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Atmospheric Effects Are Looking Up
Atmospheric Effects are Looking Up OASI Workshop 21st May 2018 by Olaf Kirchner Ever seen one of these ? OK, so how about one of these? Atmospheric Effects - caused by sun- or moonlight interacting with liquid water or ice in the air - surprisingly common - always beautiful and one or several phenomena may be seen at the same time - can be in-your-face obvious or very subtle, and ... - ... span the entire sky - a challenge to photograph - very complicated theoretical explanations Effects caused by Liquid Water Droplets - rainbows - glories, Heiligenschein and the Spectre of the Brocken - aureoles / coronae - nacreous / iridescent / Mother-of-Pearl clouds Rainbow Rainbow Ray paths for primary rainbow Ray paths through a spherical water drop Ray paths for secondary rainbow Secondary Rainbow Secondary rainbow Alexander’s Band Supernumerary rainbow Primary rainbow Rainbow Gap in cloud behind observer = partial rainbow Rainbow in spray, Geneva Jet d’Eau Supernumerary Rainbow Interference colours from different lengths of light path Rainbow Circular rainbow seen from an aircraft Rainbows don’t reflect ... Glory Colourful diffraction rings centred on the antisolar point, caused by reflection from spherical droplets Glory ... i.e. centred on where the shadow of your head would be! Brockengespenst = Spectre of the Brocken Taken against fog from Golden Gate Bridge Brocken (1142 m) . Highest point in the Harz mountains Heiligenschein = Halo Antisolar point in hydrothermal steam ... scary stuff Heiligenschein ... i.e. a glory centred on your head -
Atmospheric Phenomena by Feist
Atmospheric optical phenomena An introductory guide by Mike Feist Effects caused by water droplets— rainbows and coronae The most well known optical sky effect is the rainbow. This, as most people know, sometimes occurs when the Sun is out and it is raining. To see a rainbow you must stand with your back to the Sun with the raindrops in front of you. It does not have to be raining where you are standing but in the direction that you are looking. The arc of the primary (main) bow is centred on the antisolar point, the spot directly oppo- site the Sun, and has a radius of 42°. The antisolar point is actually centred on the shadow of your head. If the Sun is rising or setting and therefore on the horizon, the primary rainbow will be a complete semi- circle and the top will be 42° up in the sky. If, on the other hand, the Sun is 42° up in the sky, the primary bow will be on the horizon, the top just rising or setting. Con- ventionally the rainbow is said to have John Constable. Hampstead Heath with a Rainbow (1836). seven colours but all we need to remember seen in the spray near waterfalls and artifi- ous forms but with a six-sided shape. They is that, in the primary bow, the red is on cial rainbows can be made using a garden may be as flat hexagonal plates or long the outside and the blue on the inside. Out- hose. Rainbows are one of the easiest opti- hexagonal prisms or as a combination of side the primary bow sometimes there is cal effects to photograph although they the two. -
Atmospheric Optics
53 Atmospheric Optics Craig F. Bohren Pennsylvania State University, Department of Meteorology, University Park, Pennsylvania, USA Phone: (814) 466-6264; Fax: (814) 865-3663; e-mail: [email protected] Abstract Colors of the sky and colored displays in the sky are mostly a consequence of selective scattering by molecules or particles, absorption usually being irrelevant. Molecular scattering selective by wavelength – incident sunlight of some wavelengths being scattered more than others – but the same in any direction at all wavelengths gives rise to the blue of the sky and the red of sunsets and sunrises. Scattering by particles selective by direction – different in different directions at a given wavelength – gives rise to rainbows, coronas, iridescent clouds, the glory, sun dogs, halos, and other ice-crystal displays. The size distribution of these particles and their shapes determine what is observed, water droplets and ice crystals, for example, resulting in distinct displays. To understand the variation and color and brightness of the sky as well as the brightness of clouds requires coming to grips with multiple scattering: scatterers in an ensemble are illuminated by incident sunlight and by the scattered light from each other. The optical properties of an ensemble are not necessarily those of its individual members. Mirages are a consequence of the spatial variation of coherent scattering (refraction) by air molecules, whereas the green flash owes its existence to both coherent scattering by molecules and incoherent scattering -
Waikīkī Wiki Wiki Wire Apr 29—May 5, 2010
