DOCSLIB.ORG

The Fairbanks Halo of April 27, 1966 J

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Fairbanks Halo of April 27, 1966 J October 1%6 J. R. Blake 599 THE FAIRBANKS HALO OF APRIL 27, 1966 J. R. BLAKE Geophysical Instifufe, University of Alaska, College, Alaska ABSTRACT A description of a magnificent display of solar haloes visible over Fairbanks, Alaska, is presented and a photo- graphic rccord of thc nnthclic arcs is uscd to compare these arcs with the two principal theories of Wegener and Hnstings. The temperature range and interval of possible crystal formation is inferred from the halo forms and compared with aerological data at the time of the display. 1. INTRODUCTION of the ice crystals present, and on the solar altitude, h,. We refer the reader to the literature 12, 3, 5, 6, 8, 14, 16, The appearance of extensive displays of solar haloes is 17, 19,201 for further details, particularly to the exhaustive an uncommon event in most parts of the world away review by Visser [19], who describes over 50 different from the polar ice-caps. The d'splay reported here forms. The ice crystals producing the haloes usually constitutes one of the more impressive, appearances, occur in high, cirriforrn cloud, but sometimes, especially comparing favorably with the classics of history, such as over the polar ice-caps, the crystals occur very close to those described by Pernter and Exner [IS] and those the ground [4, 11, 211 giving rise to exceptionally brilliant analyzed by Visser [19]. It was visible from the general displays. vicinity of Fairbanks, Alaska and the observations here reported were made from nearby College (64'51' N., 2. DESCRIPTION 147'50' W.), between 1300 and 1530 Alaskan Standard Time (UT-10 hr.), on April 27, 1966. The accompanying photographs show the display The time of the first appearance of the haloes is not recorded by a Panon Widelux camera with a 140' horizon- known, but they were visible by 1230 and certainly well tal view (fig. l),and by an all-sky camera (fig. 2). The developed by 1300 AST, appearing in very filmy cirriform cloud covering most of the sky. The particular arcs that 1 The all-sky camera is designed for auroral photography. It consists of a convex mirror reflei tlng the entire sky via a plane mirror into the camera. The radial scale is not linear appear in such events depend on the type and orientation or cosine. FIGURE1.-Display seen by Panon Widelux camera with 140" horizontal view. High Speed Ektachrome (160 ASA) f:ll, 11250 sec. Unauthenticated | Downloaded 09/27/21 09:19 AM UTC 600 MONTHLY WEATHER REVIEW Vol. 94, No. 10 I FIGURE2.--Display seen by all-sky camera, with Pentax camera, 55-mm. Tachomar lcns, High Speed Ektnchrome at 1/500 sec. various arcs are identified in the following description by tween the 22O-parhelia and the sun, in comparison with its reference to figures 3 and 4. appearance elsewhere, even toward the anthelic point. At 1300 AST (h,=37.6'), the display was essentially that Superposed over the parhelic circle were both 120'- shown in figure 3. The most brilliant haloes were the paranthelia (lo), appearing as bright white knots of light, white, complete parhelic circle (4) , the colored 22O-par- with no arc estensions. At 1325 AST (h,=36.5') the helia (3) and their white tails superposed over the parhelic azimuth of these was measured at approximately 119' by circle, and the npper portion of the circumscribed halo (5) Prof. W. Mendenhall of the Engineering Department of and its intense white iTei1. As is frequently the case, the this University, using a surveyor's level, He also meas- parhelic circle was appreciably weaker in intensity be- ured the azimuth of &he parhelia as approximately 33' Unauthenticated | Downloaded 09/27/21 09:19 AM UTC October 1966 J. R. Blake 691 FIGURE4.-Sketch of display at 1510 AST (h,=28.8"). At this first observation, the 46"-halo (2) was not present at all, but the infralateral tangential arcs (8) were very bright and coIored, especially at their point of closest approach to the sun (the point of "tangency"). By 1320 AST (h,=36.2"), the 46'-halo was very weakly visible, and the points of minimum approach were indeed points of tangency. FIGURE%.