ABCDx: Miscellaneous Notes

Revised: 03-March-2007

Contents:

1. Propagation Notes

2. Antenna Notes


1. Propagation Notes

- Ap Example

If the 8 daily recorded 3-hour a-values for an observatory are (7, 7, 15, 15, 15, 15, 48, 48) then the 24-hour average for that observatory would be (7+7+15+15+15+15+48+48)/8 = 21.25, which is rounded off to the nearest whole-number, or 21. This would be the reported "A" value for the observatory. Once all of the "A" values from the other observation sites are accumulated, then an over-all average is determined and reported as the Planetary-A (Ap) for the day.

- Geomagnetic Storms

Disturbances to the Earth's magnetic field caused when electrons and protons ejected by solar eruptions bombard the Earth and interact with the field. The scale below, abstracted from the NOAA Space Weather website (www.sec.noaa.gov/NOAAscales/index.html#GeomagneticStorms) is used when alerts are issued along with the regular reports of the solar indices. Note the correspondence to the K-index and the expected frequency of occurrence per 11-year solar cycle.

Scale/Descriptor
Kp value
Frequency
Effects upon HF propagation & Aurora
G 5: Extreme
Kp = 9
4 per cycle
HF disruptions 1-2 days; aurora as low as FL & So.Tx
G 4: Severe
Kp = 8
100 per cycle
HF sporadic, aurora as low as AL, So.CA
G 3: Strong
Kp = 7
200 per cycle
HF radio intermittent, aurora as low as IL & OR
G 2: Moderate
Kp = 6
600 per cycle
HF fade at high US latitudes, aurora as low as NY, ID
G 1: Minor
Kp = 5
1700 per cycle
Little-no HF influence; aurora at highest US latitudes (No. MI , ME)

Reference: NOAA Space Weather Scales (www.sec.noaa.gov/NOAAscales/)

**************
- Maximum Usable Frequency (MUF) vs. Ion Region Height

This discussion is from the Propagation column in the March, 1997 issue of WorldRadio magazine by Carl Luetzelschwab, K9LA, in which he analyzed a few of the issues related to MUF by using spherical geometry rather than the usual depictions seen using "flat Earth" Cartesian geometry. Below is the author's rendering of the illustration and table that was used in the column, along with a few of the details.

For ion-region height "H", radiation angle "a", and incident angle "b", the arc of the skip distance D/2 is equal to the product of the radius and the subtended angle "c" in radians:

D/2 = R*c/(180/pi), so that D = (2R/57.3)c

Since the angles a, b, c of the triangle must add to 180, we then have

D = (2R/57.3)*(90 - a - b)

By the Law of Sines,

R/sin(b) = (r + H)/sin(90 + a)

so

b=arcsin {[(R/(R + H))]*sin(90+a)}

and we finally have

D = (2R/57.3)*arcsin {[(R/(R + H))]*sin(90+a)}

The diameter of the Earth at various latitudes may be approximated by the average of the polar and equatorial diameters [Polar diameter ~ 7,900 mi (12,720 km); Equatorial diameter ~ 7,926 mi (12,760 km)], or R = 6370 Km. Below are the results of some calculations using an Excel macro to replicate the Table 1 of the WR column. Note from the figure that as the radiation angle increases, the signal ray incident angle, b, decreases, and so the angle (90 - b) increases.

