Practical_Antenna_Handbook_0071639586

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C h a p t e r 2 : r a d i o - W a v e P r o p a g a t i o n 45 Ionospheric Propagation Following on the heels of seminal discoveries by Hertz, Marconi, and other pioneering radio scientists of the late 1800s, the early 1900s found experimenters from all walks of life constructing simple radio transmitting and receiving equipment. By 1909, radio clubs had been formed at a few colleges around the United States, and by 1914 the American Radio Relay League (ARRL), dedicated to these amateur experimenters, had been founded. Commercial, government, and amateur stations shared the airwaves in willy-nilly fashion until around 1912 when the United States began to regulate radio. In those days, “good DX” might mean the ability to communicate between, say, Boston and New York City, and the prevalent assumption was that the longer wavelengths were superior for extending those distances. Forced to shift from wavelengths as long as 1000 m (well below the bottom of today’s AM broadcast band) to 200 m (roughly around 1500 kHz, near the top of the AM broadcast band) by the new regulations, amateurs grumbled a bit but dug in and went back to figuring out how to attain better and better DX distances. As the distances increased, however, the experts were finding it harder and harder to explain how it was possible. World War I brought a halt to all amateur transmissions, and when the war was over the U.S. government was inclined to keep it that way forever. But the ARRL convinced Congress and various federal agencies of the merits of radio amateurs, and in the fall of 1919 amateurs returned to the airwaves. In 1921 and again in 1922, the ARRL sponsored transatlantic receiving tests, and in both events too many stations were heard for it to be a fluke: 30 or so the first year and 10 times that number the following year! Spurred on by these encouraging results, the ARRL and others began to investigate what it would take to convert these successes into two-way communication across the ocean. Despite the almost unanimous opinion of the best scientists of the day that the shorter wavelengths would prove to be useless, some hardy experimenters plunged below 200 m and, within a year, had shown that the shorter the wavelength, the better the DX results! Textbooks and magazines of the era were rife with theories to explain these totally unexpected results. Ultimately, the “correct” theory turned out to be one originally advanced in 1901, when Arthur Kennelly of the United States and Oliver Heaviside of England independently proposed the existence of a “reflecting” layer circling the earth some miles above it. Soon named the Kennelly-Heaviside layer, it is now known as the E layer (Fig. 2.26) of the ionosphere. Thus, it is the ionosphere that makes intercontinental radio communications possible on the MF, HF, and lower VHF bands (between roughly 0.3 and 70 MHz). Included in the range of frequencies for which ionospheric propagation is possible are the AM broadcast band, many traditional maritime frequencies, amateur bands from 160 to 6 m, and the first few channels (2, 3, and 4) of the analog broadcast television spectrum. True, in some cases (especially at the upper end of the range) “possible” does not mean “probable”, but the potential is there during sunspot maxima or during brief periods of unusual solar activity. The author recalls the winter of 1957–58, when he saw firsthand a neighboring amateur make two-way contact with six continents in one evening on the 6-m band (50 MHz), using a 5-W AM transceiver and a three-element 6-m beam dangling from the I-beam running through his basement! Kennelly and Heaviside described the unseen layer as a reflecting layer; in truth, the sparseness of the ionization and the variation of ionization with altitude make
46 p a r t I I : F u n d a m e n t a l s Figure 2.26 Classification of the earth’s atmosphere for radio propagation.
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Practical Antenna Handbook
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Practical Antenna Handbook Joseph J
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Contents Preface . . . . . . . . .
