HF Propagation and Eclipse 2017
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1 HF Propagation and Eclipse 2017 Dr. Rob Suggs KB5EZ Huntsville Amateur Radio Club Meeting 20 Oct
2 Fundamentals Shake an electron and you get electromagnetic waves Expose an electron to electromagnetic waves and it shakes, making more waves Called a Hertzian dipole Solar UV and X-rays knock electrons off the neutral atoms and molecules Free electrons in the ionosphere get shaken by your RF and emit some more RF The density of the electrons, the density of neutrals around them, and the magnetic field all affect the way they move and emit RF KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 2
3 The sun is the driver of ionospheric density It follows an 11 year cycle, on average KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 3
4 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 4
5 Forecast based on historical observations, not physics KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 5
6 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 6
7 Ionosphere and HF propagation VHF/UHF 20m 80m D layer causes absorption of lower bands F layer causes skip wiki.robotz.com KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 7
8 UV Ionizes the F layer X-rays ionize the D layer F10.7 or SFI 2800 MHz solar radio noise. Correlated With EUV KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 8
9 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 9
10 The eclipse turned off the sun for a time KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 10
11 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 11 DSCOVR
12 KB5EZ October Huntsville Amateur Radio Club Meeting 12 ISS
13 Ionosphere Response to Eclipse IRTAM model f o F2 critical frequency of the F2 layer (nf2 ~ f o F2 2 ) KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 13
14 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 14 Solar Dynamics Observatory
15 WSJT-X WSPR Mode KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 15
16 WSPR ops for Eclipse m NN4SA Tx 40m KB5EZ Tx 30m KB5EZ Rx 20m KB5EZ Rx MSFC ARC MSFC Lunar Obs. QTH Madison, AL QTH Madison, AL FT-950 FT-897 FTDX-3000 Ten Tec Rebel Dipole Portable dipole Dipole MA5B small beam 1662 spots, 47 calls 5247 spots, 52 calls 5644 spots, 195 calls 5449 spots, 347 calls KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 16
17 WSPR transmission and spot structure In a 2 minute cycle, you transmit callsign, grid square, and transmit power in dbm (db relative to a milliwatt) KB5EZ EM watts (5000 mw) Power Dist Hdg Spot # Unix Time Rx grid SNR freq Tx grid dbm drft km deg Band s/w ver error , ,KB5EZ,EM64pr,-17, ,N8LI, FN41fl,37,-1,1521,245,14,1.8.0-rc1, , ,KB5EZ,EM64pr,-20, , W5EK, EM10ci,37, 0,1146, 62,14,1.8.0-rc1, , ,KB5EZ,EM64pr, -1, ,K1EHZ, FN42ex,37,-4,1592,240,14,1.8.0-rc1, , ,KB5EZ,EM64pr,-24, , K5XL, EM12kp,33, 0, 991, 74,14,1.8.0-rc1, , ,KB5EZ,EM64pr,-26, ,KB5FIO,EM10cg,23, 0,1151, 62,14,1.8.0-rc1,0 22 million spots from 1 August to 23 August KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 17
18 WSPR Propagation Plot 80m band (3.5 MHz) KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 18
19 VOACAP Software 80m 21 August 2017 KB5EZ to K9AN KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 19
20 80m 40m 30m 20m 20
21 WSPR Signal to Noise Ratio vs Time 80m Range Heading Illinois Grid Start End Day after KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 21
22 WSPR Signal to Noise Ratio vs Time 80m Reduced D-layer attenuation (from X-rays) at mid-eclipse, stronger signal KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 22
23 WSPR SNR vs Time 7.0MHz Signal is attenuated due to F layer Reduction at higher frequency KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 23
24 30m Attenuation due to F layer reduction KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 24
25 20m KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 25
26 Summary Solar activity affects the ionosphere which affects HF propagation The 2017 total solar eclipse provided an excellent laboratory for investigating these effects It appears that electron density reduction in the D layer allowed better propagation at 80m It appears that electron density reduction in the F layer caused slightly worse propagation at 40, 30, and 20m This is only for WSPR data where my station was at one end, conclusive results will be from ALL of the data KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 26
27 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 27
28 eol.jsc.nasa.gov/video/crewearthobservationsvideos/ ISS Expedition 31 May 22, 2012 KB5EZ October 2017 Huntsville Amateur Radio Club Meeting 28
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