H
a
b
90-b
D
M-
(Km)
(Deg)
(Deg)
(Deg)
(Km)
Factor
100
0
79.9
10.1
2241
5.7
100
5
78.8
11.2
1388
5.1
100
10
75.8
14.2
925
4.1
100
25
63.2
26.8
407
2.2
100
50
39.3
50.7
164
1.3
200
0
75.8
14.2
3150
4.1
200
5
75.0
15
2225
3.9
200
10
72.7
17.3
1619
3.4
200
25
61.5
28.5
780
2.1
200
50
38.6
51.4
321
1.3
300
0
72.8
17.2
3834
3.4
300
5
72.1
17.9
2876
3.3
300
10
70.1
19.9
2192
2.9
300
25
59.9
30.1
1123
2.0
300
50
37.9
52.1
473
1.3
400
0
70.2
19.8
4400
3.0
400
5
69.6
20.4
3421
2.9
400
10
67.9
22.1
2686
2.7
400
25
58.5
31.5
1441
1.9
400
50
37.2
52.8
619
1.3
500
0
68.0
22
4889
2.7
500
5
67.5
22.5
3896
2.6
500
10
65.9
24.1
3125
2.4
500
25
57.2
32.8
1738
1.8
500
50
36.6
53.4
759
1.2

From the table, we can see immediately that as the ion-region height (H) increases, the skip does indeed increase, but the MUF decreases! The reason is clear from the data because as H increases, the incident angle decreases, bringing the ray closer to vertical incidence and therefore allowing less opportunity for the wave to be refracted, so that it exits into space unless the frequency is decreased (i.e., lower M-factor => lower MUF). Just another interesting aspect of radio wave propagation!

**************

- WWV Reports

Archives of the eight WWV SFI reports for each day may be seen at www.sec.noaa.gov/ftpmenu/forecasts/wwv.html.

Below is a summary of the reports for two days, reduced to the SFI, A, & K indices only, and arranged in row-order to better appreciate the change-over of the A-index at 2100UTC. Note the date change at 2100UTC and the estimated A-index at that time.

Issued: 2007 Jan 15 2222 UTC
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2. 0000 UTC mid-latitude  K on 15 Jan was 1
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2 0300 UTC mid-latitude  K on 15 Jan was 2
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2 0600 UTC mid-latitude  K on 15 Jan was 3
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2 0900 UTC mid-latitude  K on 15 Jan was 3
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2 1200 UTC mid-latitude  K on 15 Jan was 3 
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2 1500 UTC mid-latitude  K on 15 Jan was 6 
Indices: 14 Jan Solar flux 82; mid-latitude  A = 2 1800 UTC mid-latitude  K at 15 Jan was 4
Indices: 15 Jan Solar flux 82; estimated mid-lat  A = 21 2100 UTC mid-latitude  K on 15 Jan was 2
Issued: 2007 Jan 16 2122 UTC
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 0000 UTC mid-latitude  K on 16 Jan was 2
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 0300 UTC mid-latitude  K on 16 Jan was 0
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 0600 UTC mid-latitude  K on 16 Jan was 5
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 0900 UTC mid-latitude  K on 16 Jan was 2
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 1200 UTC mid-latitude  K on 16 Jan was 2
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 1500 UTC mid-latitude  K on 16 Jan was 2
Indices: 15 Jan Solar flux 82; mid-latitude  A = 21 1800 UTC mid-latitude  K on 16 Jan was 3
Indices: 16 Jan Solar flux 79; estimated mid-lat  A = 12 2100 UTC mid-latitude  K on 16 Jan was 2

Remember that the A-index is the 24 hour index derived from the average of the eight 3-hour K indices recorded at Boulder from 0000–2100UTC. From 0000–1800UTC, the reported A-index is for the previous 24-hours and does not change in the reports. For the 2100UTC report, the last of the day, an estimate of the A-index is used for the current day, based on the 7 measurements collected from 0000–1800UTC. At 0000 UTC, the solar flux and K-index for the next day are reported and the actual A-index is for the previous day, derived from all 8 measurements, is now shown, dropping the qualification of “estimated”.


