Fundamentals of Very Low Frequency Emission Generation Mechanisms

Total Page:16

File Type:pdf, Size:1020Kb

Fundamentals of Very Low Frequency Emission Generation Mechanisms JOURNAL OF GEOPHYSICAL RESEARCH VOL. 69, No. 21 NOVEM•ZR 1, 1964 Fundamentals of Very Low Frequency Emission Generation Mechanisms •N. BRICE 1 Radioscience Laboratory Stanford University, Stanford, California Abstract. The transfer of energy between whistler-mode signals and energetic charged particles is examined. Resonance conditions are derived, leading to a classification of the mechanismspreviously suggested for the generationof VLF emissions.The relationshipbe- tween change in energy and change in pitch angle of the particles is derived for the transverse resonance interaction with longitudinal whistler-mode waves. Features of the transverse resonanceplasma instabilities and the anomalousDoppler effect are clarified. Introduction. A number of mechanisms have force F and incremental distance As, and we been suggestedfor the generationof VLF emis- can write for the distancethe productof velocity sions which are observedin the range 300 to and time 30,000 cps. All assume that the emissionsare generated in the ionosphereor magnetosphere AW = F.As (2) by the interaction between whistler-modeelec- = F.vAt (3) tromagneticwaves and energeticparticles in the medium.In this work, by the applicationof = q(E q- v X B).vAt (4) simplephysical principles, the resonancecondi- tions for the interactionsare derived,leading to = qE.vAt (5) a systematic classification of the suggested To obtain a significantamount of energy mechanisms. Some of the more important transfer,we requirethe scalarproduct of electric properties of the mechanismsare also simply field and particle velocity to have a constant explained. (zerofrequency) component. Resonance conditions. In this section we are The motionsof chargedparticles in the mag- concernedwith the derivationfrom first principles netosphereare controlledprimarily by the earth's of the conditions necessaryfor the simplest magnetic field, so that we can conveniently resonances, so that the mutual interaction considerthe velocity to be made up of two between electromagneticwaves and particles components,%1 and vx, parallel and perpendicular which satisfy these resonanceconditions can be to the earth's magneticfield, respectively.The studied. (For a more detailed descriptionof the directionof the transverse velocity will, of course, effectsof waveson the motionof particleswhich rotate at a rate correspondingto the gyro- satisfy transverseresonance conditions see, for frequencyof the particle. example, Helliwell and Bell [1960], Bell et al. If the longitudinalvelocity of the particle is [1963],or Dungey[1963a].) matched to the wave phase velocity and the The force F on a charged particle due to wave has a longitudinal componentof electric electric (E) and magnetic(B) fieldsis given by field, we have a longitudinalresonance, since F = q(E q- v X B) (1) Ell'vii - constant (6) where q is the chargeand v the velocity of the Alternatively, if the particle experiencesan particle. electric field which rotates about the earth's The incremental change in energy of the magnetic field at the same rate and with the particle, AW, is given by the scalar product of same sense as the particle, the transverse resonancecondition is satisfied,since • Now at Faculty of Engineering, Carleton Uni- versity, Ottawa, Ontario, Canada. E•_.v•_= constant (7) 4515 4516 N. BRICE To satisfy the longitudinal resonancecondi- For frequenciesof interest,we can assume tion, we require v• cos 0 = v• (8) [y > [ >> [, (12) wherevp --- wave phasevelocity, and 0 - angle vp<< c (13) betweenwave normal and earth's magneticfield. For the transverseresonance and electrons,we For the transverse resonance, the Doppler- can then write shifted wave frequency seen by the particle must equal the particle gyrofrequencyin magni- /'a- ! (14) tude and have the same polarization. Since cos0 = --v•, whistler-mode waves are right circularly polar- and for protons(y •,• 1) ized, the electric and magnetic fields of the wave rotate about the earth's magnetic field in the same senseas an electron. The longitudinal cos0 = v•! +! Ji (15) velocity required by energetic electrons to satisfy the transverse resonance condition can • v• (16) then be derived from the classical formula for For a wave frequencyof 5 kc/s and zero Doppler shift [Panofskyand Phillips, 1962] as wave normal angle, the energiesof resonance electronsare plotted in Figure I as a function y cos0vii = v•!