Why the Sky Is Blue by John A
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12 Light Scattering AQ1
12 Light Scattering AQ1 Lev T. Perelman CONTENTS 12.1 Introduction ......................................................................................................................... 321 12.2 Basic Principles of Light Scattering ....................................................................................323 12.3 Light Scattering Spectroscopy ............................................................................................325 12.4 Early Cancer Detection with Light Scattering Spectroscopy .............................................326 12.5 Confocal Light Absorption and Scattering Spectroscopic Microscopy ............................. 329 12.6 Light Scattering Spectroscopy of Single Nanoparticles ..................................................... 333 12.7 Conclusions ......................................................................................................................... 335 Acknowledgment ........................................................................................................................... 335 References ...................................................................................................................................... 335 12.1 INTRODUCTION Light scattering in biological tissues originates from the tissue inhomogeneities such as cellular organelles, extracellular matrix, blood vessels, etc. This often translates into unique angular, polari- zation, and spectroscopic features of scattered light emerging from tissue and therefore information about tissue -
Arxiv:2008.11688V1 [Astro-Ph.CO] 26 Aug 2020
APS/123-QED Cosmology with Rayleigh Scattering of the Cosmic Microwave Background Benjamin Beringue,1 P. Daniel Meerburg,2 Joel Meyers,3 and Nicholas Battaglia4 1DAMTP, Centre for Mathematical Sciences, Wilberforce Road, Cambridge, UK, CB3 0WA 2Van Swinderen Institute for Particle Physics and Gravity, University of Groningen, Nijenborgh 4, 9747 AG Groningen, The Netherlands 3Department of Physics, Southern Methodist University, 3215 Daniel Ave, Dallas, Texas 75275, USA 4Department of Astronomy, Cornell University, Ithaca, New York, USA (Dated: August 27, 2020) The cosmic microwave background (CMB) has been a treasure trove for cosmology. Over the next decade, current and planned CMB experiments are expected to exhaust nearly all primary CMB information. To further constrain cosmological models, there is a great benefit to measuring signals beyond the primary modes. Rayleigh scattering of the CMB is one source of additional cosmological information. It is caused by the additional scattering of CMB photons by neutral species formed during recombination and exhibits a strong and unique frequency scaling ( ν4). We will show that with sufficient sensitivity across frequency channels, the Rayleigh scattering/ signal should not only be detectable but can significantly improve constraining power for cosmological parameters, with limited or no additional modifications to planned experiments. We will provide heuristic explanations for why certain cosmological parameters benefit from measurement of the Rayleigh scattering signal, and confirm these intuitions using the Fisher formalism. In particular, observation of Rayleigh scattering P allows significant improvements on measurements of Neff and mν . PACS numbers: Valid PACS appear here I. INTRODUCTION direction of propagation of the (primary) CMB photons. There are various distinguishable ways that cosmic In the current era of precision cosmology, the Cosmic structures can alter the properties of CMB photons [10]. -
RAL COLOR CHART ***** This Chart Is to Be Used As a Guide Only. Colors May Appear Slightly Different ***** Green Beige Purple V
RAL COLOR CHART ***** This Chart is to be used as a guide only. Colors May Appear Slightly Different ***** RAL 1000 Green Beige RAL 4007 Purple Violet RAL 7008 Khaki Grey RAL 4008 RAL 7009 RAL 1001 Beige Signal Violet Green Grey Tarpaulin RAL 1002 Sand Yellow RAL 4009 Pastel Violet RAL 7010 Grey RAL 1003 Signal Yellow RAL 5000 Violet Blue RAL 7011 Iron Grey RAL 1004 Golden Yellow RAL 5001 Green Blue RAL 7012 Basalt Grey Ultramarine RAL 1005 Honey Yellow RAL 5002 RAL 7013 Brown Grey Blue RAL 1006 Maize Yellow RAL 5003 Saphire Blue RAL 7015 Slate Grey Anthracite RAL 1007 Chrome Yellow RAL 5004 Black Blue RAL 7016 Grey RAL 1011 Brown Beige RAL 5005 Signal Blue RAL 7021 Black Grey RAL 1012 Lemon Yellow RAL 5007 Brillant Blue RAL 7022 Umbra Grey Concrete RAL 1013 Oyster White RAL 5008 Grey Blue RAL 7023 Grey Graphite RAL 1014 Ivory RAL 5009 Azure Blue RAL 7024 Grey Granite RAL 1015 Light Ivory RAL 5010 Gentian Blue RAL 7026 Grey RAL 1016 Sulfer Yellow RAL 5011 Steel Blue RAL 7030 Stone Grey RAL 1017 Saffron Yellow RAL 5012 Light Blue RAL 7031 Blue Grey RAL 1018 Zinc Yellow RAL 5013 Cobolt Blue RAL 7032 Pebble Grey Cement RAL 1019 Grey Beige RAL 5014 Pigieon Blue RAL 7033 Grey RAL 1020 Olive Yellow RAL 5015 Sky Blue RAL 7034 Yellow Grey RAL 1021 Rape Yellow RAL 5017 Traffic Blue RAL 7035 Light Grey Platinum RAL 1023 Traffic Yellow RAL 5018 Turquiose Blue RAL 7036 Grey RAL 1024 Ochre Yellow RAL 5019 Capri Blue RAL 7037 Dusty Grey RAL 1027 Curry RAL 5020 Ocean Blue RAL 7038 Agate Grey RAL 1028 Melon Yellow RAL 5021 Water Blue RAL 7039 Quartz Grey -