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C o n t e n t s vii 12 The Yagi-Uda
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C o n t e n t s ix Switched-Pattern
Page 12 and 13: Preface My paternal grandfather was
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Page 16 and 17: Acknowledgments As with other field
Page 18 and 19: Background and History Part I Chapt
Page 20 and 21: CHAPTER 1 Introduction to Radio Com
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Page 24 and 25: Fundamentals Part II Chapter 2 Radi
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C h a p t e r 3 : A n t e n n a B a
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CHAPTER 4 Transmission Lines and Im
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C h a p t e r 4 : T r a n s m i s s
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Chapter 5 Antenna Arrays and Array
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C h a p t e r 5 : a n t e n n a A r
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A. B. C. D. E. F. G. H. Figure 5.9
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B. C. D. E. F. G. H. Figure 5.10 Gr
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High-Frequency Building-Block Anten
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CHAPTER 6 Dipoles and Doublets A co
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C h a p t e r 6 : D i p o l e s a n
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CHAPTER 7 Large Wire Loop Antennas
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C h a p t e r 7 : L a r g e W i r e
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CHAPTER 8 Multiband and Tunable Wir
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C h a p t e r 8 : M u l t i b a n d
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CHAPTER 9 Vertically Polarized Ante
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C h a p t e r 9 : V e r t i c a l l
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Quarter-wave vertical radiator Insu
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Directional High-Frequency Antenna
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CHAPTER 10 Wire Arrays When a singl
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C h a p t e r 1 0 : W i r e A r r a
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Wire 2 C h a p t e r 1 0 : W i r e
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CHAPTER 11 Vertical Arrays Despite
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C h a p t e r 1 1 : V e r t i c a l
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CHAPTER 12 The Yagi-Uda Beam Antenn
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C h a p t e r 1 2 : T h e Y a g i -
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CHAPTER 13 Cubical Quads and Delta
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C h a p t e r 1 3 : C u b i c a l Q
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Figure 13.5 Multiband quad “spide
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High-Frequency Antennas for Special
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CHAPTER 14 Receiving Antennas for H
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C h a p t e r 1 4 : r e c e i v i n
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351 Figure 14.12 Remote tuning sche
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CHAPTER 15 Hidden and Limited-Space
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C h a p t e r 1 5 : H i d d e n a n
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CHAPTER 16 Mobile and Marine Antenn
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C h a p t e r 1 6 : M o b i l e a n
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CHAPTER 17 Emergency and Portable A
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C h a p t e r 1 7 : E m e r g e n c
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Antennas for Other Frequencies Part
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CHAPTER 18 Antennas for 160 Meters
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C h a p t e r 1 8 : a n t e n n a s
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CHAPTER 19 VHF and UHF Antennas The
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C h a p t e r 1 9 : V H F a n d U H
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CHAPTER 20 Microwave Waveguides and
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C h a p t e r 2 0 : M i c r o w a v
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λ o = c / f 8 3× 10 m / s = 9 C h
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CHAPTER 21 Antenna Noise Temperatur
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C h a p t e r 2 1 : A n t e n n a N
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C h a p t e r 2 1 : A n t e n n a N
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CHAPTER 22 Radio Astronomy Antennas
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C h a p t e r 2 2 : R a d i o A s t
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Figure 22.9 Interferometer pattern.
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CHAPTER 23 Radio Direction-Finding
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C h a p t e r 2 3 : R a d i o D i r
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Figure 23.9 Adcock array RDF antenn
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Figure 23.11 Watson-Watt Adcock arr
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Tuning, Troubleshooting, and Design
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CHAPTER 24 Antenna Tuners (ATUs) Th
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C h a p t e r 2 4 : a n t e n n a T
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CHAPTER 25 Antenna Modeling Softwar
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C h a p t e r 2 5 : A n t e n n a M
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Figure 25.3B Bent dipole wire and s
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CHAPTER 26 The Smith Chart The math
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Figure 26.2 Normalized impedance li
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A Figure 26.3 Constant resistance c
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A Figure 26.4A Constant inductive r
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C h a p t e r 2 6 : T h e S m i t h
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D C B A Figure 26.5 Radially scaled
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0.165 Y ' 1.0 j1.1 G' 1.0 Y ' 0.2
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CHAPTER 27 Testing and Troubleshoot
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C h a p t e r 2 7 : T e s t i n g a
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Mechanical Construction and Install
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CHAPTER 28 Supports for Wires and V
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C h a p t e r 2 8 : S u p p o r t s
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CHAPTER 29 Towers At some point, th
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CHAPTER 30 Grounding for Safety and
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C h a p t e r 3 0 : G r o u n d i n
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CHAPTER 31 Zoning, Restrictive Cove
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C h a p t e r 3 1 : Z o n i n g , R
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C h a p t e r 3 1 : Z o n i n g , R
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Appendices
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APPENDIX A Useful Math The material
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A p p e n d i x A : U s e f u l M a
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Appendix B Suppliers and Other Reso
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A p p e n d i x B : S u p p l i e r
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B.1.6 Rotators and Controllers Alfa
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Index Note: Boldface numbers denote
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I n d e x 747 Binns, Jack, first ma
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I n d e x 749 dipole (Cont.): slopi
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I n d e x 751 grounding and ground
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I n d e x 753 ionospheric propagati
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I n d e x 755 maximum effective len
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I n d e x 757 noise (Cont.): sky no
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I n d e x 763 transmission lines, 1
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I n d e x 765 vertically polarized
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I n d e x 767 Yagi antennas (Cont.)
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