-Sketch of display for period 1300-1430 BST (h,=37.6"- Extending below the parhelia (the focal lines of which 32.2'). Based on all-sky camera photograph by T. Ohtake. appeared to be inclined at some 60" or so to the parhelic circle, rather than normal to it) could faintly be detected the arcs of Lowitz (7), appearing as nearly straight lines, from the sun, at the same solar elevation, a figure agreeing perhaps slightly concave toward the sun, and extending excellently with that deduced from Wegener's [20] equa- toward the 22'-ring as sniooth extensions of the parhelic tions (33.1'). inclination. The arcs merged into the general glare and The circumscribed halo (5) was visible in two parts-the the point of contact could not be determined; likewise upper and lower contact arcs to the 22'-halo. Both parts the relative weakness of the arcs combined with the were very bright and colored, the lower one being con- overall glare prevented any determination of color. With siderably more diffuse than the upper one. The non- the exception of the parts very close to the parhelia, minimal refractions (analogous to the tails of the parhelia) the arcs did not persist clearly for very long, slowly produce a white haze on the outside of the focal line of this merging with the background illumination. halo, being exceptionally intense in the upper and lower Very faintly visible at this stage were portions of white solar vertical where the arcs are concave away from anthelic arcs (ll),converging approximately toward the the sun and the "tails" thus convergent. This accounts anthelic point, but not reaching it. The projection for the diffuseness of the sharply curved lower arc. The toward the sun was much more difficult to determine and upper arc did not at first reach the parhelic circle (4) but no decision could be reached as to a point of convergence later did so in a faint extension. The lower arc showed except t,hat it could not be much higher than the 22"-halo sufficient extension for the change of curvature to be in the solar vertical; it could however, have been as low detected, but did not reach the turning point back toward as the sun itself. The eastern arc was especially stronger the parhelic circle. than the other. The 22O-halo (1) was very weak, though always detect- By 1320 AST (h,=36.2") the 46'-halo had appeared able throughout the entire display. At first sight it ~eakl~7,in sections, strongest in the solar vertical. The appeared that the portion in the solar vertical was brighter, whole halo was faintly visible for a while. The anthelic whiter, and was intersected by the brilliant upper contact arcs (11) developed more strongly and extended farther arc. As the solar altitude decreased however, this portion toward the anthelic point, quite definitely converging separated from the 22O-hal0, and it was evident that Par- toward it although again not reaching it. They still ry's arc (6) was present, at first being very close to the showed no evidence of color and the extension solarward 22O-ring. It was later lost in the glare from the contact was still insufficient to define the point of convergence or arc "veil". Wegener's [20] theory shows a separation of mergence. <lo at a solar elevation of 37.6' and the observations are The whole display faded appreciably by 1345 AST thus in good agreement. (h,=35.4") , particularly the anthelic arcs and eastern Unauthenticated | Downloaded 09/27/21 09:19 AM UTC 602 MONTHLY WEATHER REVIEW Vol. 94, No. 10 120O-paranthelia. By 1430 (h,=32.2') however, the quite bright. Since the major part of Parry's arc is pro- anthelic arcs and 12O0-paranthelia reached their maximum duced by ice-columns with principal axes oriented from intensity and extent. The lower circumscribed halo, about 45" to 90" to the incident light, crystals producing arcs of Lomitz, and eastern infralateral tangential arc had a predominance of end reflections (i.e., anthelic arcs) over by this time gone completely, the western infralateral pure refraction (i.e., Parry's arc) would need to be short; arc and upper circumscribed halo were much weaker and however, short crystals would certainly destroy the very very diffuse, Parry's arc being lost in the diffuseness. The special orientation required for the production of Parry's 46"-halo existed faintly in the solar vertical. arc (a pair of prism faces must remain horizontal, thus By 1510 AST (h,=2S.S0) the display mas considerably presenting maximum air resistance and requiring long more diffuse and weaker ; however in the solar vertical, crystals and no turbulence). It thus appears that the a short, colored, but diffuse arc (9) was visible (see fig. 4), conditions for the production of Hastings' arc are mutually concave away from the sun, but in contact with the 46"- contradictory. halo which was still visible in this region. The point re- At least two other forms of anthelic arcs have been garding its tangency was specifically examined and it was reported. One (see Liljequist [11]) is not involved here. noted down as definitely tangential. Later calculation The other, however, frequently appears in observer's showed that the circumzenithal arc of Bravais (cf. [19]) reports as intersecting the sun [I, 161, although it is possi- should have been separated from the 46O-halo at this solar ble that some, at least, of these result from inaccurate elevation by about 2%".
