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To Serve As Background, We Shall Review a Generalhnterpretation of Auroral and Related Phenomena

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To Serve As Background, We Shall Review a Generalhnterpretation of Auroral and Related Phenomena PROBLEMS OF AURORAL MORPHOLOGY BY C. T. ELVEY GEOPHYSICAL INSTITUTE, UNIVERSITY OF ALASKA, COLLEGE, ALASKA In the past the problems of auroral morphology were involved with the descrip- tions of individual auroral forms-their heights, dimensions, motions, etc. An example of such arcs is shown in Figure 1. Now the problems that confront us concern the broad scale of the auroral display rather than the individual compo- nents. Our knowledge concerning the broader aspect of auroras depends upon meager and scattered evidence. A large part of the information is statistical in character, giving, for example, the average distribution of auroral display over the earth and the average frequencies of occurrence with respect to time of night, to the seasons, or to the phase of the sunspot cycle. Facts concerning the nature of a given auroral display and how it changes with time are lacking. In addition, we need to know the physical processes associated with the auroral display. These physical processes reveal themselves in many different terrestrial phenomena, such as magnetic storms, ionospheric disturbances, earth current disturbances, iono- spheric absorption, and radio noise from auroras. Each of these phenomena will serve as a tool for untangling the physical processes involved. Statistical relation- ships among the phenomena are known, but detailed studies of thir relationships have only been started. These problems constitute a large part'of the auroral program of the International Geophysical Year, 1957-1958. To serve as background, we shall review a generalhnterpretation of auroral and related phenomena. This interpretation may not be acceptable to everyone in all its details, but there is a considerable amount of observational evidence to substan- tiate it. It may be thought of as a working hypothesis that has been used in de- signing the United States auroral program for the International Geophysical Year. A neutral stream of charged particles is emitted, or propelled, from an active area on the sun. The composition of the stream should-be essentially that of the sun's atmosphere, that is, mainly protons and electrons, with a small percentage of heavier atoms. Evidence indicates that the stream or cloud of gas is propelled with sufficient velocity to reach the earth in approximately 24 hours. As the stream or cloud sweeps across the earth, the magnetic field of the earth deflects and cap- tures some of the charged particles. The particles bombard the atmosphere in regions surrounding the geomagnetic poles, the auroral zones. The particles spiral- ing down the magnetic lines of force penetrate to depths in the atmosphere corresponding to their energy. The average base of most auroral forms is 100 km. above the surface, and it is believed that a proton of 400 kev. energy will penetrate to that depth in the atmosphere. Both direct and indirect effects will result from this bombardment of the atmosphere. The most important direct effect of this bombardment of the atmosphere is the polar aurora, wherein the particles excite the outer shells of electrons of the atmos- pheric gases to radiate light. Second, the particles ionize the gas, leaving trails of electrons that are detected by radar and radio waves and have become known as "radar auroras." A third direct effect, and one which promises to become an extremely important one, is the discovery of X-rays in auroral regions by the rocket group of Iowa State University working under Van Allen.' The X-rays have 63 Downloaded by guest on September 26, 2021 64 GEOPHYSICS: C. T. ELVEY PROC. N. A. S. been detected by using rockoons (balloon-launched rockets) in a survey across the auroral zone from the North Atlantic Ocean into the Davis Straiht, west of Green- land. Other possible direct effects of the bombardment are the heating of the atmosphere in the auroral zone, causing disturbances in the atmospheric circulation, and the emission of radio noise by the charged particles moving in the earth's magnetic field. FIG. 1.