NOAA Observations of Solar Irradiance - |LASP|CU...
Transcript of NOAA Observations of Solar Irradiance - |LASP|CU...
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14 Sept 2005 SORCE Meeting 1
NOAA Observations of SolarIrradiance
Rodney ViereckNOAA SEC
A presentation of the past, present, and futureobservations of solar irradiance made by NOAA
GOES XRS GOES 8-12 XRSX-Ray
EUV
UV
UVVISIR
Total1970 1980 1990 2000 2010 2020 . . . . . .
Year
GOES NOP XRS
GOES NOP EUVS
POES (and NIMBUS) SBUV POES SBUV NPOESS OMPS and SIM
NPOESS SIM
NPOESS TIM
Spec
tral B
and
GOES
NOAA POES
NPOESS
GOES R+ XRS
GOES R+ EUVS
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14 Sept 2005 SORCE Meeting 2
0.1 1.0 10010 1000 10000Wavelength (nm)
Sola
r Irr
adia
nce
0.1
10
1000
105
Solar Variability(m
ax min)/m
in
IRVISUVEUVX-RAY
GOES XRS
GOES SXI (Imager)
GOES EUV*
POESSBUV
NPOESS(SIM)*
NPOESS(TIM)*
Overview of NOAA Solar Observations:Spectral Coverage
NOAA is monitoring, or plans to monitor, much of the solarspectrum.
Solar Spectrum
Solar Variability
* Planned for future NOAA satellites
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14 Sept 2005 SORCE Meeting 3
GOES X-Ray Sensor (XRS)
Operational Requirement(Space Weather)Detect onset of flareMeasure flare magnitude
Expanded Utility (SpaceClimate)Long-term measure of solar x-ray irradiance
Planed inclusion in theSolar2000 EUV irradiance andflare model (Tobiska andBouwer)
X-Ray Sensor IssuePresently adjusting irradianceto match earlier spacecraft
XRS Long * 0.7 XRS Short * 0.85
Very Large (X17) Flare of Last WeekHF Radio Wave Absorption
Impacted Location and Frequencies
Solar X-Ray Daily Background
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14 Sept 2005 SORCE Meeting 4
GOES R+ XRS
GOES XRS
Past Data is Available at the NOAA National Geophysical DataCenter http://spidr.ngdc.noaa.gov/spidr/
Presently, GOES 10 and 12 are operational, GOES 11 is stored on-orbit. GOES N will be launched in October 2005, GOES O and P are in final stages of assembly. GOES R is in initial planning stage
XRS will remain very similar into the foreseeable future
GOES NOP XRS
GOES
Sat
ellit
eSe
ries
1970 1980 1990 2000 2010 2020 . . . . . . Year
Toda
y
GOES 8-12 XRSEarly GOES XRS
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14 Sept 2005 SORCE Meeting 5
GOES EUV Irradiance(new for GOES NOP: Launch Oct. 2005)
0 10 20 30 40 50 60 70 80 90 100 110 120 130 140
1
10
100
1000
10000
100000
1000000
1E7
EUVEEUVD
EUVC
EUVB
EUVA
Inst
rum
ent R
espo
nse
Wavelength (nm)
-200
-180
-160
-140
-120
-100
-80
-60
-40
-20
0
20
40
60
80
100
120
Atmospheric Heating Rate Hea
ting
Rat
e(d
eg/h
r)
100
150
200
250
300
350
400
450
500
0 20 40 60 80 100 120
Energ
y D
eposi
tion (
W/m
3
)
1E-12
1.9E-12
3.8E-12
7.3E-12
1.4E-11
2.7E-11
5.3E-11
1E-10
2E-10
3.9E-10
7.5E-10
1.5E-9
2.8E-9
5.5E-9
1.1E-8
2.1E-8
4E-8
Alti
tud
e (
km)
Wavelength (nm)
Space WeatherRequirements driven by Ionospheric models
(Communications,Navigations)
Thermospheric models(Satellite drag)
Original GOES N EUVS Bands
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14 Sept 2005 SORCE Meeting 6
GOES R+Bands or Lines?
The next generationof GOES EUV sensorsis under development. What is the best
compromise between fullspectral coverage andcost?
Can we model the entirespectrum with just a fewspectral lines ratherthan bands?
TIMED SEE data showthat we can measure afew spectral lines andmodel the rest of theEUV spectrum
0 20 40 60 80 100 120
0.0
0.1
0.2
F10 + F10(81 day Avg)
Mg II + F10 + F10(81 day Avg)
Five Bands + Mg II + F10 + F10(81 day Avg)
Five Lines + Mg II + F10 + F10(81 day Avg)
Sta
ndard
Devia
tion
Wavelength (nm)
0 20 40 60 80 100 12010
-10
10-9
10-8
10-9
10-8
10-7
10-6
10-5
10-4
10-3
10-2
EUV-A EUV-B EUV-C EUV-D EUV-E
Wavelength (nm)
FeIX
/X
HeI
I
FeXV
IM
gIX
HI
TIMED SEE Solar Spectrum
GOES N EUVS Bands
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14 Sept 2005 SORCE Meeting 7
EUV Irradiance:Relevant to Climate Change Research?