Load more

Recommended publications
  • The Dust Storm of January 22, 1933. Over Sections of Illinois, Indiana, and Michigan
    JANUARY,1933 MONTHLY WEATHER REVIEW 17 hours thereafter the wind was comparatively light, but circle; half of the. paraselenic circle; a lunar pillar, vertical from 8 o'clock till midnight the hourly movement es- t,hrough the moon, ancl a cross, produced by the lunar ceeded 40 miles. pillar and the adjacent portions of the paraselenic circle. The greatest damage occurred in the vicinity of Chey- J. H. Spencer, senior meteorologist, and A. P. Iieller, enne, principally to roofs, chimneys, spouting, window junior met,eorologist, Buffalo, N. P., observed from 8 glass, small garages, street signs and wres. At Fort p. m., February 8, 1933, to after midnight (brightest from Frances E. Warren the damage, esceeded $12,000 and in 9: 30 p. in. to 10: 30 p. m.) the halo of 22'; the paraselenic Cheyenne more than $10,000. In the immediate vicinity circle, c,omplete; and a portion of the halo of 46'. of Cheyenne the damage to buildings amounted to about NOTE.-on these dates the moon was nea.rly full, that $3,000. In the rest of the State the damage is placed at is, at about i6s brightest, and the hdo-producing cirrus $20,000 to $40,000. so thin that the brighter stars were clearly visible through For more than a month prior to this storm there had it. In short, bobh the moon and the cirrus haze were in been very little precipitation and the wind, being ahnor- their optiumum stja.tes for producing visible halos. mally high, had removed moisture Irom the soil to a con- Similar solar halos were observed on this date, Febru8.V siderable depth.
    [Show full text]
  • 1 Atmospheric Halos Columnar and Plate Ice Crystals 22° and 46
    Dr. Christopher M. Godfrey Atmospheric Halos University of North Carolina at Asheville Columnar and Plate Ice Crystals Complex Display at South Pole Image © Marko Riikonen ATMS 455: Physical Meteorology – Spring 2021 ATMS 455: Physical Meteorology – Spring 2021 Good/Bad Crystals for Halo Formation 22° and 46° Halos Crystals collected during a superb Crystals from a mediocre halo South Pole display on 17 January display 16 days earlier. They have 1986. Apart from a few small air large inclusions and their faces are bubble inclusions, the crystals imperfect. (Photographs from really are like their hexagonal plate Atmospheric Halos by Walter Tape) and column ideals. Source: http://www.atoptics.co.uk/halo/xtalreal.htm ATMS 455: Physical Meteorology – Spring 2021 ATMS 455: Physical Meteorology – Spring 2021 22º Halo Sundog (Parhelion) © S. Hudson ATMS 455: Physical Meteorology – Spring 2021 ATMS 455: Physical Meteorology – Spring 2021 1 Ice Crystal Phenomena Halos and Sundog 22º Halo 46º Halo Parhelic Circle Sundog © S. Hudson ATMS 455: Physical Meteorology – Spring 2021 ATMS 455: Physical Meteorology – Spring 2021 © C. Godfrey 22º Halo and Sundogs Sundog 22º Halo (parhelion) Parhelic Circle Sun Sundog Sundog © S. Hudson ATMS 455: Physical Meteorology – Spring 2021 ATMS 455: Physical Meteorology – Spring 2021 © E. Godfrey 22º Halo Upper Tangent Arc Parhelic Parhelic Circle Circle Positioned at top of 22° halo Diamond dust was falling when the photo was taken Sun Sundog (parhelion) © C. Godfrey ATMS 455: Physical Meteorology – Spring 2021 ATMS 455: Physical Meteorology – Spring 2021 2 Circumzenithal Arc Upper Tangent Arc with Circumzenithal Arc Circumzenithal Arc You are looking almost straight up with the sun at the bottom of the image Formed by refraction through hexagonal plate crystals Supralateral Arc The supralateral arc is more common than, and is often 22º Halo mistaken for, the 46° halo Sun is below 32° elevation © C.