- (9) of geomagneticlatitude a along the field line terminatingat 60ø geomagnetic latitude (L - 4). where ]H is the gyrofrequencyof the energetic It was assumedthat in the magnetospherethe electrons and plasmafrequency was given by y = (1 -- v]!c")-•/• (10) /'o= 1000fH1/2 (17) _•_1 for nonrelativistic electrons. To obtain a This model of electron density distribution transverse resonance for whistler mode w•ves was deducedfrom measurementsof whistlersby •nd protons, • reversal of polarization must be Smith [1960] for the geomagneticequatorial effected, since the w•ve as seen by the proton plane. This doesnot necessarilyimply that the must •ppe•r to be left circuitfly polarized. For same model applies to the electron density • given circuitfly polarizedw•ve, •s the velocity variation along a field line. The use of this of the observeris increased,the observedw•ve modelis justifiedhere, since we are onlyinterested frequency decreasesuntil it re•ches zero, when in indicating the order of magnitudeof the the observer'svelocity is m•tched with the w•ve particleenergies required to satisfythe resonance phase velocity. As the velocity is further in- conditionsat differentlocations in the magneto- creased,the observedfrequency increasesfrom sphere.For the ionosphere(a = 60ø) energies zero, •nd the w•ve •ppe•rs to h•ve the opposite were computedfor plasmafrequencies of 3 and polarization from that found by • st•tion•ry 7 Mc/s. It was alsoassumed that one-thirdof observer. Thus when the observer's velocity the kinetic energyof the electronwas contained exceedsthe w•ve phase velocity, the polariza- in the longitudinalvelocity. For protons,for tions in the fixed •nd moving framesof reference the longitudinalresonance, the requiredenergy •re opposite, •nd the Doppler s•ft is referred is alsoshown in Figure 1. The energyrequired to •s •nom•lous [•nzburg, 1960]. for the transverseresonance is not greatly As noted •bove, we require •n •nom•lous different,as is shownby (16). From Figure 1 Doppler shift to obtain • transverse resonance it is seenthat, for the longitudinalresonance, between whistler-mode w•ves •nd protons, so the energiesrequired are smallest in the iono- that the proton longitudinal velocity required sphere. For the transverse resonance and for the resonanceis given by electrons,the energiesrequired are large except near the top of the magnetic field line path •v•cos J+ J' (11) (small valuesof a). In examiningthe suggestedmechanisms for the where[• is the ion (proton)gyrofrequency. generationof VLF emissions,we note that all GENERATION OF VLF EMISSIONS 4517 ratio of proton to electron mass) greater than that for electrons. As a result, the number + + densityof suitableparticles that can realistically iOs be postulatedis much less for protons than for + electrons. The other six possible mechanisms + + have all been previously suggested for the • I05 + generationof VLF emissions. + Cerenkov radiation from electrons (L, e, S) was suggestedor consideredby Kolomenskii øo" [1956], Ellis [1957], Eidman [1958], Dowden [1960], Ellis [1960], Gendrin [1960], Ondoh[1961, I 1962, 1963], Gershman and Ugarov [1961], Beneditkovand Eydman [1961], Clemmow[1962], io$ E] PROTONENERGY, LONGITUDINAL RESONANCE and McKenzie [1963]. G ELECTRONENERGY, LONGITUDIN.Z•_ RESONANCE The traveling wave amplificationhypothesis + ELECTRONENERGY, TRANSVERSE RESONANCE (L, e, I) has been examinedby Helliwell [1956], io2 I i I I I •) o I0 20 30 40 50 60 Gallet [1959], Gallet and Helliwell [1959], Bell GEOMAGNETIC LATITUDE (DEGREES) and Helliwell [1960], Barrington [1960], Kimura [1961], Adachi and Mushiake [1962], and Dowden Fig. 1. Particle energies required to satisfy the resonance conditions at different latitudes along a [1962a].Doppler-shifted cyclotron radiation from magnetic field line path. protons (T, p, S) has been treated by Aarons [1960], MacArthur [1959], Murcray and Pope involve either the longitudinal or the transverse [1960a, b], Santirocco [1960], and Knox and resonance,and that in all casesprotons or elec- Rycro•t[1964], while the correspondingradiation trons are suggestedto be the energeticparticles. from electrons(T, e, S) has been postulatedby In addition some authors have suggestedthat Dowden[1962b, c, d, e, •; 1963] and considered individual particles