Waikīkī Improvement Association Volume X1, No. 17 Waikīkī Wiki Wiki Wire Apr 29—May 5, 2010 83rd Annual Lei Day Celebration Saturday – May 1, 2010, 9 a.m.—5 p.m. Queen Kapi‘olani Regional Park Bandstand 9:00-10:00 a.m. Royal Hawaiian Band 10:15-11:15 a.m. Investiture Ceremony for the 2010 Lei Queen & Court 11:30 a.m.-12:15 p.m. Kapena 12:30 p.m. Official Opening of the Lei Contest Exhibit by the 2010 Lei Queen & Court (approx 12:30 p.m.) 12:30-1:00 p.m. Na Wahine O Ka Hula Mai Ka Pu‘uwai 1:15-2:00 p.m. Maunalua 2:15-2:45 p.m Polynesian Cultural Center 3:00-3:30 p.m. Halau Hula ‘O Hokulani 3:45-4:00 p.m. Super B. Boy Crew 4:10-4:35 p.m. Kolohe Kai 4:40-5:15 p.m. Nesian N.I.N.E. 5:15-5:30 p.m. Announcements and Closing The Hawaiian Steel Guitar Association will play from 12:15 – 3:00 p.m., in the lei exhibit/ho‘olaule‘a area (open area between the bandstand and the shell). The Lei Contest Exhibit will be open to the public from 12:30-5:30 p.m., in the open area between the bandstand and the shell. Calling all mo‘opuna (grandchildren) - come visit Tutu (grandmother) at Tutu’s Hale from 1:00-5:00 p.m., and hear stories, learn a song, a hula, how to make a lei, and learn how to weave with lauhala. -
The Quest for the Gegenschein Erwin Matys, Karoline Mrazek
The Quest for the Gegenschein Erwin Matys, Karoline Mrazek The sun’s counterglow — or gegenschein — is kind of a stargazers’ legend. Every amateur astronomer has heard about it, only a few of them have actually seen it, and even fewer were lucky enough to capture an image of this dim and ghostlike apparition. As a fellow observer put it: “The gegenschein is certainly not a GOTO-object.” Matter of fact, it isn’t an object at all. But let’s start from the beginning. What exactly is the gegenschein? It is widely known that the space between the planets isn’t empty. The plane of the solar system is filled with an enormous disk of small dust particles with sizes ranging from less than 1/1000 mm up to 1 mm. It is less commonly known that this interplanetary dust cloud is a highly dynamic structure. In contrast to conventional wisdom, it is not an aeon-old leftover from the solar system’s formation. This primordial dust is long gone. Today’s interplanetary dust is — in an astronomical sense of speaking — very young, only millions of years old. Most of the particles originate from quite recent incidents, like asteroid collisions. This is not the gegenschein. The picture shows the zodiacal light, which is closely related to the gegenschein. Here imaged from a rural site, the zodiacal light is a cone of light extending from the sun along the ecliptic, visible after dusk and before dawn. The gegenschein stems from the same dust cloud, but is much harder to detect or photograph. -
Wfc3 Isr 2014
SPACE TELESCOPE SCIENCE INSTITUTE Operated for NASA by AURA Instrument Science Report WFC3 2014-11 The Near Infrared Sky Background N. Pirzkal May 13, 2014 ABSTRACT WFC3 IR observations are often background limited. In the vast majority of cases, when HST is pointed away from the Earth Limb, the main contribution to this background light is caused by zodiacal infrared light, including the Gegenschein, the diffuse glow in the sky centered upon Earth's antisolar point. In this ISR, we present direct measurements of the infrared background levels as observed by WFC3 since its launch and in several broad band filters. We compare our observations to the values currently used in the Exposure Time Calculator (ETC) and derive a model of the IR background levels as a function of Ecliptic Latitude and Sun Angle. Data and Analysis WFC3 IR images have been continuously monitored since the installation of WFC3 on board of HST, as part of the \Blob" Monitoring Program (Pirzkal et al. 2012) and the making of deep sky-flats (Pirzkal et al. 2011). The data that were used and details of the procedures used are given in Pirzkal et al. 2011 and Pirzkal et al. 2012. As part of this routine monitoring, we naturally needed to accurately measure the background level in each of the available infrared exposures. The was done by first generating an object mask using SExtractor for each individual FLT file. This mask was then used to mask out sources in each of the IMSET of the original IMA file and we then computed the background in each IMSET Copyright c 2008 The Association of Universities for Research in Astronomy, Inc. -
Atmospheric Optical Phenomena and Radiative Transfer