Best Plants for Problem Clay Soils: Perennials
Visit us on the Web: www.gardeninghelp.org Best Plants for Problem Clay Soils: Perennials Perennials Amsonia tabernaemontana — Bluestar This Missouri native features uptight clusters of light blue star-like flowers in late spring. Its narrow willow-like leaves turn yellow to peach-colored in fall. Bluestar may require staking if grown in shade and may be pruned after flowering to maintain a compact shape. It is most attractive when grown massed, in native plant gardens, shade gardens, open woodland areas, and borders. Asclepias incarnata — Swamp milkweed Despite its common name and native habitat, swamp milkweed may be grown in the average garden. Its fragrant white, pink or mauve flowers attract butterflies and mature into slender pods with silky-haired seeds. Swamp milkweed is a good choice for sunny, low or moist areas such as stream or pond banks, borders, and butterfly gardens. Baptisia australis — Blue false indigo Blue false indigo has beautiful purplish blue lupine-like flowers borne in erect spikes above the trifoliate leaves. The flowers mature into black seed pods that rattle in the breeze and are an interesting addition to dried flower arrangements. This herbaceous perennial does best in full sun as plants grown in part shade may grow taller and need support. Due to an extensive root system, blue false indigo will tolerate drought, but it should not be disturbed once it is established. Attractive in almost any situation including borders, prairies, cottage gardens, and native plant gardens, this plant is best used as a single specimen plant or in small groups. Baptisia australis var. -
Rayleigh Scattering by Gas Molecules: Why Is the Sky Blue?
Please do not remove this manual from from the lab. It is available via Canvas DEMO NOTES: This manual contains demonstrator notes in blue italics Optics Rayleigh Scattering: 12 hrs Rayleigh scattering by gas molecules: why is the sky blue? Objectives After completing this experiment: • You will be familiar with using a photomultiplier tube) as a means of measuring low intensities of light; • You will have had experience of working safely with a medium power laser producing visible wavelength radiation; • You will have had an opportunity to use the concept of solid angle in connection with scattering experiments; • You will have had the opportunity to experimentally examine the phenomenon of polarization; • You should understand how the scattering of light from molecules varies accord- ing to the direction of polarization of the light and the scattering angle relative to it; • You should have a good understanding of what is meant by cross-section and differential cross section. • You should be able to describe why the daytime sky appears to be blue and why light from the sky is polarized. Note the total time for data-taking in this experiment is about one hour. There are a lot of useful physics concepts to absorb in the background material. You should read the manual bearing in mind that you need to thoroughly understand how you will calculate your results from you measurements BEFORE your final lab session. This is an exercise in time management. Safety A medium power Argon ion laser is used in this experiment. The light from it is potentially dangerous to you and other people in the room. -
Indigo: Sources, Processes and Possibilities for Bioregional Blue
Indigo: Sources, processes and possibilities for bioregional blue Nicholas Wenner and Matthew Forkin June 2017 Photo by Kalie Cassel-Feiss by Kalie Photo Table of Contents Introduction . .3 Indigo . .4 The Indigo Process . 11 Conclusions . 15 Photo by Paige Green Green by Paige Photo Indigo Overview 2 Introduction his report was completed with funding generously provided by the Jena and Michael King TFoundation as part of Fibershed’s True Blue project . It is one project of many that support Fibershed’s larger mission: “Fibershed develops regional and regenerative fiber systems on behalf of independent working producers, by expanding opportunities to implement carbon farming, forming catalytic foundations to rebuild regional manufacturing, and through connecting end-users to farms and ranches through public education.” In this report we present the various sources of blue dye and of indigo, and motivate the use of plant-based indigo in particular . We also identify the limitations of natural dyes like indigo and the need for larger cultural and systemic shifts . The ideal indigo dye production system would be a closed-loop system that moves from soil to dye to textiles and back to soil . The indigo process has three basic steps: planting, harvesting, and dye extraction . In this document, we provide an overview of each, and detailed explorations are given in two separate documents that will be available through Fibershed by late-summer 2017 . This report is based on a literature review of academic research, natural dye books, online content, and personal interviews . It benefited greatly from conversations with (and the generosity of) many skilled artisans and natural dyers, including Rowland Ricketts, Jane Palmer, and Kori Hargreaves . -