will emit Cerenkov or cyclo- by Brice [1963] and Hansen [1963]. tron radiation and that, if a large number of A transverseresonance plasma instability for particlesradiate, an emissionis observed.These a proton beam (T, p, I) was found by Kimura radiation processesare, in essence,single particle [1961] and Maeda and Kimura [1962, 1963], and effects. Others have considered collective effects the transverseresonance plasma instability for of energetic particles and suggested plasma electrons(T, e,I) wassuggested by Brice [1963] instabilities. We can now classify the various and wasinvestigated by Bell andBuneman [1964]. suggestedmechanisms according to the resonance Energytransfer. It is instructiveto examine condition, longitudinal (L) or transverse(T), the transfer of energy from waves to particles and the type of particles, protons (p) or elec- for the transverse
Recommended publications
  • WWVB: a Half Century of Delivering Accurate Frequency and Time by Radio
    Volume 119 (2014) http://dx.doi.org/10.6028/jres.119.004 Journal of Research of the National Institute of Standards and Technology WWVB: A Half Century of Delivering Accurate Frequency and Time by Radio Michael A. Lombardi and Glenn K. Nelson National Institute of Standards and Technology, Boulder, CO 80305 [email protected] [email protected] In commemoration of its 50th anniversary of broadcasting from Fort Collins, Colorado, this paper provides a history of the National Institute of Standards and Technology (NIST) radio station WWVB. The narrative describes the evolution of the station, from its origins as a source of standard frequency, to its current role as the source of time-of-day synchronization for many millions of radio controlled clocks. Key words: broadcasting; frequency; radio; standards; time. Accepted: February 26, 2014 Published: March 12, 2014 http://dx.doi.org/10.6028/jres.119.004 1. Introduction NIST radio station WWVB, which today serves as the synchronization source for tens of millions of radio controlled clocks, began operation from its present location near Fort Collins, Colorado at 0 hours, 0 minutes Universal Time on July 5, 1963. Thus, the year 2013 marked the station’s 50th anniversary, a half century of delivering frequency and time signals referenced to the national standard to the United States public. One of the best known and most widely used measurement services provided by the U. S. government, WWVB has spanned and survived numerous technological eras. Based on technology that was already mature and well established when the station began broadcasting in 1963, WWVB later benefitted from the miniaturization of electronics and the advent of the microprocessor, which made low cost radio controlled clocks possible that would work indoors.
    [Show full text]
  • Study of the Phenomenon of Whistler Echoes
    RADIO SCIENCE Journal of Research NBS jUSNC- URSI Vol. 69D, No. 3, March 1965 Study of the Phenomenon of Whistler Echoes T. Laaspere, W. C. Johnson, and J. F. Walkup Contribution From the Radiophysics Laboratory, Thayer School of Engineering, Dartmouth College, Hanover, N.H. (Received July 6, 1964; revi sed Nove mbe r 5, 1964) In considering the propagation of long whistle rs and whistle r echo trains, the question arises about where the downcoming whistlers are refle cted. The several s uggestions that have been made include ground reflection and refl ection at the lowe r boundary of the ionosphere. In either case, the echo of a daytime whistler would make several more passes through the absorbing V region than the whistler itself, a nd we should expect whistl ers occurring a round noon to have a much smaller probabil­ ity of havin g echoes than whistlers occurring at ni ght. An analysis of several years of data obt ained a t the Da rtmouth Co ll ege whistl e r stati on yield s the result, however, that although the ave rage whi stl er rate is muc h hi ghe r at ni ght than during the day, the probability of a whi stl er having a n echo shows little cha nge from midnight to midday. Consistent with this observati on are the results of anoth er study showing that the diffe rence in the intensity of a noo ntime whis tle r and its echo may be onl y a few decibels. If th e th eoreti cal predicti ons about absorption of whi s tle r-mode waves a re even nearly correct, our results on whi stl e r echoes a re in compatible with the lowe r-boundary or ground·re fl ecti on model.