Climate change in the upperatmosphere.
Upper atmosphere is a driven systeminternal variability is small compared tothe response to external forcing.
EUV variability and upper atmosphericresponse vary by factors of 10.
Upper atmospheric response toanthropogenic forcing is negative(cooling)
Upper atmospheric response toanthropogenic forcing is smallcompared to the response to solarforcing.
Removing the natural (solar) signal toobserve the secular or anthropogenicsignal requires very good solar data.
Solar MaxSolar Min
Keating380 km
Roble400 km
Marcos 400km
Akmaev200 km
Emmert530 km
NOV time = 19 UTC
1940 1950 1960 1970 1980 1990 2000
80
100
120
140
Kp
1940 1950 1960 1970 1980 1990 2000
1.5
2.0
2.5
3.0
3.5
foF2 - solar removed
1940 1950 1960 1970 1980 1990 2000
-15
-10
-5
0
5
10
foF2 in percent - solar removed
1940 1950 1960 1970 1980 1990 2000
-10
0
10
NOV time = 20 UTC
1940 1950 1960 1970 1980 1990 2000
80
100
120
140
Kp
1940 1950 1960 1970 1980 1990 2000
1.5
2.0
2.5
3.0
3.5
foF2 - solar removed
1940 1950 1960 1970 1980 1990 2000
-15
-10
-5
0
5
10
foF2 in percent - solar removed
1940 1950 1960 1970 1980 1990 2000
-15
-10
-5
0
5
10
15
NOV time = 21 UTC
1940 1950 1960 1970 1980 1990 2000
60
80
100
120
140
Kp
1940 1950 1960 1970 1980 1990 2000
1.5
2.0
2.5
3.0
3.5
foF2 - solar removed
1940 1950 1960 1970 1980 1990 2000
-10
-5
0
5
10
foF2 in percent - solar removed
1940 1950 1960 1970 1980 1990 2000
-10
-5
0
5
10
Trends in the Thermosphere
Trends in the IonosphereBoulder (Nov 1900UT)
From Akmaev (2005)
From Weatherhead (2004)
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14 Sept 2005 SORCE Meeting 8
SORCE XPS
GOES R+ EUVS
NOAA EUV Sensor
Starting in 2005 (or sometime after), NOAA will begincontinuous monitoring of solar EUV irradiance.
Planned GOES N Schedule: Launch October 2005 Post Launch Test To May 2006 On Orbit Storage ???? Begin Operations 2007, 2008, 2009, ???
1970 1980 1990 2000 2010 2020 . . . . . . Year
Toda
y
Sate
llite SOHO SEM
TIMED SEE
SDO EVE
GOES NOP EUVSAEROS
-A
AEROS-A
SM-5
AE-E
SOLRAD 11
EUV
Hole
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14 Sept 2005 SORCE Meeting 9
Solar UV Observationsfrom NOAA POES SBUV and SBUV2
(see publications and presentations by Matt DeLand)
The Solar Backscatter UltraVioletSensor (SBUV) Scanning monochrometer Nadir viewing (Designed to measure
ozone) Periodically (daily), a diffuser directs
sunlight into sensor Daily measurements
Continuous scan mode (170-405 nm, 1.1nm resolution)
Discrete mode, sampling 12wavelengths around the 280 nm Mg IIabsorption feature.
Primary solar product is the Mg IIcore-to-wing ratio a measure ofsolar chromospheric activity. Proxy for UV Proxy for EUV Proxy for Total Solar Irradiance
Models
Solar UV Spectrum from the SBUV
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14 Sept 2005 SORCE Meeting 10
Calculating the Mg II Core-to-Wing Ratio
277 278 279 280 281 282 283Wavelength (nm)
1.0E5
1.5E5
2.0E5
2.5E5
3.0E5
3.5E5
Rel
ativ
e In
ten s
i t y 791011 5 4 3 12612 8
(Allen et al., 1978)
SBUV Discrete Grating Steps
Wavelength (nm)
h (280.27 nm)
k (279.56 nm)
Rel
ativ
e In
tens
ity
SBUV Scan Data
The h and k Mg II emission lines (core)are highly variable while the adjacentsolar spectral features (wings) are morestable
Even though the SBUV does not resolvethe lines, the bottom of the spectralfeature is still more variable than thewings
The SBUV Mg II ratio is the ratio ofthe sum of the core values to the wingvalues
(6 + 7 + 8)(1 + 2 + 11 + 12)
Mg II = Core/Wings
=
12 11 10 9 8 7 6 5 4 3 2 1
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14 Sept 2005 SORCE Meeting 11
Mg II Observations:Creating a Composite Mg II Index
Rodney A. Viereck(1), Linton E. Floyd, L.(2), Patrick C. Crane(2), Thomas N. Woods(3), Barry G. Knapp(3), GaryRottman(3), Mark Weber(5), Lawrence C. Puga(1), Matthew T. DeLand(6)
In spite of large variations in the absolute values of the Mg II observations,the measurements are highly correlated. This allows simple linear scaling ofeach dataset to a common value.
