terrestrial gamma-ray flashes (tgfs) observed with fermi-gbm
DESCRIPTION
Terrestrial Gamma-Ray Flashes (TGFs) Observed with Fermi-GBM G. J. Fishman 1 , M. S. Briggs 2 , and V. Connaughton 2 for the GBM TGF Team 1 NASA-Marshall Space Flight Center Huntsville, AL USA 2 Univ. Alabama in Huntsville Huntsville, AL USA - PowerPoint PPT PresentationTRANSCRIPT
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Terrestrial Gamma-Ray Flashes (TGFs) Observed with Fermi-GBM
G. J. Fishman1, M. S. Briggs2, and V. Connaughton2
-for the GBM TGF Team
1NASA-Marshall Space Flight CenterHuntsville, AL USA
2Univ. Alabama in HuntsvilleHuntsville, AL USA
Thunderstorms and Elementary Particle Acceleration (TEPA 2010)
Nor Amberd, Armenia6-11 September 2010
( -for TEPA Web site posting)
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TGFs - Overview & Some New Results
History; Spacecraft observations
Observations from Fermi-GBM
Future Space Missions
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Observations of TGFs with
Four Spacecraft:
I. BATSE /Compton Observatory: 1991-2000
II. Solar Spectroscopic Imager
III. AGILE Gamma-ray Telescope
IV. Gamma-ray Burst Monitor (GBM) on the Fermi
Gamma-ray Space Telescope (this talk)
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I. Burst and Transient Source Experiment (BATSE) - Compton Observatory (CGRO) 1991-2000
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BATSE TGFs:
Determined rough spectral properties (extremely energetic) Associated with thunderstorms Observed 78 in 9 years
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TGFs from BATSE (showing saturation at ~300,000 cps)
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II. RHESSI (Ramaty High-Energy Solar Spectroscopic Imager)
- Solar Observatory
- Launched 2002; currently operational
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Time Profiles of some RHESSI TGFs:
RHESSI Observations of TGFs: Doesn’t require trigger; all data are transmitted
Detected many more TGFs than BATSE, but they were much weaker
Determined very hard spectra (> 20 MeV)
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SAA Region
Hi Bkgnd - Low Sensitivity Region
High Background, Low Sensitivity Region
Map of RHESSI TGFs (820 events)
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GLOBAL FLASH RATE – ANNUAL (from LIS-TRMM data)H. Christian et al.
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Large CsI Scintillator
Can Detect TGFs
III. AGILE - Italian Gamma-ray Astronomy Satellite
- 100kg Experiment
- Launched: April 2007
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Launched June 11, 2008
NASA Kennedy Space CenterFermi
Gamma-Ray Space Telescope
IV. GBM(Gamma-ray Burst Monitor)
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GBMDetector Locations on the
Fermi Spacecraft – Launched June 2008
BGO Det.
(1 of 2)NaI Det.
(3 of 12)
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GBM (Gamma-ray Burst Monitor)
on the Fermi Observatory - Launched June 11, 2008- Primary Objective: GRBs
FermiGamma-Ray
Space Telescope
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Gamma-Ray Burst Monitor (GBM) Sodium Iodide (NaI) Detectors (12)
1.27 cm thick 12.7 cm dia.
8 keV to 1 MeV
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GBM Bismuth Germinate (BGO) Detectors (2)
12.7 cm thick 12.7 cm dia.
150 keV to 45 MeV
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Gam
ma-
ray
Ener
gy C
han.
(~1
MeV
max
.)
milliseconds (rel. to trigger time)
TGFNaI Detectors (all 12 combined)
“Overflow” Chan. (127)
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0
20
40
60
80
100
120
140
-12 -11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0
0
20
40
60
80
100
120
140
-11 -10 -9 -8 -7
7
1
45
40
20
7
5.5
4.2
2.0
1.3
0.3
45
40
20
7
5.5
4.2
2.0
1.3
0.3
MeV
Spectral Differences
TGF #1:
Low energies dominate
TGF #7:
High energies dominate
MeV
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6 of the fastest TGFs
Risetimes & Falltimes ~7 μs to 15 μs
(4 μs per bin)
(400 μs , total span}
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Narrowest Pulse seen with GBM, ~ 50 μs
Two Well-separated, Double-Pulse TGFs seen with GBM (all detectors summed)
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Fermi – GBMLocations of 85 TGFs
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TGF & Lightning are usually Simultaneous
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How simultaneous?