ATMOSPHERIC OPTICAL PHENOMENA AND RADIATIVE TRANSFER BY STANLEY DAVID GEDZELMAN AND MICHAEL VOLLMER Sky colors, rainbows, and halos are simulated using models that include light scattered as it passes through clear air and clouds of finite optical depth. ivid rainbows, ice crystal halos, coronas, iridescence, glories, mirages, sky colors, and crepuscular rays have Valways inspired awe and wonder. This makes simulating atmospheric optical phenomena both a scientific and aesthetic undertaking. Atmospheric optics has a venerable history (Pernter and Exner 1922; Minnaert 1993; Humphreys 1940; Tricker 1970; Greenler 1980; Meinel and Meinel 1983; Lynch and Livingston 2001), because the phenomena appear so simple and striking, and because scientists emphasized this branch of atmospheric science at a time when it was far more difficult to examine large-scale weather systems. Discoveries made about or involving the rainbow by Rene Descartes, Isaac Newton, and Thomas Young rank among the early triumphs of the scientific revolution (Boyer 1987). All optical phenomena are produced when air molecules, aerosol particles, or hydrometeors either scatter or absorb light as it passes through the atmosphere. Many of the observed features of the optical phenomena can be reproduced by applying a scattering theory of light to a single particle. This can be done at various levels of complexity. The most accurate and perhaps most intricate Rainbow. " University Corporation for Atmospheric theories involve • i Research, Photo by Carlye Calvin BAH5- AMERICAN METEOROLOGICAL SOCIETY Unauthenticated | DownloadedAPRIL 2008 10/09/21 01:28 AM UTC solving Maxwell's equations with appropriate bound- flattening of drops (Fraser 1983), while models of ary conditions. -
2003 Astronomy Magazine Index
2003 astronomy magazine index Catchall (Martian crater), 11:30 observing Mars from, 7:32 hydrogen, 10:28 Subject index CCD (charge-coupled device) cameras, planets like, 6:48–53 Hydrus (constellation), 10:72–75 3:84–87, 5:84–87 seasons of, 3:72–73 A CCD techniques, 9:100–105 tilt of axis, 2:68, 5:72–73 I accidents, space-related, 7:42–47 Celestron C6-R (refractor), 11:84 EarthExplorer web site, 4:30 Achernar (star), 10:30 iceball, found beyond Pluto, 1:24 Celestron C8-N (reflector), 11:86 eclipses India, plans to visit Moon, 10:29 Advanced Camera for Surveys, 4:28 Celestron CGE-1100 (amateur telescope), in Australia (2003), 4:80–83 ALMA (Atacama Large Millimeter Array), infrared survey, 8:31 11:88 lunar integrating wavelengths, 4:24 3:36 Celestron NexStar 8 GPS (amateur telescope), of 2003, 5:18 Amalthea (Jupiter’s moon), 4:28 interferometry 1:84–87 of May 15, 2003, 5:60, 80–83, 88–89 techniques for, 7:48–53 Amateur Achievement Award, 9:32 Celestron NexStar 8i (amateur telescope), solar Andromeda Galaxy VLT interferometer, 2:32 11:89 of May 31, 2003, 5:80–83, 88–89 International Space Station, 3:31 picture of, 2:12–13 Centaurus A (NGC 5128) galaxy Edgar Wilson Award, 11:30 young stars in, 9:86–89 Internet, virtual observatories on, 9:80–85 1,000 Mira stars discovered in, 10:28 Egg Nebula, 8:36 Intes MK67 (amateur telescope), 11:89 Annefrank (asteroid), 2:32 picture of, 10:12–13 elliptical galaxies, 8:31 antineutrinos, 4:26 Io (Jupiter’s moon), 3:30 ripped apart satellite galaxy, 2:32 Eta Carinae (nebula), 5:29 ISAAC multi-mode instrument, 4:32 antisolar point, 10:18 Centaurus (constellation), 4:74–77 ETX-90EC (amateur telescope), 11:89 Antlia (constellation), 4:74–77 cepheid variable stars, 9:90–91 Europa (Jupiter’s moon), 12:30, 77 aphelion, 6:68–69 Challenger (space shuttle), 7:42–47 exoplanet magnetosphere, 11:28 J Apollo 1 (spacecraft), 7:42–47 J002E3 satellite, 1:30 Chamaeleon (constellation), 12:80–83 extrasolar planets. -
The Isophote Maps of the Gegenschein Obtained by CCD Observations
Earth Planets Space, 50, 477–480, 1998 The isophote maps of the Gegenschein obtained by CCD observations Masateru Ishiguro1, Hideo Fukushima2, Daisuke Kinoshita3, Tadashi Mukai1, Ryosuke Nakamura4, Jun-ichi Watanabe2, Takeshi Watanabe1, and John F. James5 1The Graduate School of Science and Technology, Kobe University, Kobe 657-8501, Japan 2National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan 3Department of Physics, Faculty of Science, Tohoku University, Sendai 980-77, Japan 4Information Processing Center, Kobe University, Nada, Kobe 657-8501, Japan 529, Merchants’ Quay, Salford, M5 2XF, England (Received December 8, 1997; Revised January 16, 1998; Accepted February 3, 1998) We summarize the results of our Gegenschein observations at Norikura (altitude 2876 m, Japan) in Sept. 18, 1996, and at Kiso (altitude 1130 m, Japan) in Feb. 9–14, and March 4 and 5,1997. The instrument consisting of fish-eye lens or the wide angle lens attached to the cooled CCD camera was used with green filter. It is found that the position of the maximum brightness near the antisolar point (the Gegenschein) is slightly deviated approximately 0.◦4 from the antisolar point to the south in September, whereas nearly 0.◦7 to the north in February/March. Furthermore, a gradient of the relative intensity along a line perpendicular to the ecliptic is remarkably different with changing seasons, i.e. the brightness decreases faster towards the north in September, in contrast with its quick decrease towards the south in February/March. Our observed evidence suggests that these variations of the peak position and the brightness gradient of the Gegenschein are caused by the annual motion of the Earth with respect to the plane of the zodiacal cloud, and does not conflict with the predictions deduced from the cloud model having its symmetric plane beyond the Earth’s orbit coinciding with the invariable plane of the solar system. -