A Study on Numerical Integration Methods for Rendering Atmospheric
Open Phys. 2019; 17:241–249 Research Article Tomasz Gałaj and Adam Wojciechowski A study on numerical integration methods for rendering atmospheric scattering phenomenon https://doi.org/10.1515/phys-2019-0025 In this paper, a qualitative comparison of three, pop- Received Jan 29, 2019; accepted Mar 07, 2019 ular numerical integration methods to compute the sin- gle scattering integral is presented. In provided research, Abstract: A qualitative comparison of three, popular and three methods have been chosen, namely Midpoint, Trape- most widely known numerical integration methods in zoidal and Simpson’s Rules. These three methods are fairly terms of atmospheric single scattering calculations is pre- popular in Computer Graphics field. Atmospheric scatter- sented. A comparison of Midpoint, Trapezoidal and Simp- ing is calculated using backward ray tracing algorithm tak- son’s Rules taking into account quality of a clear sky gener- ing into account variable light conditions [5]. Then, these ated images is performed. Methods that compute the atmo- methods are compared with each other taking into account spheric scattering integrals use Trapezoidal Rule. Authors quality of the generated images of the sky. As a subproduct try to determine which numerical integration method is of this research, the fidelity of the framework presented the best for determining the colors of the sky and check by Bruneton in [3] is being checked. Authors try to deter- if Trapezoidal Rule is in fact the best choice. The research mine which numerical integration method is the best for does not only conduct experiments with Bruneton’s frame- calculating the colors of the sky and check if Trapezoidal work but also checks which of the selected numerical inte- Rule is in fact the best choice. -
Opaque Colors
When glazing, it helps to know which colors are transparent and which are opaque. Whether a particular color is transparent or opaque has to do simply with its inherent chemical makeup. An opaque color will offer more coverage than a transparent one; that much is obvious. But it is important to remember that opacity and transparency have nothing to do with color saturation/intensity or color permanence. Both groups contain fugitive colors as well as powerful ones (red can fade quickly in UV light; blue used in even small quantities will turn the mixture strongly blue). This list is provided to help you determine which colors are best used for underpainting, which are best for glazing right out of the tube, and which may require the use of a glazing medium. Opaque Oil Colors Transparent Oil Colors Whites Whites lead white zinc white titanium white transparent white Yellows Yellows cadmium yellow (all tones) aureolin (cobalt yellow) Naples yellow Indian yellow yellow ochre transparent gold ochre jaune brilliant transparent oxide yellow nickel titanate yellow stil de grain jaune Reds and Oranges Reds and Oranges cadmium red (light and dark) alizarin crimson cadmium orange rose madder (light and dark) English red ultramarine red Mars red quinacridone red Venetian red quinacridone burnt orange terra rosa transparent red oxide vermillion naphthol scarlet anthraquinoid red perinone orange Greens Greens chromium green oxide viridian permanent green phthalo green cadmium green phthalo turquoise green gold terre verte Browns Browns burnt umber burnt sienna raw umber raw sienna Pozzuoli earth brown madder alizarin transparent brown stil de grain brun Blues Blues cerulean blue ultramarine blue cobalt blue phthalo blue manganese blue indanthrone blue indigo Violets Violets cadmium purple cobalt violet Mars violet manganese violet caput mortuum violet carbazole violet quinacridone violet rose dore’ dioxazine purple Blacks and Neutrals Blacks and Neutrals lamp black ivory black peach black Davy’s gray Mars black Paynes gray . -
Ozone: Twilit Skies, and (Exo-)Planet Transits
