Instructor's Guide for Virtual Astronomy Laboratories
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Lecture 12 the Rings and Moons of the Outer Planets October 15, 2018
Lecture 12 The Rings and Moons of the Outer Planets October 15, 2018 1 2 Rings of Outer Planets • Rings are not solid but are fragments of material – Saturn: Ice and ice-coated rock (bright) – Others: Dusty ice, rocky material (dark) • Very thin – Saturn rings ~0.05 km thick! • Rings can have many gaps due to small satellites – Saturn and Uranus 3 Rings of Jupiter •Very thin and made of small, dark particles. 4 Rings of Saturn Flash movie 5 Saturn’s Rings Ring structure in natural color, photographed by Cassini probe July 23, 2004. Click on image for Astronomy Picture of the Day site, or here for JPL information 6 Saturn’s Rings (false color) Photo taken by Voyager 2 on August 17, 1981. Click on image for more information 7 Saturn’s Ring System (Cassini) Mars Mimas Janus Venus Prometheus A B C D F G E Pandora Enceladus Epimetheus Earth Tethys Moon Wikipedia image with annotations On July 19, 2013, in an event celebrated the world over, NASA's Cassini spacecraft slipped into Saturn's shadow and turned to image the planet, seven of its moons, its inner rings -- and, in the background, our home planet, Earth. 8 Newly Discovered Saturnian Ring • Nearly invisible ring in the plane of the moon Pheobe’s orbit, tilted 27° from Saturn’s equatorial plane • Discovered by the infrared Spitzer Space Telescope and announced 6 October 2009 • Extends from 128 to 207 Saturnian radii and is about 40 radii thick • Contributes to the two-tone coloring of the moon Iapetus • Click here for more info about the artist’s rendering 9 Rings of Uranus • Uranus -- rings discovered through stellar occultation – Rings block light from star as Uranus moves by. -
The Search for Exomoons and the Characterization of Exoplanet Atmospheres
Corso di Laurea Specialistica in Astronomia e Astrofisica The search for exomoons and the characterization of exoplanet atmospheres Relatore interno : dott. Alessandro Melchiorri Relatore esterno : dott.ssa Giovanna Tinetti Candidato: Giammarco Campanella Anno Accademico 2008/2009 The search for exomoons and the characterization of exoplanet atmospheres Giammarco Campanella Dipartimento di Fisica Università degli studi di Roma “La Sapienza” Associate at Department of Physics & Astronomy University College London A thesis submitted for the MSc Degree in Astronomy and Astrophysics September 4th, 2009 Università degli Studi di Roma ―La Sapienza‖ Abstract THE SEARCH FOR EXOMOONS AND THE CHARACTERIZATION OF EXOPLANET ATMOSPHERES by Giammarco Campanella Since planets were first discovered outside our own Solar System in 1992 (around a pulsar) and in 1995 (around a main sequence star), extrasolar planet studies have become one of the most dynamic research fields in astronomy. Our knowledge of extrasolar planets has grown exponentially, from our understanding of their formation and evolution to the development of different methods to detect them. Now that more than 370 exoplanets have been discovered, focus has moved from finding planets to characterise these alien worlds. As well as detecting the atmospheres of these exoplanets, part of the characterisation process undoubtedly involves the search for extrasolar moons. The structure of the thesis is as follows. In Chapter 1 an historical background is provided and some general aspects about ongoing situation in the research field of extrasolar planets are shown. In Chapter 2, various detection techniques such as radial velocity, microlensing, astrometry, circumstellar disks, pulsar timing and magnetospheric emission are described. A special emphasis is given to the transit photometry technique and to the two already operational transit space missions, CoRoT and Kepler. -
TOPICS in CELESTIAL MECHANICS 1. the Newtonian N-Body Problem