TAG , Grades K
Subject: TAG Grade: K,1,2 Note: TAG instruction occurs one day a week for each student. These plans are meant to replace the time that would be spent on core learning activities (reading, ELA/writing, math social studies/science) for that one day each week. Students should still complete activities for specials classes (art, music, PE) on their TAG day. Week 4 Standards (include both TAG standards S1E1. Obtain, evaluate, and communicate weather data to and grade level standards addressed) identify weather patterns S1P1. Obtain, evaluate, and communicate information to investigate light and sound. TAG Creative Thinking and Problem Solving Gifted students demonstrate skills in fluency, flexibility, elaboration and originality to generate innovative ideas, products, and/or solutions to problem. Brief Description During this lesson, students will learn about moonbows. They will begin by reading an article on moonbows and answering a discussion question to practice fluency and originality. Students will then complete a CSI handout to practice flexibility, elaboration, and originality. Students may complete an optional experiment using a glass of water and a piece of paper. Student Directions: 1. Read the Wonderopolis article on Moonbows. Adapted from https://wonderopolis.org/wonder/how-rare-is-a-moonbow 2. Discussion question: If there's a pot of gold at the end of a rainbow made by the sun, what do you think would await you at the end of a moonbow? Come up with a list of at least three different possibilities of things that might be found at the end of a moonbow. Share your list with a friend or family member. -
RAINBOWS Written by Peg Zenko with Special Edit by Les Cowley
The Weather Observers Guide to RAINBOWS Written by Peg Zenko with special edit by Les Cowley Even after the most destructive thunderstorms have just passed, the sky can display a bright, stunning blend of colors in the graceful, perfectly circular arc of a rainbow. The subject of song, verse and Biblical prophecy, rainbows are associated with light and peace. Many cultures have myths surrounding the rainbow. In Norse, it is called Bifrost (The Trembling Roadway). They are the easiest of atmospheric optic phenomena to spot, even though they occur in our observing area roughly an average of only 5% as often as the common 22-degree solar halo. The first step in spotting rainbows is to recognize sky colors that are commonly mistaken for rainbows. The solar halo (left) is sometimes mistaken for a rainbow because it displays similar colors, and is also circular. The halo, however, appears around the sun, in a radial arc of 22 degrees, and the much larger rainbow is always opposite the sun. Another difference is that the red band of the halo Continued (RAINBOWS continued) appears on the inner circumference of the circle, and red is on the outside of the rainbow. Another misconception is that a very frequent colorful solar companion, the sundog, is a little piece of rainbow. Sundogs (right) also appear near the 22-degree radius halo. In this instance it’s difficult to detect an arc, but the obvious clue is that it is near the sun. The optic phenomena that most closely resembles a rainbow is the circumzenithal arc, or CZA. -
The Fall Sky by Dr
The Fall Sky by Dr. Arthur Babcock Planets Leonids on 17 November and the Geminids on 14 December, will be washed out by the Moon. Mercury will be visible in the western evening sky from the start of the quarter through early November. It Comets then becomes lost in the glare of the Sun, but take heart: Comet C/2018 W2 (Africano) is predicted to be at on 11 November there will be a transit of Mercury, the 8th magnitude (i.e., visible in binoculars) for the first part of first since 2016. On the Central Coast, we will miss the the season. C/2017 T2 (PanSTARRS) may brighten to 9th beginning of the transit, which begins before sunrise. The magnitude in December and 8th magnitude in earlt 2020. moment of greatest transit occurs at about 7:20am, and by Seiichi Yoshida’s Home Page (www.aerith.net) is a good 10:03, the transit will be over. Because the disc of the place to get finder charts and other information on comets. planet as seen from Earth is so small (much smaller than the disc of Venus during a transit), observing the transit of Eclipses Mercury requires a telescope with a magnification of at No eclipses will be visible from the Central Coast least 50x. Since the telescope will be pointed squarely during this quarter. There will be an annular solar eclipse on at the Sun, a proper solar filter is an absolute require- 26 December, but it won’t be visible from these parts. ment. After the transit, the planet becomes visible in the Interplanetary Dust morning sky from late November until the end of the period.