-System of auroral arcs. A very important and practical secondary effect, the nondeviative absorption of radio waves in the ionosphere, has been discussed by Chapman and Little.2 The X-rays excited by the incoming charged particles will ionize the atmospheric gases, mostly at the levels below the aurora and in layers, owing to the exponential in- crease of density. The authors show that the absorption will be present both by day and by night, even though there is a minimum of auroral activity near the middle of the day, as shown by radar techniques. Although the X-rays will be far lower in intensity during the day, the full effect is felt because the sunlight pre- vents the attachment of electrons and oxygen atoms. At night the attachment process can proceed uninhibitedly. Consequently a far greater supply of X- rays is required to produce the same amount of absorption. It also seems reason- able that the sporadic E clouds associated with auroras may be explained by the X- ray phenomenon. Downloaded by guest on September 26, 2021 VOL. 43, 1957 GEOPHYSICS: C. T. ELVEY 65 Other secondary, or perhaps we should call them tertiary, effects result from the moving of the ionized gases by the tides, winds, and turbulence of the upper atmos- phere. These effects will evidence themselves as ionospheric storms, in- creased scintillation of radio stars, and other ionospheric phenomena associated with auroral displays. The moving charges will produce electric currents in the upper atmosphere that will reflect as induced currents in the earth, the earth poten- tial disturbances. Likewise, the magnetic fields associated with the atmos- pheric electric currents will produce the disturbances associated with magnetic storms. Returning now to the description of an auroral display and its changes or de- velopment with time, we find that most descriptions are from the local, or small- scale, point of view. It is possible to obtain a fairly good description of the develop- ment of a small auroral display from observations at one point; however, attempt- ing to generalize with regard to the whole display or to extensive displays is very hazardous. Under the best of observing conditions, the observer can see auroras over an area whose radius is approximately 1,000 km. Nevertheless, the resolution of auroral forms at distances greater than 500 km. is rather poor; hence it is safer to restrict interpretations to those within a radius of 500 km. The above is based on the assumption that the height of the base of the aurora is 100 km. Recently, Heppner3 made a study of the development of auroral displays along the magnetic meridian through College, Alaska. He assumed the height of the lower edge of the auroral forms and was thus able to determine from measurements of the elevation above the horizon the geomagnetic latitude of the place where the auroral form was incident. He illustrated the development of the auroral dis- play graphically by plotting the auroral forms in coded symbols on a chart. The ordinate is geomagnetic latitude, and the abscissa is time. Figure 2 is the diagram for the aurora on the night of January 25-26, 1952. We have expanded this idea to show the distribution of auroras in two dimensions. Visual observations from five stations are combined to give synoptic maps of the dis- tribution of auroras over Alaska for each quarter-hour. The synoptic maps for the beginning of each hour during the night of March 26/27, 1954, are shown in Figure 3. Observers working in the region of the auroral zone, where auroras frequently not only cover the entire sky but also are often very active, find it difficult to record visual observations satisfactorily. Therefore, we have investigated the possibility of making the observations photographically. An idea of Gartlein4 for photo- graphing the auroras over the entire sky has been adopted. It is termed the "all- sky" camera and consists of a convex mirror with a 16-mm. camera mounted above it. The photographs are images of the entire sky as seen in the convex mirror. Exposures are made at 1-minute intervals and thus give comprehensive records of auroral displays. A typical photograph of an arc system is shown in Figure 4. This photograph was made with the earlier model of the camera, in which the dura- tion of the exposure was 54 seconds. The remaining 6 seconds of each minute was used to transport the film for the next exposure. The results of the measurements of Figure 4 are shown graphically in Figure 5. It is to be noted that when arcs are photographed, it is frequently possible to trace them to the visible horizon. Knowing the elevation of the visible horizon from actual measurement, it is very Downloaded by guest on September 26, 2021 m . I I I I I I I - I I ...I I I I I I I I I I I I II I I I I' It12 14IS1 fI? Is 20to 21 23 0 1 2 4 S * ? * 9 10ItN f I I . .- I ItiI A A I HORIZONTAL DISTURBANCE MAGNETIC MERIDIAN lo' -AZ(5) E 4100- 0-so . tr Ir r ,rTTI,rTT,rJ~r~rd 20 22 7 11 I I I I I I* + zI I I I I *Az I G G CG _ -69- -69- CLOUDS lfi HAZE G: >~~~~~ -68- -68- W>- 67- -67- C :-66- -66- A I du AM P .-j-65- SLISHT -1 65- - -COLLESE - O-COLLESE _~~~~~~~P 4= e PI w-64- HAZ9 -64- 0 C-63- 63- 2 0 co 'amp -62- -61 - -61- ____ _ _ _ >~~~~~ CLOUDS a H A ZE9 -60- -60- I TWIL1 JANUARY 25,1952-.JANUARY 26, 1952 S S 5 0 I 3 4 a 7 10 11 1I I Is 1 le t 17 o 1 tot0oI 2 23 a 3 I I I I I I I I I I I I I ImI I I II.ii SYMBOLS ?INCOMPLETE OBSERVATIONS DIFFUSE, RAYED PATCHES HOMOGENEOUS ARCS BANDS = DIFFUSE SURFACES RAYED ARCS BANDS OF IP PP FAINT TO MODERATE INTENSITY PULSATING AURORA ACTIVE, BRIGHT RAYED FORMS GLOW m FIG.
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