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ESWW10 / PROBA2 splinter. Modelling f lare induced ionization enhancements of the lower ionosphere with LYRA data relating Space LYRA – Earth VLF data. Vida Žigman , UNG, Nova Gorica,Slovenia. Guest Investigator Program Fourth Call:Sep 2013- Jun 2014. Davorka Grubor, UB, Belgrade, Serbia - PowerPoint PPT Presentation
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Vida Žigman, UNG, Nova Gorica,Slovenia
ESWW10 Antwerp, 18-22 November 2013
Modelling flare induced ionization enhancements of the lower ionosphere with
LYRA data relating Space LYRA – Earth VLF data
Guest Investigator ProgramFourth Call:Sep 2013- Jun 2014
ESWW10 / PROBA2 splinter
Davorka Grubor, UB, Belgrade, Serbia Craig Rodger, Department of Physics, University of
Otago, Dunedin, New ZealandMark Clilverd, British Antarctic Survey, Cambridge,UK
UnderstandImpact of Flares!On the Lower Ionosphere 50-100 km height
• Observations of the effects of Solar X-ray flares from Earth – VLF transmission
• Correlation: VLF data - space based measurements
• Can we exploit LYRA data? • How to combine data and model:
N(t,h), LWPM• (some) RESULTS – 90 km height
• Prospects
OUTLINE Objectives:
DATA:
LYRA ch2-4(Zr); 6 – 20 nm+X-ray(< 2 nm)
(SWAP ?)
GOES 12-15 ( 0.1-0.8 nm ) Flare classification
SPACE : Solar irradiance
GOES
2011_02_28_M1.1
Dammasch et al. 2012COSPAR
Dominique et al. 2013 Solar Physics, DOI: 10.1007.
The LYRA Instrument Onboard PROBA2: Description and In-Flight Performance
Characteristics of the Lyra Irradiance:
•Lyra peaks after GOES •Lyra descends slower than GOES
LYRA - 4 years in orbit
LG
DATA:
EARTH : VLF data - AMPLITUDE & PHASE on different sunlit paths from receivers Rx
• Belgrade IP VLF Observatory – Belgrade University • Casey and Scott Base stations, Antarctica –
Otago University, Dunedin NZ
BAS, Cambridge, UK
raypath
trace
great circle
EARTH
reflection pointD region
Earth-ionosphere
waveguide
T (transmitter)
R (receiver)
Radiowave propagation (Supported by NOSC LWPC)
Solar Lyman Alpha (121.6 nm)
during flares: Solar X-rays
emitVLF
f < 30 kHz
Transmitter:NWC/19.8 kHz
Receiver:Belgrade AbsPAL
On Earth:
D-region
measureAMPLITUDE
& PHASEDISTURBANCES
2011_02_18 NWC - Bgd
06:00 07:00 08:00 09:00 10:00 11:00
10-5
10-4
10-3
1E-8
1E-7
1E-6
1E-5
1E-4
1E-3
I X
[W
/m2 ]
Lyr
a I[
W/m
2 ]
time UT
NWC-Bgd 20110218
40
50
60
70
ampl
itude
[dB
]
0
350
700
phas
e [d
eg]
M6.6C4.2C8.5 C7.6
OBSERVATIONS:
All data in
1 min cadence
NWC – Bgd
11974 km
q( t ) = k I (t)
2Nqdt
dN
1
1
)1(2
dt
dNN
q
dt
dN
MODELLING:
time dependence!
-50
-40
00:00 04:48
10-6
1x10-5
1x10-4
10-3
10-2
0
10-3
10-2
I X [W
/m2 ]
I [W
/m2 ]
NPM20120307_SCOTT BASE
0028 UTLYRA ch2-4(Zr); 6-20 nm + X ray
GOES15 0.1-0.8 nm
0024 UT_X5.4
time UT
01:15.478 UT; 1.37E-4
Irradiance I (t) 2012_03_07
FROM LYRA!
From Goes
)()( maxmax ItNttttmaxmax IPA,
AMP & PHA Time delay!
4.0x10-4
8.0x10-4
1.2x10-3
1.6x10-3
2.0x10-3
20:40 20:50 21:00 21:10 21:20 21:30 21:4010-7
10-6
1x10-5
1x10-4
0
100
200
300
400
500
2057_M1.5
I L (
W/m
2 )ph
ase
(d
eg
)
-44
-42
-40
-38
-36
-34
am
plit
ud
e (
dB
)
time UT
I x (W
/m2 )
NPM_SB_20131028_2057_M1.5
10 10.1 10.2 10.3
1 1011
2 1011
3 1011
4 1011
5 1011
6 1011
7 1011
N [
m-3],
I X
x 1
016 ,
I L x
1014
[W
m-2]
Time UT
Electron density at 90 km height from AMPLITUDE time delay
)',( AA tt 4.14 1011 GOES (2, 1.92)1.74 1011 LYRA (1, 0.79)
Nmax [m-3]
LYRA Imax 1012 UT , 3.35 mW/m2
min1LG
[min]
NWC- Bgd 20110218_1011_M6.6
10:00
10-5
10-4
10-3
1E-8
1E-7
1E-6
1E-5
1E-4
1E-3
I X
[W
/m2 ]
Lyr
a I[
W/m
2 ]
time UT
NWC-Bgd 20110218
40
50
60
70
ampl
itude
[dB
]
0
400
phas
e [d
eg]
1013
2013_05_13 NPM – Scott BaseOBSERVATIONS:
00:00 04:00 08:00 12:00 16:00 20:00 24:00
10-4
10-3
10-2
1E-6
1E-5
1E-4
C8.3X1.7
2205 UT
X2.8C9.3
( Ix
GO
ES W
/m2 )
2207 UT
2209 UT
(Ix
Lyr
a W
/m2 )
LYRA_ 20130513
time UT
2207 UT
-75
-70
-65
-60
-55
-50
-45
-40
-35
-30
-25
-20
-15
ampl
itude
(dB
)
NPM-SB 20130513-1200
-800
-400
0
400
800
phas
e (d
eg)
(M1.3)
Lll
L
Scott
Gde je NPM?