    [Show full text]
  • Halos from Prismatic Crystals
    Atmospheric Halos and the Search for Angle x Item Type Book Authors Tape, Walter; Moilanen, Jarmo Publisher American Geophysical Union Download date 06/10/2021 22:55:50 Link to Item http://hdl.handle.net/11122/6400 CHAPTER 6 Halos From Prismatic Crystals his chapter treats what might be called the classical halos—the halos arising in Tthe simplest sorts of ice crystals, namely, hexagonal prismatic crystals. These halos, then, are not the odd radius halos. The treatment is not intended to be comprehensive. More information, including ray path diagrams and many more simulations, can be found in the book Atmospheric Halos [76]. Also, at the time of this writing there was at least one halo simulation program available on the internet.1 With it, you can change the sun elevation, the crystal shapes, crystal orientations, etc., and see for yourself how the halos are expected to change. The halos in this chapter are organized according to the crystal orientations that make them (Figure 6.1). By far the most common orientations are plate orientations, column orientations, and random orientations. Parry orientations are rare, and Lowitz orientations are rarer still. Plate arcs Recall that a crystal is in plate orientation when its two basal faces are (more or less) horizontal. Numbering the crystal faces 1, 2, . , 8 as in Figure 6.1, we always assume—without loss of generality—that in plate orientation it is face 1 that is the top horizontal face. The halos that arise in crystals with plate orientations are known as plate arcs. Plate arcs from prismatic crystals are shown in Figure 6.2.
    [Show full text]
  • A Study on Atmospheric Halo Visualization
    A Study on Atmospheric Halo Visualization Sung Min Hong and Gladimir Baranoski Technical Report CS-2003-26 September, 2003 School of Computer Science University of Waterloo 200 University venue West Waterloo, Ontario, Canada N2L 3G1 2 Contents 1 Introduction 3 2 Halo Phenomena 5 2.1 General description of halo phenomena .............. 5 2.2 Ice crystal model and halo phenomena .............. 6 3 Survey of Halo Simulation 15 3.1 History of halo simulation ..................... 15 3.2BasicMonteCarloMethods.................... 16 3.3 Extended Monte Carlo Methods ................. 19 3.4 Photo Realistic Rendering ..................... 21 4 Implementation 25 4.1 Ice crystal modelling ........................ 25 4.2 Sunlight modelling ......................... 26 4.3 Parametrization of ice crystal orientation . .......... 27 4.4MonteCarloraytracing...................... 29 5 Application 31 5.1 Initial setup ............................. 31 5.2 22◦ halo simulation ......................... 32 5.3 Parhelion and parhelic circle simulation . .......... 33 5.4 Composite halo simulation ..................... 33 6Conclusion 37 A Reflectance of Dielectrics 41 i ii CONTENTS List of Figures 2.1 22◦ haloattheSouthPoleredrawnfrom[15]........... 6 2.2 Some crystal collected at the South Pole redrawn from [15]. 6 2.3 Frequent halos redrawn from [15]. ................. 7 2.4 Ice crystal and light ray directions redrawn from [5] ...... 7 2.5 Mechanism of 22◦ halos redrawn from [7]. .......... 8 2.6 Deviation angles for 22◦ and 46◦ halos redrawn from [10]. 9 2.7 Refractive index vs. wavelength and temperature redrawn from [4]................................... 10 2.8 22◦ halos and viewing mechanism redrawn from [7]. ...... 11 2.9 Light pass in ice crystal and parhelia photo redrawn from [7]. 12 2.10 Light path for circumzenithal arc and photo redrawn from [7].
