Stanford VLF Remote Sensingsolar-center.stanford.edu/SID/AWESOME/Goddard.pdf · Science,...
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Stanford VLF Remote Sensing Science, Engineering, Educational outreach Morris Cohen Along with Phil Scherrer, Deborah Scherrer, Umran Inan, Ray Mitchell, Justin Tan Space, Telecommunications and Radioscience Laboratory Stanford University Stanford, California 94305 http://www-star.stanford.edu/~vlf/ http://sun.stanford.edu
Transcript of Stanford VLF Remote Sensingsolar-center.stanford.edu/SID/AWESOME/Goddard.pdf · Science,...
Stanford VLF Remote SensingScience, Engineering, Educational outreach
Morris CohenAlong with Phil Scherrer, Deborah Scherrer, Umran Inan,
Ray Mitchell, Justin Tan
Space, Telecommunications and Radioscience Laboratory
Stanford UniversityStanford, California 94305
http://www-star.stanford.edu/~vlf/http://sun.stanford.edu
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Stanford VLF Remote Sensing
� The collaborators
� Ionosphere/magnetosphere overview
� Electromagnetic effects
� SID Receiver
� AWESOME Receiver
� Educational Outreach
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The Stanford Collaborators
� Phil/Deborah Scherrer
� Ray Mitchell
� Umran Inan
� Morris Cohen
� Justin Tan
� Center for Integrated Space Weather Modeling (CISM)
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The Ionosphere
Source: HAARP
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The Magnetosphere
Source: NASA, Rice University
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Electromagnetic Effects
� Solar Flare Detection
� Cosmic Gamma Rays
� Chorus Emissions
� Lightning
� Whistler waves
� LEP Events, hurricane studies
� Early/fast Events
� Mesospheric lightning discharges� Sprites, elves, blue jets, TGFs
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Sudden Ionospheric Disturbance
� Strong solar flares penetrate to lower ionospheric region, cause transient changes
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VLF Transmitters
Source: Great Circle Mapper, Karl Swartz
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SID Event – an Example
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2.5
3
3.5
4
4.5
5
07:0
0:0
3
07:3
1:2
6
08:0
2:4
8
08:3
4:1
1
09:0
5:3
4
09:3
6:5
6
10:0
8:1
9
10:3
9:4
2
11:1
1:0
5
11:4
2:2
7
12:1
3:5
0
12:4
5:1
3
13:1
6:3
5
13:4
7:5
8
14:1
9:2
1
14:5
0:4
4
15:2
2:0
6
15:5
3:2
9
16:2
4:5
2
16:5
6:1
4
17:2
7:3
7
17:5
9:0
0
18:3
0:2
3
19:0
1:4
5
19:3
3:0
8
20:0
4:3
1
20:3
5:5
3
21:0
7:1
6
21:3
8:3
9
22:1
0:0
1
22:4
1:2
4
23:1
2:4
7
23:4
4:1
0
00:1
5:3
2
00:4
6:5
5
01:1
8:1
8
01:4
9:4
0
02:2
1:0
3
02:5
2:2
6
03:2
3:4
9
03:5
5:1
1
04:2
6:3
4
04:5
7:5
7
05:2
9:1
9
06:0
0:4
2
06:3
2:0
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Local Nighttime DaytimeSunrise Local Nighttime
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0.5
1
1.5
2
2.5
3
07:0
0:0
3
07:3
5:3
1
08:1
0:5
9
08:4
6:2
7
09:2
1:5
6
09:5
7:2
4
10:3
2:5
2
11:0
8:2
0
11:4
3:4
8
12:1
9:1
6
12:5
4:4
4
13:3
0:1
2
14:0
5:4
0
14:4
1:0
8
15:1
6:3
6
15:5
2:0
4
16:2
7:3
2
17:0
3:0
0
17:3
8:2
8
18:1
3:5
6
18:4
9:2
4
19:2
4:5
3
20:0
0:2
1
20:3
5:4
9
21:1
1:1
7
21:4
6:4
5
22:2
2:1
3
22:5
7:4
1
23:3
3:0
9
00:0
8:3
7
00:4
4:0
5
01:1
9:3
3
01:5
5:0
1
02:3
0:2
9
03:0
5:5
7
03:4
1:2
5
04:1
6:5
3
04:5
2:2
1
05:2
7:5
0
06:0
3:1
8
06:3
8:4
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Quiet
Day
Active
Day
NLK
24.8 kHz
Source: Ray Mitchell
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SID Event – an Example
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2.5
3
3.5
4
4.5
5
07:0
0:0
3
07:3
1:2
6
08:0
2:4
8
08:3
4:1
1
09:0
5:3
4
09:3
6:5
6
10:0
8:1
9
10:3
9:4
2
11:1
1:0
5
11:4
2:2
7
12:1
3:5
0
12:4
5:1
3
13:1
6:3
5
13:4
7:5
8
14:1
9:2
1
14:5
0:4
4
15:2
2:0
6
15:5
3:2
9
16:2
4:5
2
16:5
6:1
4
17:2
7:3
7
17:5
9:0
0
18:3
0:2
3
19:0
1:4
5
19:3
3:0
8
20:0
4:3
1
20:3
5:5
3
