Dammasch

Antarctica logistic providers