2. Antenna Notes

- Understanding Elevation & Azimuthal Plots

Antenna modeling programs commonly produce output graphics and data showing the expected radiation pattern of the antenna in one of 3 viewing options: as a 3-dimensional figure; a vertical slice ("Elevation Plot") through the 3-D pattern; or a horizontal slice ("Azimuthal Plot") through the 3-D pattern. The elevation view tells us about the radiation angle and the azimuthal view is the one that we most often use for evaluating direction of radiation. Below are the Elevation and Azimuthal plots of a simple 20m 3-element Yagi antenna used for illustration. Elements are 1" OD untapered and lengths are: Reflector = 35.0 ft; Driven = 32.7 ft; Director = 30.0 ft. Boom length is 28 ft and modeling is done for the antenna at a height of 66 ft (one wavelength) above real ground.

The modeling software automatically labels the outer-most point of the radiation pattern maxima as "0 dB" because the intent of the plots on the circular graph is to show the pattern of energy distribution in comparison to the maximum. The modeling program has calculated the maximum gain over an isotropic radiator to be 13.02 dBi (10.7 dBd), so the outer ring of the plot is set to that value. We can then see from the two plots that there is quite a bit of interesting variation in the energy distribution as it radiates from the source. Note also that the scale of the rings is compressed as they get smaller, because decibels are logarithmic numbers that compress as they get larger or smaller.

Note from the data in the Elevation plot (left), that there are two major beam lobes emerging from the antenna, with a radiation maxima in the lower lobe at an angle of 14o. In addition to the angle of maximum radiation power emission, the "thickness" or "width" of the beam is also calculated between the two angles above and below 14o at which the power is reduced by half, that is, reduced by 3 dB. If we look at the -3 dB ring (inwards from the 0 dBi max), we see where the power is down by half from the maximum, indicated by the two purple lines at 7.0o and 15.3o. This is called the "Half-power Beamwidth", or just the "Beamwidth". It should be clear that antennas generally radiate energy in beams and not single rays; however, it is theoretically possible (and feasible at UHF and above) to design antennas that produce extremely narrow beamwidths. Additional information can be likewise determined for the other lobes.

Let's now look at the horizontal, or Azimuthal, radiation pattern, which can be viewed as a slice from any angle. Since for DX, we are interested in a low angle of radiation, for this antenna model we will use 14o above ground from which to view the azimuthal pattern. In the figure on the right, we see from the data that the horizontal forward gain at the chosen radiation angle (14o) is 13.02 dBi (10.7 dBd), as we already knew from the Elevation plot. In addition, the calculated data tells us that the antenna has a F/B of 18.64 dB, a figure that we can easily read from the plot, as diagrammed below.

Here is another look at the azimuthal view, labeled and annotated to explain the numbers in the figure. The modeling software automatically labels the outer-most point of the radiation pattern maxima as "0 dB" because the intent of the circular graph is to show the radiation energy distribution within 360o, relative to the maximum.

The azimuthal beamwidth is seen to be 65.0o (purple lines defining -3db points), a fairly wide "funnel". That's why exact "pointing" of your 20m beam is not extremely critical, as long as you are within a few degrees of the proper beamheading.

Why is a negative scale used? Remember that gain in dB is a logarithm of the power ratio, and that logarithms of fractions are negative numbers. Since any "gain" at a point inside of the outer-most circle will have to be less than the maximum, it will then be a fraction, hence negative. Even if the data were not printed out, we could, as illustrated above, get an estimate of the F/B ratio by reading the chart.

Another important point to remember is that these patterns from which we derive the antenna gain are viewed in the far-field, many wavelengths from the antenna. Note that the "gain" at the radiation source (antenna at the center of the pattern) is not a consideration and is shown to be essentially zero ( -50dB or less).

- Gain, F/B, & Bandwidth

To see how the forward gain and F/B ratio are related to frequency, here is a set of superimposed azimuthal plots of the above 3-el Yagi produced by having the modeling software sweep the frequency from 14.0 MHz - 14.4 MHz in 0.2 MHz steps:

We see that the forward gain is less affected by frequency change than is the F/B, which ranges from approximately 24 dB at 14.0 MHz (Blue-line), down to about 15 dB at 14.4 MHz (Black-line). Data figures are for the sweep end-frequency (Black-line patter @ 14.4 MHz).