    [Show full text]
  • Study on the Guiding Mechanism of Whistler Radio Waves Saburo Adachi
    RADIO SCIENCE Journal of Research NBSjUSNC-URSI Vol. 69D, No.4, April 1965 Study on the Guiding Mechanism of Whistler Radio Waves Saburo Adachi Deparbnent of Electrical Communications, Tohoku University, Sendai, Japan (Received October 14, 1964; revised November 23, 1964) A full wave theory is applied to the whistler radio wave propagation along a plasma slab with an enhanced or depressed plasma density which is imbedded in an infinite magnetoplasma. Rigorous dispersion equation is solved for a thin slab in approximate but explicit forms. Three types of propagation modes are found: (a) a completely trapped surface wave mode along the depressed slab in the frequency region above a half of gyrofrequency and below a gyrofrequenc y, (b) a com· pletely trapped surface wave mode along the highly enhanced slab in the frequency region above a half of gyrofrequency and below a certain cutoff frequency less than a gyrofrequency, and (c) a partially trapped (leaky) surface wave mode along th e enhanced slab in the freque ncy region above a certain cutoff frequency and below a half of gyrofrequenc y. Di s· persion properti es, fi eld di stributions and an attenuation of the third mode due to th e leakage of the transmitted power are discussed in detail. The attenuation is found to in crease very rapidly wit.h increasing frequency, thickness and enhancement of ionization of th e slab. The exact numerical solutions are also obtained and compared with the approximate solutions. 1. Introduction A number of theoretical investigations have been made on the propagation of whis tler radio waves since the publication of Storey's famous paper [Storey, 1953], and not a few papers have dealt with the propagation path and the guiding mechanism of the whistlers.
    [Show full text]
  • EHC 238 Front Pages Final.Fm
    This report contains the collective views of an international group of experts and does not necessarily represent the decisions or the stated policy of the International Commission of Non- Ionizing Radiation Protection, the International Labour Organization, or the World Health Organization. Environmental Health Criteria 238 EXTREMELY LOW FREQUENCY FIELDS Published under the joint sponsorship of the International Labour Organization, the International Commission on Non-Ionizing Radiation Protection, and the World Health Organization. WHO Library Cataloguing-in-Publication Data Extremely low frequency fields. (Environmental health criteria ; 238) 1.Electromagnetic fields. 2.Radiation effects. 3.Risk assessment. 4.Envi- ronmental exposure. I.World Health Organization. II.Inter-Organization Programme for the Sound Management of Chemicals. III.Series. ISBN 978 92 4 157238 5 (NLM classification: QT 34) ISSN 0250-863X © World Health Organization 2007 All rights reserved. Publications of the World Health Organization can be obtained from WHO Press, World Health Organization, 20 Avenue Appia, 1211 Geneva 27, Switzerland (tel.: +41 22 791 3264; fax: +41 22 791 4857; e- mail: [email protected]). Requests for permission to reproduce or translate WHO publications – whether for sale or for noncommercial distribution – should be addressed to WHO Press, at the above address (fax: +41 22 791 4806; e-mail: [email protected]). The designations employed and the presentation of the material in this publication do not imply the expression of any opinion whatsoever on the part of the World Health Organization concerning the legal status of any country, territory, city or area or of its authorities, or concerning the delimitation of its frontiers or boundaries.
    [Show full text]
  • Formation of Ionospheric Precursors of Earthquakes—Probable Mechanism and Its Substantiation
    Open Journal of Earthquake Research, 2020, 9, 142-169 https://www.scirp.org/journal/ojer ISSN Online: 2169-9631 ISSN Print: 2169-9623 Formation of Ionospheric Precursors of Earthquakes—Probable Mechanism and Its Substantiation Georgii Lizunov1, Tatiana Skorokhod1, Masashi Hayakawa2, Valery Korepanov3 1Space Research Institute, Kyiv, Ukraine 2Hayakawa Institute of Seismo Electromagnetics Co., Ltd., Tokyo, Japan 3Lviv Center of Institute for Space Research, Lviv, Ukraine How to cite this paper: Lizunov, G., Sko- Abstract rokhod, T., Hayakawa, M. and Korepanov, V. (2020) Formation of Ionospheric Pre- The purpose of this article is to attract the attention of the scientific commu- cursors of Earthquakes—Probable Me- nity to atmospheric gravity waves (GWs) as the most likely mechanism for chanism and Its Substantiation. Open the transfer of energy from the surface layers of the atmosphere to space Journal of Earthquake Research, 9, 142-169. https://doi.org/10.4236/ojer.2020.92009 heights and describe the channel of seismic-ionospheric relations formed in this way. The article begins with a description and critical comparison of sev- Received: October 20, 2019 eral basic mechanisms of action on the ionosphere from below: the propaga- Accepted: March 13, 2020 tion of electromagnetic radiation; the closure of the atmospheric currents Published: March 16, 2020 through the ionosphere; the penetration of waves throughout the neutral at- Copyright © 2020 by author(s) and mosphere. A further part of the article is devoted to the analysis of theoretical Scientific Research Publishing Inc. and experimental information relating to the actual GWs. Simple analytical This work is licensed under the Creative Commons Attribution International expressions are written that allow one to calculate the parameters of GWs in License (CC BY 4.0).
