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Planet Positions: 1 Planet Positions
Planet Positions: 1 Planet Positions As the planets orbit the Sun, they move around the celestial sphere, staying close to the plane of the ecliptic. As seen from the Earth, the angle between the Sun and a planet -- called the elongation -- constantly changes. We can identify a few special configurations of the planets -- those positions where the elongation is particularly noteworthy. The inferior planets -- those which orbit closer INFERIOR PLANETS to the Sun than Earth does -- have configurations as shown: SC At both superior conjunction (SC) and inferior conjunction (IC), the planet is in line with the Earth and Sun and has an elongation of 0°. At greatest elongation, the planet reaches its IC maximum separation from the Sun, a value GEE GWE dependent on the size of the planet's orbit. At greatest eastern elongation (GEE), the planet lies east of the Sun and trails it across the sky, while at greatest western elongation (GWE), the planet lies west of the Sun, leading it across the sky. Best viewing for inferior planets is generally at greatest elongation, when the planet is as far from SUPERIOR PLANETS the Sun as it can get and thus in the darkest sky possible. C The superior planets -- those orbiting outside of Earth's orbit -- have configurations as shown: A planet at conjunction (C) is lined up with the Sun and has an elongation of 0°, while a planet at opposition (O) lies in the opposite direction from the Sun, at an elongation of 180°. EQ WQ Planets at quadrature have elongations of 90°. -
Sun Tool Options
Sun Study Tools Sophomore Architecture Studio: Lighting Lecture 1: • Introduction to Daylight (part 1) • Survey of the Color Spectrum • Making Light • Controlling Light Lecture 2: • Daylight (part 2) • Design Tools to study Solar Design • Architectural Applications Lecture 3: • Light in Architecture • Lighting Design Strategies Sun Tool Options 1. Paper and Pencil 2. Build a Model 3. Use a Computer The first step to any of these options is to define…. Where is the site? 1 2 Sun Study Tools North Latitude and Longitude South Longitude Latitude Longitude Sun Study Tools North America Latitude 3 United States e ud tit La Sun Study Tools New York 72w 44n 42n Site Location The site location is specified by a latitude l and a longitude L. Latitudes and longitudes may be found in any standard atlas or almanac. Chart shows the latitudes and longitudes of some North American cities. Conventions used in expressing latitudes are: Positive = northern hemisphere Negative = southern hemisphere Conventions used in expressing longitudes are: Positive = west of prime meridian (Greenwich, United Kingdom) Latitude and Longitude of Some North American Cities Negative = east of prime meridian 4 Sun Study Tools Solar Path Suns Position The position of the sun is specified by the solar altitude and solar azimuth and is a function of site latitude, solar time, and solar declination. 5 Sun Study Tools Suns Position The rotation of the earth about its axis, as well as its revolution about the sun, produces an apparent motion of the sun with respect to any point on the altitude earth's surface. The position of the sun with respect to such a point is expressed in terms of two angles: azimuth The sun's position in terms of solar altitude (a ) and azimuth (a ) solar azimuth, which is the t s with respect to the cardinal points of the compass. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Equatorial and Cartesian Coordinates • Consider the Unit Sphere (“Unit”: I.E
Coordinate Transforms Equatorial and Cartesian Coordinates • Consider the unit sphere (“unit”: i.e. declination the distance from the center of the (δ) sphere to its surface is r = 1) • Then the equatorial coordinates Equator can be transformed into Cartesian coordinates: right ascension (α) – x = cos(α) cos(δ) – y = sin(α) cos(δ) z x – z = sin(δ) y • It can be much easier to use Cartesian coordinates for some manipulations of geometry in the sky Equatorial and Cartesian Coordinates • Consider the unit sphere (“unit”: i.e. the distance y x = Rcosα from the center of the y = Rsinα α R sphere to its surface is r = 1) x Right • Then the equatorial Ascension (α) coordinates can be transformed into Cartesian coordinates: declination (δ) – x = cos(α)cos(δ) z r = 1 – y = sin(α)cos(δ) δ R = rcosδ R – z = sin(δ) z = rsinδ Precession • Because the Earth is not a perfect sphere, it wobbles as it spins around its axis • This effect is known as precession • The equatorial coordinate system relies on the idea that the Earth rotates such that only Right Ascension, and not declination, is a time-dependent coordinate The effects of Precession • Currently, the star Polaris is the North Star (it lies roughly above the Earth’s North Pole at δ = 90oN) • But, over the course of about 26,000 years a variety of different points in the sky will truly be at δ = 90oN • The declination coordinate is time-dependent albeit on very long timescales • A precise astronomical coordinate system must account for this effect Equatorial coordinates and equinoxes • To account -