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14 Sept 2005 SORCE Meeting 12
Cross Correlations Between Mg II Data Sets
Linear correlationsbetween UV sensorswith
differentresolutions
measuring atdifferent timesof the day
from differentsatellites.
Combining thesemeasurements into asingle time series isfairly straightforward.
0.260 0.265 0.270 0.275 0.280 0.285 0.290
0.260
0.265
0.270
0.275
0.280
0.285
0.290
0.295
0.260 0.265 0.270 0.275 0.280
0.260
0.265
0.270
0.275
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0.285
0.265 0.270 0.275 0.280 0.285 0.290
0.265
0.270
0.275
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0.285
0.290
0.255 0.260 0.265 0.270 0.275 0.280 0.285 0.290 0.295
0.255
0.260
0.265
0.270
0.275
0.280
0.285
0.290
0.295
NOAA9
N7N9
R = 0.99737
a
c
SUSIM
NOAA9
R = 0.99147
d
NOAA16
SUSIM
R = 0.99540
R = 0.99628
SUSIM
GOME
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14 Sept 2005 SORCE Meeting 13
UV Applications:Mg II Core-to-Wing Ratio
Mg II Index is a measure of solar chromospheric variability used as a proxy for EUV and UV variability and in models of TSI. one of the longest records of solar variability.
1978 1982 1986 1990 1994 1998 2002 2006
0.260
0.265
0.270
0.275
0.280
0.285
0.290
0.295
Mg II In
dex
Year
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14 Sept 2005 SORCE Meeting 14
NOAA SBUV Sensors
1970 1980 1990 2000 2010 2020 . . . . . . Year
NOAA 16 SBUV
Toda
yUARS SUSIM
UARS SOLSTICE
UMETSAT GOME
SORCE SOLSTICE
NOAA 17 SBUV
NOAA N SBUV
NOAA 18 SBUV
NPP OMPS
NPOESS OMPS and SIM
NIMBUS 7 SBUV
NOAA 9 SBUV
NOAA 11 SBUV
The present SBUV/2 instrumentsNOAA-14 Launched Dec 1994NOAA-16 Launched Sept 2000NOAA-17 Launched June 2004NOAA-18 Launched May 2005NOAA-N Launch-ready in 2008
The Future NOAA UV Solar ObservationsNPP OMPS Launch 2009NPOESS OMPS Launch 2011NPOESS SIM Launch 2013
Not measuring Mg II
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14 Sept 2005 SORCE Meeting 15
TSIS measures the solar input into the Earths energy balance -- a key factor inunderstanding the change in climate
NPOESS TSIS consists of
Two sensors:
Total Irradiance Monitor (TIM): Measures total solar irradiance
Spectral Irradiance Monitor (SIM): Measures spectral irradiance in the 200 to 2000 nm range
A Thermal Pointing System (TPS) that integrates thermal and mechanical designs forsun-staring and calibration, and includes
A Fine Sun Sensor (FSS)
Associated Electronic Modules
TIM and SIM are based on heritage SORCE (Solar Radiation and ClimateExperiment)
TSIS is procured from the University of Colorado, Laboratory for Atmosphericand Space Physics (CU LASP)
TSIS will be located on 1730 satellite aft nadir deck and will be launched firston NPOESS C3 (2013?) and later on NPOESS C6 (2018??)
Total and Spectral Irradiance onNPOESS TSIS
(National Polar orbiting Operational Environmental Satellite System Total and Spectral Irradiance Sensor)
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14 Sept 2005 SORCE Meeting 16
NPOESS TSIS
SpectralIrradianceMonitor (SIM)
TotalIrradianceMonitor (TIM)
Electronics Modules
PointingPlatform
SupportStructure
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14 Sept 2005 SORCE Meeting 17
NPOESS C6 TIM
NPOESS C6 SIM
NPOESS C3 TIM
NOAA Total and Spectral Irradiance Sensors
Total Irradiance and Spectral Irradiance Requirement for long-term solar irradiance trends and information Long accurate records require instrument-to-instrument overlap
Gaps in record create much larger uncertainties in the trends Gap in SIM data seems inevitable unless SORCE lasts for a long long time Gap in TIM will not occur if all sensors operate longer than planned and
launches are not delayed (lots of ifs)
2002 2004 2006 2008 2010 2012 2014 2016 2018 2020 2022 Year
GLORY TIM
NPOESS C3 SIM
Toda
y
SIM Data Gap
SORCE TIM
SORCE SIM
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14 Sept 2005 SORCE Meeting 18
Summary
NOAA has been monitoring the x-ray irradiance for more than 20years
NOAA has been monitoring the UV solar irradiance for more than20 years
NOAA will begin to monitor the EUV solar irradiance in a few weeks
NOAA will monitor total and spectral solar irradiance on NPOESSsome time in the future (2013?)
Total Solar Irradiance (TIM)
Spectral Irradiance (SIM) of the UV, Visible, and IR wavelengths
All of these observations will continue into the foreseeable future.