    [Show full text]
  • Spatial Correlation Between Lightning Strikes and Whistler Observations
    234 South African Journal of Science 105, May/June 2009 Research Letters lightning is most prevalent here, whistlers are very rare. At Spatial correlation between medium latitudes whistlers become far more common. Whistlers recorded in this region have the general characteristics of higher lightning strikes and whistler frequencies arriving before the lower frequencies. These whistlers observations from Tihany, propagate mainly through the plasmasphere. At higher latitudes the whistlers have a distinct nose-frequency. This means that Hungary after the initial frequency a signal of both rising and descending frequencies will be recorded. However, due to the rare occurrence of lightning at high latitudes, whistlers are fairly uncommon a,b,c* a,d a J. Öster , A.B. Collier , A.R.W. Hughes , compared to middle latitudes. b e L.G. Blomberg and J. Lichtenberger The specific shape of a whistler is determined by the plasma density and strength of the magnetic field in the duct. Whereas the former principally determines the propagation delay, the latter dictates the frequency of minimum delay. Whistlers A whistler is a very low frequency (VLF) phenomenon that acquires generated at higher latitudes spend more time in the duct thus its characteristics from dispersive propagation in the magneto- experiencing greater dispersion. sphere. Whistlers are derived from the intense VLF radiation The focus of this study was to examine the relationship produced in lightning strikes, which can travel great distances between whistlers and lightning strikes. This was achieved by within the Earth-ionosphere waveguide (EIWG) before penetrating performing correlation calculations between a whistler data set the ionosphere, and exciting a duct.
    [Show full text]
  • Dependence of Whistler Activity on Geomagnetic Latitude* MANORAN]AN RAO
    Indian Journal of Radio & Space Physics Vol. 1, June 1971, pp. 192·194 Dependence of Whistler Activity on Geomagnetic Latitude* MANORAN]AN RAO. LALMANI, V. V. SOMAYA]ULU & B. A. P. TANTRY Electronics & Radio Physics Laboratory, Department of Physics, Banaras Hindu University, Varanasi 5 ManuscriPt received 16 March 1972 It is shown that the couplin~ between the ordinary and extraordinary magneto-ionic waves in the lower ionospheric regions should also be considered as one of the factors which control the dependence of whistler activity on the ~eoma~netic latitude. Introduction In this communication we wish to point out that the coupling between the ordmary and extraordi• nafY magneto-ionic waves in the lOWEr ionsphelic latitudinal variation of the whi:;tler occur• layers siouid also ie considered as one of the factors OUR knowledge of the diurnal, seasonal and rence is derived mainly from the synoptic which control the dependence vf whistler activity observations made at a chain of stations under on the geomagnetic latitude. We also show t.rat the whistler-eastl and whistler-west .networks2,3 the dependmce of the coupling parameter 011 the during the IGY and IGC periods. An important latitude satisfaCtorily exphJins the observed whistler feature of the latitudinal variation of the whistlel activity. Towards this end ",e first derive the ex• activity if:: the high whistler rate occurrence ob· pression for the coupling parameter following the selVed at high geomagnetic latitudes in contrast to treatment given by Budden9 and tben briefly dis• the low rate at low geomagnetic latitudes4•5• A cuss the physical mechanism of the coupling pheno• part of the observed latitudinal variaticn in wbistlEr menon.