Radar Remote Sensing of Pyroclastic Deposits in the Southern Mare Serenitatis and Mare Vaporum Regions of the Moon Lynn M
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 114, E11004, doi:10.1029/2009JE003406, 2009 Click Here for Full Article Radar remote sensing of pyroclastic deposits in the southern Mare Serenitatis and Mare Vaporum regions of the Moon Lynn M. Carter,1 Bruce A. Campbell,1 B. Ray Hawke,2 Donald B. Campbell,3 and Michael C. Nolan4 Received 21 April 2009; revised 12 July 2009; accepted 3 August 2009; published 5 November 2009. [1] We use polarimetric radar observations to study the distribution, depth, and embedded rock abundance of nearside lunar pyroclastic deposits. Radar images were obtained for Mare Vaporum and the southern half of Mare Serenitatis; the imaged areas contain the large Rima Bode, Mare Vaporum, Sulpicius Gallus, and Taurus-Littrow pyroclastic deposits. Potential pyroclastic deposits at Rima Hyginus crater, the Tacquet Formation, and a dome in Mare Vaporum are also included. Data were acquired at S band (12.6 cm wavelength) using Arecibo Observatory and the Green Bank Telescope in a bistatic configuration. The S band images have resolutions between 20 and 100 m/pixel. The pyroclastic deposits appear dark to the radar and have low circular polarization ratios at S band wavelengths because they are smooth, easily penetrable by radar waves, and generally contain few embedded blocks. Changes in circular polarization ratio (CPR) across some of the pyroclastic deposits show areas with increased rock abundance as well as deposits that are shallower. Radar backscatter and CPR maps are used to identify fine-grained mantling deposits in cases where optical and near-infrared data are ambiguous about the presence of pyroclastics. -
10Great Features for Moon Watchers
Sinus Aestuum is a lava pond hemming the Imbrium debris. Mare Orientale is another of the Moon’s large impact basins, Beginning observing On its eastern edge, dark volcanic material erupted explosively and possibly the youngest. Lunar scientists think it formed 170 along a rille. Although this region at first appears featureless, million years after Mare Imbrium. And although “Mare Orien- observe it at several different lunar phases and you’ll see the tale” translates to “Eastern Sea,” in 1961, the International dark area grow more apparent as the Sun climbs higher. Astronomical Union changed the way astronomers denote great features for Occupying a region below and a bit left of the Moon’s dead lunar directions. The result is that Mare Orientale now sits on center, Mare Nubium lies far from many lunar showpiece sites. the Moon’s western limb. From Earth we never see most of it. Look for it as the dark region above magnificent Tycho Crater. When you observe the Cauchy Domes, you’ll be looking at Yet this small region, where lava plains meet highlands, con- shield volcanoes that erupted from lunar vents. The lava cooled Moon watchers tains a variety of interesting geologic features — impact craters, slowly, so it had a chance to spread and form gentle slopes. 10Our natural satellite offers plenty of targets you can spot through any size telescope. lava-flooded plains, tectonic faulting, and debris from distant In a geologic sense, our Moon is now quiet. The only events by Michael E. Bakich impacts — that are great for telescopic exploring. -
Location #1: Peary/Whipple Crater