Distribution of GBM TGF peaks - WWLLN sferic peaks.
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2 Exceptions:
Of 15 associated sferics (5 ms, 300 km), 2 are not consistent with being simultaneous with the TGF pulse
Difference: ~few ms.
Lightning sfericLightning sfericTGF TGF
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TGF & Lightning - Summary
• Simultaneous, no preferred order
• GBM detects gamma-ray TGFs within 300 km of sub-spacecraft.
• We need other VLF data to explore shape, size of sferics (Duke, Stanford, LASA groups).
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Triggered TGF Rate in GBM: ~1/mo., prior to 11 Nov. 2010
~8/mo., after “ “
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Median TGF Pulse Duration = 0.11ms
- Does not include 5 longer “electron” TGFs
- Solid column – includes 10 possible un-resolved pulses
Pulse Durations of First 50 GBM TGFs
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Electron TGFs: No Storm in Region Below Spacecraft
Below Spacecraft
Geomagnetic Conjugate Region
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Five “Electron” TGFs (in the first 50)
Characteristics: Longer than usual
Fast rise, then decaying
Some are not over thunderstorms
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31
Long “Electron” TGF
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August 2010 – Implemented “un-triggered” TGF capability
Over selected “America’s Region”:
- RHESSI TGFs
- RHESSI TGFs, May-November
est.: ~several TGFs per day in this Reion
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First look at a GBM an Un-triggered TGF
Binned Data 20μs/bin
TGF Full-Width: ~0.25ms Total cts above bkgnd: ~35 cts Peak ct. rate: ~20kcps (Spectrum appears similar to strong TGFs)
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TGFs –
Major Observational Questions:
Altitude of origin?
Extent & volume of the emitting region?
Beaming properties of the emission?
What is the intensity distribution of TGFs ? Are TGFs related to Gigantic Blue Jets ?
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Plot by M. Briggs
TGF #5 , Individual Detectors, 0.1ms binsN
aI (
12)
B
GO
(2)
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NaI
(12
)
BGO
(2)
TGF #1 , Individual Detectors, 0.1ms bins
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Time Profiles – All Detectors Combined
Energies of Single Counts -BGO Detectors Only
Properties of 10 Short TGF Pulses
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Four Longer TGF Pulses (~1-3 ms)
Time Profiles – All Detectors Combined
Energies of Single Counts -BGO Detectors Only
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Overlapping Double Pulses
- 3 in the first 50 TGFs
(~7 others are less obvious)
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Overlapping Double Pulses
- 3 in the first 50 TGFs
(~7 others are less obvious)
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NaI
(12
)
BGO
(2)
TGF #1 , Individual Detectors, 0.1ms bins
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Plot by M. Briggs
TGF #5 , Individual Detectors, 0.1ms binsN
aI (
12)
B
GO
(2)
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Fermi – GBMLocations of 85 TGFs
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GBM TGF Papers - 2010➡ “First Results on Terrestrial Gamma-ray Flashes from the Fermi Gamma-ray Burst Monitor”, M. S. Briggs, et al., JGR
➡ “Associations between Fermi GBM Terrestrial Gamma-ray Flashes and sferics from the WWLLN”, V. Connaughton, et al., in press, JGR
➡ “Temporal Properties of Terrestrial Gamma-ray Flashes from the Gamma-ray Burst Monitor on the Fermi Observatory”, G. J. Fishman, submitted to JGR
➡ “Positrons observed from Terrestrial Lightning with Fermi GBM”, M. S. Briggs, et al., in preparation
Complete list of Huntsville Gamma-Ray Team Publications: http://gammaray.nsstc.nasa.gov/publications/tgf_journal.html
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TGF Simulation - Courtesy J. Dwyer, Florida Tech.Gamma-rays (red); Electrons (blue)
200
150
100
50
20
Altit
ude
(km
)
-200 -100 0 100 200
Horizontal Distance (km)
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Future Spacecraft to Study TGFs:
Firefly – NSF cubesat; GSFC; Siena College
ASIM – on ISS; ESA, led by Danish
TIRANIS – French & others
CHIBIS-M – Russian (IKI) & others
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End