    [Show full text]
  • The Properties of Lion Roars and Electron Dynamics in Mirror Mode
    Journal of Geophysical Research: Space Physics RESEARCH ARTICLE The Properties of Lion Roars and Electron Dynamics in Mirror 10.1002/2017JA024551 Mode Waves Observed by the Magnetospheric Special Section: MultiScale Mission Magnetospheric Multiscale (MMS) Mission Results Throughout the First Primary H. Breuillard1 ,O.LeContel1 , T. Chust1, M. Berthomier1, A. Retino1 , D. L. Turner2 , Mission Phase R. Nakamura3 , W. Baumjohann3 , G. Cozzani1, F. Catapano1, A. Alexandrova1, L. Mirioni1 , D. B. Graham4 , M. R. Argall5 , D. Fischer3 , F. D. Wilder6 , D. J. Gershman7 , A. Varsani3 , Key Points: 8 4 8 6 6 • Intense lion roars are observed in P.-A. Lindqvist , Yu. V. Khotyaintsev , G. Marklund ,R.E.Ergun , K. A. Goodrich , mirror modes by high time N. Ahmadi6 , J. L. Burch9 , R. B. Torbert5 , G. Needell5 , M. Chutter5 ,D.Rau5 , resolution instruments on board I. Dors5 , C. T. Russell10 , W. Magnes3 , R. J. Strangeway10 , K. R. Bromund7 ,H.Wei10 , Magnetospheric MultiScale mission • Nonlinear lion roars are observed up F. Plaschke3 , B. J. Anderson11 ,G.Le7 , T. E. Moore7 , B. L. Giles7 , W. R. Paterson7 , . to 0 4fce due to their high amplitude, C. J. Pollock7 , J. C. Dorelli7,L.A.Avanov7 , Y. Saito12 , B. Lavraud13 , S. A. Fuselier9 , which may have been underestimated 11 11 1 in previous studies B. H. Mauk , I. J. Cohen , and J. F. Fennell • Possible signatures of linear and 1 nonlinear resonant interaction Laboratoire de Physique des Plasmas, UMR7648, CNRS, Ecole Polytechnique, UPMC Univ Paris 06, Univ. Paris-Sud, between lion roars and electrons,
    [Show full text]
  • Electron Beams As the Source of Whistler‐Mode Auroral Hiss at Saturn A
    GEOPHYSICAL RESEARCH LETTERS, VOL. 37, L09102, doi:10.1029/2010GL042980, 2010 Click Here for Full Article Electron beams as the source of whistler‐mode auroral hiss at Saturn A. J. Kopf,1 D. A. Gurnett,1 J. D. Menietti,1 P. Schippers,1 C. S. Arridge,2,3 G. B. Hospodarsky,1 W. S. Kurth,1 S. Grimald,4 N. André,4 A. J. Coates,2,3 and M. K. Dougherty5 Received 23 February 2010; revised 26 March 2010; accepted 30 March 2010; published 4 May 2010. [1] Over the last three years, the Cassini spacecraft has been by electron beams associated with the aurora. Initially auroral in a series of high inclination orbits, allowing investigation hiss was believed to be produced by incoherent Cherenkov and measurements of Saturnian auroral phenomena. During radiation [Jørgensen, 1968]. However, this theory later this time, the Radio and Plasma Wave Science (RPWS) proved insufficient to explain the observed intensities, which Investigation on Cassini detected low frequency whistler were far too large for this mechanism [Taylor and Shawhan, mode emissions propagating upward along the auroral field 1974]. Around the same time, sounding rocket experiments lines, much like terrestrial auroral hiss. Comparisons of observed whistler mode plasma waves in conjunction with an RPWS data with Cassini Plasma Spectrometer (CAPS) artificially injected electron beam [Cartwright and Kellogg, plasma measurements during a high‐latitude pass on 17 1974; Monson et al., 1976]. Maggs [1976] first suggested October 2008, show that intense upward moving electron that auroral hiss was generated by a coherent beam‐plasma beams with energies of a few hundred eV were associated interaction at the Landau resonance velocity.