Location, Location, Location A Lunar Investment Strategy Hoyt Davidson Near Earth LLC June 2017 ISU's International Institute of Space Commerce Lunar Economic Action Plan (LEAP) Space and Questions from 1960 Still Relevant Today Economic Development • How can we utilize our dynamic system of competitive private enterprise in space, as on earth, to make newly discovered resources useful to man? • How can private enterprise and private capital make their maximum contribution? Philosophy and Policy The ultimate goal is not to impress others, or merely to explore our planetary system, but to use accessible space for the benefit of humankind. It is a goal that is not confined to a decade or a century. Nor is it confined to a single nearby destination, or to a fleeting dash to plant a flag. The idea is to begin preparing now for a future in which the material trapped in the Sun's vicinity is available for incorporation into our way of life. Dr. John Marburger, Head of the Office of Science and Technology Policy 2006 3 The Investment Premise • Just as on Earth, lunar real estate “value” is driven by location, location, location Rank Location Why Valuable 1 Peary Crater Best 1st industrial base and settlement 2 Sinus Medii Good cargo port & space elevator site 3 Largest skylights / lava tubes Best large scale settlements 4 Tsiolkovskiy crater, dark side Prime radio astronomy site 5 High helium-3 concentrations Potential high value mining 6 Lipsky Crater Space elevator site for Earth-Moon L2 7 Aristillus High Thorium concentrations • Lunar real -
List of Targets for the Lunar II Observing Program (PDF File)
Task or Task Description or Target Name Wood's Rükl Target LUNAR # 100 Atlas Catalog (chart) Create a sketch/map of the visible lunar surface: 1 Observe a Full Moon and sketch a large-scale (prominent features) L-1 map depicting the nearside; disk of visible surface should be drawn 2 at L-1 3 least 5-inches in diameter. Sketch itself should be created only by L-1 observing the Moon, but maps or guidebooks may be used when labeling sketched features. Label all maria, prominent craters, and major rays by the crater name they originated from. (Counts as 3 observations (OBSV): #1, #2 & #3) Observe these targets; provide brief descriptions: 4 Alpetragius 55 5 Arago 35 6 Arago Alpha & Arago Beta L-32 35 7 Aristarchus Plateau L-18 18 8 Baco L-55 74 9 Bailly L-37 71 10 Beer, Beer Catena & Feuillée 21 11 Bullialdus, Bullialdus A & Bullialdus B 53 12 Cassini, Cassini A & Cassini B 12 13 Cauchy, Cauchy Omega & Cauchy Tau L-48 36 14 Censorinus 47 15 Crüger 50 16 Dorsae Lister & Smirnov (A.K.A. Serpentine Ridge) L-33 24 17 Grimaldi Basin outer and inner rings L-36 39, etc. 18 Hainzel, Hainzel A & Hainzel C 63 19 Hercules, Hercules G, Hercules E 14 20 Hesiodus A L-81 54, 64 21 Hortensius dome field L-65 30 22 Julius Caesar 34 23 Kies 53 24 Kies Pi L-60 53 25 Lacus Mortis 14 26 Linne 23 27 Lamont L-53 35 28 Mairan 9 29 Mare Australe L-56 76 30 Mare Cognitum 42, etc. -
3.- the Geographic Position of a Celestial Body
Chapter 3 Copyright © 1997-2004 Henning Umland All Rights Reserved Geographic Position and Time Geographic terms In celestial navigation, the earth is regarded as a sphere. Although this is an approximation, the geometry of the sphere is applied successfully, and the errors caused by the flattening of the earth are usually negligible (chapter 9). A circle on the surface of the earth whose plane passes through the center of the earth is called a great circle . Thus, a great circle has the greatest possible diameter of all circles on the surface of the earth. Any circle on the surface of the earth whose plane does not pass through the earth's center is called a small circle . The equator is the only great circle whose plane is perpendicular to the polar axis , the axis of rotation. Further, the equator is the only parallel of latitude being a great circle. Any other parallel of latitude is a small circle whose plane is parallel to the plane of the equator. A meridian is a great circle going through the geographic poles , the points where the polar axis intersects the earth's surface. The upper branch of a meridian is the half from pole to pole passing through a given point, e. g., the observer's position. The lower branch is the opposite half. The Greenwich meridian , the meridian passing through the center of the transit instrument at the Royal Greenwich Observatory , was adopted as the prime meridian at the International Meridian Conference in 1884. Its upper branch is the reference for measuring longitudes (0°...+180° east and 0°...–180° west), its lower branch (180°) is the basis for the International Dateline (Fig. -
1 the Equatorial Coordinate System