    [Show full text]
  • MSE3 Ch22 Atmospheric Optics
    Chapter 22 Copyright © 2011, 2015 by Roland Stull. Meteorology for Scientists and Engineers, 3rd Ed. OptiCs COntents Light can be considered as photon particles or electromagnetic waves, ei- Ray Geometry 833 ther of which travel along paths called Reflection 833 22 rays. To first order, light rays are straight lines Refraction 834 within a uniform transparent medium such as air Huygens’ Principle 837 or water, but can reflect (bounce back) or refract Critical Angle 837 (bend) at an interface between two media. Gradual Liquid-Drop Optics 837 refraction (curved ray paths) can also occur within Primary Rainbow 839 a single medium containing a smooth variation of Secondary Rainbow 840 optical properties. Alexander’s Dark Band 841 Other Rainbow Phenomena 841 The beauty of nature and the utility of physics come together in the explanation of rainbows, halos, Ice Crystal Optics 842 and myriad other atmospheric optical phenomena. Parhelic Circle 844 Subsun 844 22° Halo 845 46° Halo 846 Halos Associated with Pyramid Crystals 847 ray GeOmetry Circumzenith & Circumhorizon Arcs 848 Sun Dogs (Parhelia) 850 Subsun Dogs (Subparhelia) 851 When a monochromatic (single color) light ray Tangent Arcs 851 reaches an interface between two media such as air Other Halos 853 and water, a portion of the incident light from the Scattering 856 air can be reflected back into the air, some can be re- Background 856 fracted as it enters the water (Fig. 22.1), and some can Rayleigh Scattering 857 be absorbed and changed into heat (not sketched). Geometric Scattering 857 Similar processes occur across an air-ice interface.
    [Show full text]
  • Atmospheric Halos
    Atmospheric Halos Rings around the sun and moon and related apparitions in the sky are caused by myriad crystals of ice. Precisely how they are formed is st11l a challenge to modern physics by David K. Lynch }tyone who spends a fair amount of halo and is bilaterally symmetrical with different length and is perpendicular to time outdoors and keeps an eye it. At the top and bottom the two are the plane of the a axes. on the sky is likely to see occa­ tangent. The circumzenith arc appears Although many forms of ice can oc­ sionally a misty ring or halo around the as an inverted rainbow centered on the cur. only about four are important in sun or the moon. The phenomenon is zenith. facing the sun. meteorological optics. The others are well established in folklore as a sign that Many other phenomena of this kind either too rare or do not have smooth. a storm is coming. Actually the halo is have been identified. and I shall describe regular optical faces. The important only one of a number of optical effects a number of them. As the optical effects forms are the plate. which resembles a that arise from the same cause. which is of atmospheric ice crystals are enumer­ hexagonal bathroom tile. the column. the reflection and refraction of light by ated. however. a point is reached where the capped column and the bullet (a col­ crystals of ice in the air. Whenever cir­ their existence and properties become umn with one pyramidal end). rus clouds or ice fogs form.
    [Show full text]
  • A Solar Halo Phenomenon
    Ko. 3911, OcTOBER 14, 1944 NATURE 491 If a body is convex and has area A, it was proved The bands seen by Mr. Archenhold were also seen by Cauchy that A is equal to four times the mean here ; but according to our notes they were coloured, of the area of the projection of the body on a plane even when they passed through the sun. This in­ for all orientations of the latter. This result has a dicates a diffraction origin for the colours. Unfortun­ limited application in the estimation by photographic ately, it was not noticed whether the red or violet or photometric means of the average surface area was nearer the sun ; such an observation would have of a number of small particles suspended in a liquid. distinguished a refraction origin from a diffraction With larger particles such as stones, however, it sug­ origin. We think that Mr. Archenhold's explanation gests that the area of projection should be measured is too simple, since it is geometrically impossible for in a number of different directions by some such a collection of reflecting and refracting elements optical method. The average of these multiplied by between earth and sun to produce a straight band four will give the surface area. In order to give equal of light not passing through the sun, except for un­ weight to each observation it is desirable to choose likely distributions of orientation. the directions of projections to be those of the It is evident that knowledge of atmospheric optics normals to a dodecahedron or an icosahedron.