    [Show full text]
  • What Is Rf? It's Like Magic
    Originally appeared in the December 2011 issue of Communications Technology. WHAT IS RF? IT’S LIKE MAGIC By RON HRANAC The cable industry has, since the very first systems in the late 1940s, embraced and been based on radio frequency (RF) technology. These days, we’ve also embraced the digital world — and a subset of digital technology called Internet protocol (IP) — but RF still is needed in most cable networks to transport digital data to and from devices in our subscribers’ homes. The answer to the question in the title of this month’s column is far more complicated than it seems initially. A good place to start is with an explanation of “R” and “F.” What’s radio frequency? Here’s one high-level perspective: It’s that portion of the electromagnetic spectrum from a few kilohertz to about 300 gigahertz. The radio-frequency part of the electromagnetic spectrum is further broken down into two chunks: radio waves and microwaves. Some references define radio waves as those with a frequency starting at about 3 kHz (the beginning of the very low frequency [VLF] band) and extending to 300 MHz (the beginning of the ultra high frequency [UHF] band), with microwaves covering roughly 300 MHz to 300 GHz. The latter is the beginning of the far infrared (FIR) portion of the electromagnetic spectrum. Other references have microwaves starting at frequencies higher than 300 MHz; indeed, many RF engineers consider the microwave spectrum to be higher than about 1 GHz. Radio frequency also can be defined as a rate of oscillation within the 3 kHz to 300 GHz range (more on this in a moment).
    [Show full text]
  • Very-Low-Frequency Radio Propagation in the Ionosphere
    JOURNAL OF RESEARCH of the National Bureau of Standards-D. Radio Propagation Vol. 66D, No. 6, November- December 1962 Very-Low-Frequency Radio Propagation In the Ionosphere Daniel W. Swift Contribution from Research and Advanced Development Division, Avco Corporation, Wilmington, Mass. (R eceived April 27, 1962 ; revised June 5, 1962) Equations describing the propagation of radio waves in a horizontally stratified a niso­ tropic ionosphere were developed by considering the limit.ing case of a la rge number of in­ finitesimall y t hin slabs of constant electron density a nd collision frequency. The quasi­ longitudin al approximation was used. The propagation equations appeared as four co upled first-order linear differential equations, co upled by gradients in electron density and collision frequency. The quasi-longit udina l a pproxima tion permitted use of particul a rl y s imple forms for t he co upling coe ffi cients, t hese forms bein g a menable to simple analysis. Coupling between two ordinary or two extraordinary modes was found to be co nsid erably stronger than cross coupling between ordinary a nd extraordinary mode . Cross couplin g was related to the rate of change of the direction of the phase normal. It was found that the re fl ection of VLF radio waves from t he daytime ionosphere is relatively insensitive to t he angle of incidence on the ionosphere except for highly oblique propagation. "Vhistler penetration was a lso found to be insensitive to the angle of in cid ence on the ionosphere. 1. Introduction In this report, we shall consider the full-'wave solutions for a very low frequency radio wave propagating obliquely into a horizontally stratified ionosphere.
    [Show full text]
  • L Dependence of Energetic Electron Precipitation Driven by Magnetospherically Reflecting Whistler Waves J
    JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 107, NO. A8, 1150, 10.1029/2001JA000303, 2002 L dependence of energetic electron precipitation driven by magnetospherically reflecting whistler waves J. Bortnik, U. S. Inan, and T. F. Bell Space, Telecommunications, and Radioscience Laboratory, Electrical Engineering Department, Stanford University, Palo Alto, CA 94305, USA Received 19 September 2001; revised 16 November 2001; accepted 30 November 2001; published 1 August 2002. [1] Ray tracing analysis and a first-order treatment of the wave frequency and electron energy dependence of gyroresonant pitch angle scattering reveals the L shell dependence of the time-integrated energetic electron (>150 keV) precipitation flux in the drift loss cone due to a single cloud-to-ground lightning stroke. Primary features of the L dependence are determined by the ray paths of magnetospherically reflecting nonducted whistler waves, as well as the refraction of the wave normal vectors due to ionospheric horizontal electron density gradients at low latitudes. Calculations for lightning source latitudes of 25°,35°, and 45°, with an assumed ‘‘average’’ ionospheric electron density profile, as well as an International Reference Ionosphere model profile, indicate that horizontal ionospheric electron density gradients can cause the whistler wave energy to focus near the geomagnetic equator on the first magnetospheric traverse, resulting in a spatially narrow precipitation signature at low L shells (1.4 < L < 1.65). The magnitude of this low-L peak is found to be sensitively dependent on the local ionospheric density gradients. Subsequent magnetospheric reflections result in a broad precipitation peak at higher L shells (1.8 < L < 4.2), which is robustly present, with magnitude being relatively insensitive to lightning source-latitude and ionospheric horizontal gradients.
    [Show full text]