General Astronomy (29:61) Fall 2013 Lecture 3 Notes , August 30, 2013 1 The Equatorial Coordinate System We can define a coordinate system fixed with respect to the stars. Just like we can specify the latitude and longitude of a place on Earth, we can specify the coordinates of a star relative to a coordinate system fixed with respect to the stars. Look at Figure 1.5 of the textbook for a definition of this coordinate system. The Equatorial Coordinate System is similar in concept to longitude and latitude. • Right Ascension ! longitude. The symbol for Right Ascension is α. The units of Right Ascension are hours, minutes, and seconds, just like time • Declination ! latitude. The symbol for Declination is δ. Declination = 0◦ cor- responds to the Celestial Equator, δ = 90◦ corresponds to the North Celestial Pole. Let's look at the Equatorial Coordinates of some objects you should have seen last night. • Arcturus: RA= 14h16m, Dec= +19◦110 (see Appendix A) • Vega: RA= 18h37m, Dec= +38◦470 (see Appendix A) • Venus: RA= 13h02m, Dec= −6◦370 • Saturn: RA= 14h21m, Dec= −11◦410 −! Hand out SC1 charts. Find these objects on them. Now find the constellation of Orion, and read off the Right Ascension and Decli- nation of the middle star in the belt. Next week in lab, you will have the chance to use the computer program Stellar- ium to display the sky and find coordinates of objects (stars, planets). 1.1 Further Remarks on the Equatorial Coordinate System The Equatorial Coordinate System is fundamentally established by the rotation axis of the Earth. -
2 Coordinate Systems
2 Coordinate systems In order to find something one needs a system of coordinates. For determining the positions of the stars and planets where the distance to the object often is unknown it usually suffices to use two coordinates. On the other hand, since the Earth rotates around it’s own axis as well as around the Sun the positions of stars and planets is continually changing, and the measurment of when an object is in a certain place is as important as deciding where it is. Our first task is to decide on a coordinate system and the position of 1. The origin. E.g. one’s own location, the center of the Earth, the, the center of the Solar System, the Galaxy, etc. 2. The fundamental plan (x−y plane). This is often a plane of some physical significance such as the horizon, the equator, or the ecliptic. 3. Decide on the direction of the positive x-axis, also known as the “reference direction”. 4. And, finally, on a convention of signs of the y− and z− axes, i.e whether to use a left-handed or right-handed coordinate system. For example Eratosthenes of Cyrene (c. 276 BC c. 195 BC) was a Greek mathematician, elegiac poet, athlete, geographer, astronomer, and music theo- rist who invented a system of latitude and longitude. (According to Wikipedia he was also the first person to use the word geography and invented the disci- pline of geography as we understand it.). The origin of this coordinate system was the center of the Earth and the fundamental plane was the equator, which location Eratosthenes calculated relative to the parts of the Earth known to him. -
Surveyor 1 Space- Craft on June 2, 1966 As Seen by the Narrow Angle Camera of the Lunar Re- Connaissance Orbiter Taken on July 17, 2009 (Also See Fig
i “Project Surveyor, in particular, removed any doubt that it was possible for Americans to land on the Moon and explore its surface.” — Harrison H. Schmitt, Apollo 17 Scientist-Astronaut ii Frontispiece: Landing site of the Surveyor 1 space- craft on June 2, 1966 as seen by the narrow angle camera of the Lunar Re- connaissance Orbiter taken on July 17, 2009 (also see Fig. 13). The white square in the upper photo outlines the area of the enlarged view below. The spacecraft is ca. 3.3 m tall and is casting a 15 m shadow to the East. (NASA/LROC/ ASU/GSFC photos) iii iv Surveyor I: America’s First Moon Landing by William F. Mellberg v © 2014, 2015 William F. Mellberg vi About the author: William Mellberg was a marketing and public relations representative with Fokker Aircraft. He is also an aerospace historian, having published many articles on both the development of airplanes and space vehicles in various magazines. He is the author of Famous Airliners and Moon Missions. He also serves as co-Editor of Harrison H. Schmitt’s website: http://americasuncommonsense.com Acknowledgments: The support and recollections of Frank Mellberg, Harrison Schmitt, Justin Rennilson, Alexander Gurshstein, Paul Spudis, Ronald Wells, Colin Mackellar and Dwight Steven- Boniecki is gratefully acknowledged. vii Surveyor I: America’s First Moon Landing by William F. Mellberg A Journey of 250,000 Miles . December 14, 2013. China’s Chang’e 3 spacecraft successfully touched down on the Moon at 1311 GMT (2111 Beijing Time). The landing site was in Mare Imbrium, the Sea of Rains, about 25 miles (40 km) south of the small crater, Laplace F, and roughly 100 miles (160 km) east of its original target in Sinus Iridum, the Bay of Rainbows.