    [Show full text]
  • Act III, Signature Xvii - (1)
    ...in this part of the West the stars, as I had seen them in Wyoming, are big as roman candles and as lonely as the Prince of the Dharma who's lost his ancestral grove and journeys across the spaces between points in the handle of the Big Dipper, trying to find it again [Jack Kerouac, On The Road (New York: Penguin Books, 1976), p. 222]. III — xvii — What Was Just Finished Was Tremulously Ribald. Lethean photons convert fetches of shimmering zest into fine, generic clinkers. These giant pure snows hit finth comet home, twirling into the guarded Hotspur sphere. Jasmine, in semblance to partial vision, shares the crown inter alia, and both horses nettle actors whirling under total knit troth tenets. Privily their poor heist, a gown blinding to see children, Plair is soon fired between spiritual heart throbs. ~ page 215 ~ toccata Act III, Signature xvii - (1) Main Entry: toc£ca£ta Pronunciation: t„-‚kä-t„ Function: noun Etymology: Italian, from toccare to touch, from (assumed) Vulgar Latin— more at touch Date: circa 1724 : a musical composition usually for organ or harpsichord in a free style and characterized by full chords, rapid runs, and high harmonies. [Following text courtesy of Wikipedia]: Renaissance. The form first appeared in the late Renaissance period. It originated in northern Italy. Several publications of the 1590s include toccatas, by composers like Girolamo Diruta, Adriano Banchieri, Claudio Merulo, Andrea and Giovanni Gabrieli, Luzzasco Luzzaschi and others. These are keyboard compositions in which one hand, and then the other, performs virtuosic runs and brilliant cascading passages against a chordal accompaniment in the other hand.
    [Show full text]
  • 19. Radiation and Optics in the Atmosphere and 19.3 Aerosols and Clouds
    1165 Radiation19. Radiation and Optics in the Atmosphere and 19.3 Aerosols and Clouds ..............................1172 This chapter describes the fundamentals of ra- diation transport in general and in the Earth’s 19.4 Radiation and Climate ..........................1174 atmosphere. The role of atmospheric aerosol and 19.5 Applied Radiation Transport: Remote clouds are discussed and the connections between Sensing of Atmospheric Properties .........1176 radiation and climate are described. Finally, nat- 19.5.1 Trace Gases ................................1176 ural optical phenomena of the atmosphere are 19.5.2 The Fundamentals of DOAS ...........1176 discussed. 19.5.3 Variations of DOAS .......................1178 19.5.4 Atmospheric Aerosols...................1179 19.1 Radiation Transport 19.5.5 Determination of the Distribution in the Earth’s Atmosphere.....................1166 of Solar Photon Path Lengths........1181 19.1.1 Basic Quantities Related 19.6 Optical Phenomena in the Atmosphere...1182 to Radiation Transport .................1166 19.6.1 Characteristics 19.1.2 Absorption Processes ...................1166 of Light Scattering by Molecules 19.1.3 Rayleigh Scattering......................1166 and Particles ..............................1182 19.1.4 Raman Scattering........................1167 19.6.2 Mirages......................................1185 19.1.5 Mie Scattering.............................1168 19.6.3 Clear Sky: 19.2 The Radiation Transport Equation ..........1169 Blue Color and Polarization ..........1186 19.6.4 Rainbows 1187 19.2.1 Sink Terms (Extinction).................1169 ................................... 19.2.2 Source Terms 19.6.5 Coronas, Iridescence and Glories ...1189 19.6.6 Halos 1191 (Scattering and Thermal Emission). 1169 ......................................... 19.2.3 Simplification of the Radiation 19.6.7 The Color of the Sun and Sky ........1193 19.6.8 Clouds and Visibility 1195 Transport Equation......................1170 ...................