Astronomical Science Ozone: Twilit Skies, and (Exo-)planet Transits Robert Fosbury1 the atmosphere, can be rich and varied. This article is about the effect of ozone George Koch 2 The processes that result in this palette on the colour of the twilit sky and, in the Johannes Koch 2 are geometrically complex, but comprise same vein, its appearance as the strong- a limited number of now well-understood est telluric absorption feature in the visi- physical effects. This understanding was ble spectrum of the Earth as it would be 1 ESO not gained easily. From the time when seen by a distant observer watching it 2 Lycée Français Jean Renoir, München, early humans first consciously posed the transit in front of the Sun. We present and Germany question: “What makes the sky blue?”, to analyse spectrophotometric observations the time when the processes of scatter- of sunset and also discuss observations ing by molecules and molecular density of the eclipsed Moon reported by Pallé et Although only a trace constituent gas fluctuations were elucidated, thousands al. (2009). in the Earth’s atmosphere, ozone plays of years passed, during which increas- a critical role in protecting the Earth’s ingly intensive experiments and theories surface from receiving a damaging flux were developed and carried out (Pesic, Ozone of solar ultraviolet radiation. What is not 2005). generally appreciated, however, is that Ozone (O3 or trioxygen) is an unstable the intrinsically weak, visible Chappuis Most physicists, if asked why the sky is allotrope of oxygen that most people can absorption band becomes an important blue, would answer with little hesitation: detect by smell at concentrations as influence on the colour of the entire sky “Because of Rayleigh scattering by mole low as 0.01 parts per million (ppm). -
An Attempt to Detect Rayleigh Scattering in the Atmospheres of Extrasolar Planets Using a Ground-Based Telescope
Wesleyan University Blue Skies Through a Blue Sky: An Attempt To Detect Rayleigh Scattering in the Atmospheres of Extrasolar Planets Using a Ground-Based Telescope by Kristen Luchsinger A thesis submitted to the faculty of Wesleyan University in partial fulfillment of the requirements for the Degree of Master of Arts in Astronomy with a Planetary Science Concentration Middletown, Connecticut April, 2017 Acknowledgements I would like to thank the Astronomy department at Wesleyan University, which has been incredibly supportive during my time here. Both the faculty and the stu- dent community have been both welcoming and encouraging, and always pushed me to learn more than I thought possible. I would especially like to thank Avi Stein and Hannah Fritze, who first made me feel welcome in the department, and Girish Duvurri and Rachel Aranow, who made the department a joyful place to be. They, along with Wilson Cauley, were always willing to talk through any issues I encountered with me, and I am sure I would not have produced nearly as polished a product without their help. I would also like to thank the telescope operators, staff, and fellow observers from the time I spent at Kitt Peak National Observatory. Through their support and friendliness, they turned what could have been an overwhelming and fright- ening experience into a successful and enjoyable first ever solo observing run. I would like to thank my advisor, Seth Redfield, for his constant support and encouragement. Despite leading three undergraduate and one graduate student through four theses on three different topics, Seth kept us all moving forward, usually even with a smile and constant, genuine enthusiasm for the science. -
Scattering and Polarization
Scattering and Polarization C HAP T E R 13 13.1 these two molecules interferes de 1 3.2 INTRODUCTION structively. as in Figure 12.4 (along RAYLEIGH SCATTERING the x-axis). and this Is so for any - sideways direction from which you - So far we have considered what look at the beam. Air. on the other When white light scatters from hap pens when light encounters ma hand, is a gas. so there is no guar some molecules. it scatters selec terial obstacles of a size much antee that there will be another tively because part of the light is ab greater than the wavelength (geo molecule half a wavelength beyond sorbed at the resonant frequ encies metrical optics) or of a size so small the first-sometimes there may be a of the molecules-the scattered as to be comparable with the wave few extra molecules around one light Is then colored. For man y length of light (wave optics). But point, sometimes a few less. You see other molecules. however, the im you can also observe effects due the scattering from these pOints be portant resonant frequenCies are to even smaller obstacles, much cause of these fluctuations. (The significantly higher than visible fre smaller than the wavelength of visi TRY IT suggests ways to enhance quencies. White light nevertheless ble light. When light interacts with the scattering in air.) becomes colored when it scatters an isolated object that small, it Scattering is selective in several from these molecules-the higher shakes all the charges in the object, ways: light of certain wavelengths the frequency of the incident light. -