21:0
7:1
6
21:3
8:3
9
22:1
0:0
1
22:4
1:2
4
23:1
2:4
7
23:4
4:1
0
00:1
5:3
2
00:4
6:5
5
01:1
8:1
8
01:4
9:4
0
02:2
1:0
3
02:5
2:2
6
03:2
3:4
9
03:5
5:1
1
04:2
6:3
4
04:5
7:5
7
05:2
9:1
9
06:0
0:4
2
06:3
2:0
5
Local Nighttime DaytimeSunrise Local Nighttime
GOES
Data
Active
Day
NLK
24.8 kHz
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Cosmic Gamma Rays
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Chorus Emissions
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Lightning Detection
EW
NSIncident wave S
Φ
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Whistlers in the Magnetosphere
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Whistler Wave – an Example
Sferics
Whistler
Triggered
emissions
Palmer Station, Antarctica 2 March 1992 0839:06 UT
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Lightning Induced Electron Precipitation (LEP Events)
Source: Bill Peter
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LEP Events – an Example
Hurricane
Isabel
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Early Fast Events
Source: Bill Peter
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Mesospheric Phenomenon
Source: Nikolai Lehtinen
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Runaway Electrons
Source: Nikolai Lehtinen
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Sprites and Early/Fast Events
Early fast events are highly correlated with
sprites, indicating connection with ionospheric
heating and runaway electronsSource: Robert Marshall
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TGFs and Sferics
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The Hardware
� SID Detector
� AWESOME Receiver
A tmosphericW eatherE ducationalS ystem forO bservation andM odeling ofE ffects
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The SID Detector
� Designed by Ray Mitchell
� Low cost, compact, easy to use
� Narrowband amplitude receiver
� 1 sample per 5 seconds
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The SID Detector – Overview
Pre-Amp
24.8KHzFilter
SignalStrength
DATAQComputer
RS-232
Coax
=
All frequencies
DC voltageLevel
10 bit, Analog to DigitalConversion Sample every
5 Seconds
Source: Ray Mitchell
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SID Detector - Pictures
Pre-Amp DataQPost-Amp
Wire Loop Antenna
Source: Ray Mitchell
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The AWESOME Receiver
� Designed by Morris Cohen, Justin Tan
� Ultra sensitive
� Medium cost (~$2000)
� Narrowband amplitude/phase
� Broadband 100kHz data
� Deployed worldwide
� Auto-calibration
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AWESOME Receiver – Overview
B-Field Antenna
PreampLong Cable
Line Receiver
Analog to Digital
ComputerGPS
Antenna
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AWESOME Receiver – Pictures
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AWESOME Receiver – Data
Data taken from Palmer Station, Antarctica
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More Data, Calibration
Data taken from Homer, Alaska
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Educational Outreach
� Center for Integrated Space Weather Modeling (CISM)� Run by Boston University
� Stanford selected for educational outreach
� Distribute SID detectors widely� 3 Beta sites working
� 100 units in production
� 3 foreign sites planned (Tanzania, India, Tibet)
� Distribute selected AWESOME detectors
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Educational Outreach (con’t)
� Research purpose� data sent to Stanford via internet, DVDs
� Educational purposes� Monitor solar flares/VLF activity� Build antenna, maintain electronics� Participate in research campaigns
� Promote in developing countries through UN?
� http://solar-center.stanford.edu/~SID� http://www-star.stanford.edu/~hail/
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nQ e it ou s s