    [Show full text]
  • Arctic Ocean 2002
    Arctic Ocean 2002 Journal Notes with Special Emphasis on Birds and Halos Henrik Kylin Department of Environmental Assessment Swedish University of Agricultural Sciences Box 7050 SE-750 07 Uppsala Sweden 2004 Rapport 2004:14 © Henrik Kylin 2004 How then, am I so different from the first men through this way? Like them I left a settled life, I threw it all away To seek a Northwest Passage at the call of many men To find there but the road back home again Stan Rogers Northwest Passage Acknowledgments Sincere thanks to all expedition participants who contributed with observations. Tim Newberger is thanked for an exceptional number of bird reports and interesting discussions on everything from birds to halos and the construction of a violin. Special thanks also to Eric Dyring, Uppsala, who provided literature on halos and to Walt Tape, University of Fairbanks, Alaska, for fruitful discussions of halo phenomena. Thanks are also due to the Swedish Polar Research Secretariat and the officers and crew of the icebreaker Oden for making the expedition possible. Henk Bouwman, Philip Chiverton, Dave Mitchell, and Tim Newberger gave helpful comments on the manuscript at different stages of the writing process. Introduction The purpose of “Arctic Ocean 2002” (AO-02) was to investigate the late winter/early spring conditions in the Fram Strait between Svalbard and Greenland and the East Greenland Sea, particularly the East Greenland Current, with some complementing work in Storfjorden southeast of Svalbard. The East Greenland Current flows southward along the eastern coast of Greenland bringing with it ice far south. To be able to operate at sea in the heavy ice of the High Arctic – during AO-02 we went up to 82° N – you need a powerful icebreaker, and the Swedish icebreaker Oden was used as research platform.
    [Show full text]
  • Downloaded 10/02/21 05:25 PM UTC M
    322 MONTHLY WEATHER REVIEW. JUNE,1920 pressure need not be considered at resent. The range of mounted in a light invar frame (D), in such manner that movement required and freedom from vibration must be changes of length corres onding to changes of tempera- secured by the use of stron elements well supported. ture are engraved upon tB. e record-plate by the style (E). The ap aratus. describe% . herein is su gested as a The strips (T, T) are insulated from their support. btisis for Purther e,xperimental study. It flas not been The inner ends or ed es of the plate-carrier (C)and the constructed, but the princi le of bfr. Dines's smc.essfu1 frame (D), are securef under tension, to spring hinges engraving instrument has R een followed, and essential in the center of the tube (E"), and therefore restrict the parts already have been used to a limited extent in in- motions of the pressure tubes to an arc whose axis is instruments produced by Richard and other manufac- the center of the tube (E"). By this mertns longitudinal turers. Referring to figures 14, 15 and 16, the pressure- movements of tlie pressure tubes are prevented and element (B) is composed of two helical Bourdon tubes there are no pivots with the Tariable friction inevitable secured in a light frame (A), so that their free ends move when Bourdon tubes of this kind are mounted in the in opposite directions when there is a change of pressure. usual way, Another a plication of this device, in the A smgle tube could be used, but the double-tube ele- construction of R simpP e thermograph without pivots, ment 1s preferred.for the reason that thereby may be is shown in figures 17 and 1s.
    [Show full text]
  • 1963: Optical Phenomena in Planetary Meteorology
    Visibility Laboratory- University of California Scripps Institution of Oceanography San Diego 52, California OPTICAL PHENOMENA IN PLANETARY METEOROLOGY •:,:,-.:.-t p: •..-/.L.-. pr.-'Orio Ejj-"--Mye£s•'-'"''•"'" August 1963 SIO Ref. 63-4 Approved: S. Q. Duntley, Director VJ '••. Visibility Laboratory Optical Phenomena in Planetary Meteorology It has recently been suggested by Professor John D, Isaacs, of the Scripps Institution of Oceanography, University of California, San Diego, that significant information concerning the atmospheres of Venus, Mars, and Jupiter might be wrested from terrestrial observa­ tion of their anti-corona, halo, and rainbow phenomena. This report is a compilation, in the form of an annotated bibliography, of avail­ able information concerning what is now known of planetary atmospheres, pertinent optical phenomena in terrestrial meteorology, and the means for acquisition of further data concerning terrestrial and extra­ terrestrial atmospheres. In its outline of a general approach to planetary atmospheric research, the National Research Council Committee on Atmospheric Sciences (NRS-1962) states: "Firstly, it is cheaper to make an observation from the earth, or from a balloon, than it is from a space vehicle. Therefore, during the early phase, every effort should be made to gain knowledge with the aid of suitable terrestrial observations," (Vol. 1, Section 3.4.1) "As observations become available, there will develop an increasing need for experimental and theoretical studies of physical as well as dynamical phenomena and for com­ parisons with results gained from research on our own atmosphere." (Vol. 1, Section 3.4.4) Thus the potential value of further thought and research along these lines is recognized.
    [Show full text]