Casey Scott B.
NWC/19.8 kHz
NPM/21.4 kHz
NPM- Scott Base
11260 km
-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
10-2
0118 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
[de
g]
time UT
0.1-0.8 nm GOES15_20120307
0024 UTX5.4
Ix
[W/m
2 ]
data missing
data missing
2012_03_07_ NPM-Casey
-70
-60
-50
-40
00:00 04:00 08:00 12:00 16:00 20:00 24:00
10-6
1x10-5
1x10-4
10-3
10-2
-2000
-1000
0
10-4
10-3
10-2
10-1
I X [
W/m
2 ]
I [W
/m2 ]
NPM20120307_SCOTT BASE
Tx out of order
0.1-0.8 nm GOES15_20120307 0024_X5.4
time UT
PH
A [
deg]
AM
P [
dBm
]
01:15.478 UT; 1.37E-4
00:11.496 UT 00:19.5 UT01:15.498 UT
data missing
2012_03_07_ NPM-Scott Base
1.2 1.4 1.6 1.8
2 1011
4 1011
6 1011
8 1011
1 1012
N [
m-3],
I X
x 1
015 ,
I L x
1014
[W
m-2]
Time UT
-100
-80
-600
0
600
00:00 04:48
10-6
1x10-5
1x10-4
10-3
10-2
10-3
10-2
0115 UT
0118 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
pha
se [
deg]
time UT
GOES15 0.1-0.8 nm
0024 UTX5.4 I
x [W
/m2 ]
-50
-40
00:00 04:48
10-6
1x10-5
1x10-4
10-3
10-2
0
10-3
10-2
I X [
W/m
2 ]
I [W
/m2 ]
NPM20120307_SCOTT BASE
0028 UTLYRA ch2-4(Zr); 6-20 nm + X ray
GOES15 0.1-0.8 nm
0024 UT_X5.4
time UT
PH
A [
deg]
AM
P [
dBm
]
20120307_0115_ NPM-Casey X1.4 NPM_Scott Base - - - - - - - - - - - -
)5.3,5.2(
min),( PA tt
maxN
(7.4 1011, 1012) m-3
Overall: at 90 km
LG0
10-4
10-3
00:00 04:00 08:00 12:00 16:00 20:00 24:0010-9
10-8
10-7
10-6
1x10-5
1x10-4
M4
.4M
2.7
M2
.8
M1.4C5.2M5.1X1.02057_M1.5
I (W
/m2 )
day
NPM-SB 20131028
time UT
Ix (
W/m
2 )
-60
-45
-30a
mp
litu
de
(d
B)
-600
-400
-200
0
200
400
ph
ase
(d
eg
)
2013_10_28_ NPM-Scott Base
20.9 21 21.1 21.2 21.3
2.5 1010
5 1010
7.5 1010
1 1011
1.25 1011
1.5 1011
1.75 1011
N [
m-3],
I X
x 1
016 ,
I L x
1014
[W
m-2]
Time UT
NPM-Scott Base 20131028_2057_M1.5Electron density at 90 km height from AMPLITUDE & PHASE time delay
7.36 1010 GOES (2.5, 2.32)3.89 1010 LYRA (0.5, 0.52)
AMP
9.76 1010 GOES (3.5, 3.30)1.05 1011 LYRA (1.5, 1.58)
PHA
min2LG
LYRA Imax 2059 UT , 1.78 mW/m2
Nmax [m-3] )',( tt [min]
4.0x10-4
8.0x10-4
1.2x10-3
1.6x10-3
2.0x10-3
20:40 20:50 21:00 21:10 21:20 21:30 21:4010-7
10-6
1x10-5
1x10-4
0
100
200
300
400
500
2057_M1.5
I L (
W/m
2 )ph
ase
(d
eg
)
-44
-42
-40
-38
-36
-34
am
plit
ud
e (
dB
)
time UT
I x (W
/m2 )
Summary • LYRA data can be used to assess the flare enhanced electron density at the ceiling of the D-region - 90 km.
Nmax, N(t) • N(t) according to LYRA decreases slower than according to
GOES.• The predictions of the maximal flare induced electron density at 90 km height are in reasonabe agreement.
M1.5 M6.6 X1.4 Nmax [m.3] (7.4 1010, 1011) 2 - 4 1011 (7.5 1011, 1012)
Prospects: • Can the lower ionization efficiency be compensated by higher irradiance ?
• Assessment with Long Wavelength Propagation Capability LWPC (NOSC)
Thanks to
Proba2 Science Centre D. Berghmans
M. Dominique LYRA Team M. West
NOAA/SWPC
Antarctica logistic providers
The Audience !
ESWW10 Antwerp, 18-22 November 2013
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