TOPICS IN CELESTIAL MECHANICS RICHARD MOECKEL 1. The Newtonian n-body Problem Celestial mechanics can be defined as the study of the solution of Newton's differ- ential equations formulated by Isaac Newton in 1686 in his Philosophiae Naturalis Principia Mathematica. The setting for celestial mechanics is three-dimensional space: 3 R = fq = (x; y; z): x; y; z 2 Rg with the Euclidean norm: p jqj = x2 + y2 + z2: A point particle is characterized by a position q 2 R3 and a mass m 2 R+. A motion of such a particle is described by a curve q(t) where t runs over some interval in R; the mass is assumed to be constant. Some remarks will be made below about why it is reasonable to model a celestial body by a point particle. For every motion of a point particle one can define: velocity: v(t) =q _(t) momentum: p(t) = mv(t): Newton formulated the following laws of motion: Lex.I. Corpus omne perservare in statu suo quiescendi vel movendi uniformiter in directum, nisi quatenus a viribus impressis cogitur statum illum mutare 1 Lex.II. Mutationem motus proportionem esse vi motrici impressae et fieri secundem lineam qua vis illa imprimitur. 2 Lex.III Actioni contrarium semper et aequalem esse reactionem: sive corporum duorum actiones in se mutuo semper esse aequales et in partes contrarias dirigi. 3 The first law is statement of the principle of inertia. The second law asserts the existence of a force function F : R4 ! R3 such that: p_ = F (q; t) or mq¨ = F (q; t): In celestial mechanics, the dependence of F (q; t) on t is usually indirect; the force on one body depends on the positions of the other massive bodies which in turn depend on t. -
Tidal Forces - Let 'Er Rip! 49
Tidal Forces - Let 'er Rip! 49 As the Moon orbits Earth, its gravitational pull raises the familiar tides in the ocean water, but did you know that it also raises 'earth tides' in the crust of earth? These tides are up to 50 centimeters in height and span continent-sized areas. The Earth also raises 'body tides' on the moon with a height of 5 meters! Now imagine that the moon were so close that it could no longer hold itself together against these tidal deformations. The distance were Earth's gravity will 'tidally disrupt' a solid satellite like the moon is called the tidal radius. One of the most dramatic examples of this is the rings of Saturn, where a nearby moon was disrupted, or prevented from forming in the first place! Images courtesy NASA/Hubble and Cassini. Problem 1 - The location of the tidal radius (also called the Roche Limit) for two 1/3 bodies is given by the formula d = 2.4x R (ρM/ρm) where ρM is the density of the primary body, ρm is the density of the satellite, and R is the radius of the main body. For the Earth-Moon system, what is the Roche Limit if R = 6,378 km, ρM = 3 3 5.5 gm/cm and ρm = 2.5 gm/cm ? (Note, the Roche Limit, d, will be in kilometers if R is also in kilometers, and so long as the densities are in the same units.) Problem 2 - Saturn's moons are made of ice with a density of about 1.2 gm/cm3 .If Saturn's density is 0.7 gm/cm3 and its radius is R = 58,000 km, how does its Roche Limit compare to the span of the ring system which extends from 66,000 km to 480,000 km from the planet's center? Problem 3 - In searching for planets orbiting other stars, many bodies similar to Jupiter in mass have been found orbiting sun-like stars at distances of only 3 million km. -
Kepler Press
National Aeronautics and Space Administration PRESS KIT/FEBRUARY 2009 Kepler: NASA’s First Mission Capable of Finding Earth-Size Planets www.nasa.gov Media Contacts J.D. Harrington Policy/Program Management 202-358-5241 NASA Headquarters [email protected] Washington 202-262-7048 (cell) Michael Mewhinney Science 650-604-3937 NASA Ames Research Center [email protected] Moffett Field, Calif. 650-207-1323 (cell) Whitney Clavin Spacecraft/Project Management 818-354-4673 Jet Propulsion Laboratory [email protected] Pasadena, Calif. 818-458-9008 (cell) George Diller Launch Operations 321-867-2468 Kennedy Space Center, Fla. [email protected] 321-431-4908 (cell) Roz Brown Spacecraft 303-533-6059. Ball Aerospace & Technologies Corp. [email protected] Boulder, Colo. 720-581-3135 (cell) Mike Rein Delta II Launch Vehicle 321-730-5646 United Launch Alliance [email protected] Cape Canaveral Air Force Station, Fla. 321-693-6250 (cell) Contents Media Services Information .......................................................................................................................... 5 Quick Facts ................................................................................................................................................... 7 NASA’s Search for Habitable Planets ............................................................................................................ 8 Scientific Goals and Objectives ................................................................................................................. -
Kepler's Laws of Planetary Motion
Kepler's laws of planetary motion In astronomy, Kepler's laws of planetary motion are three scientific laws describing the motion ofplanets around the Sun. 1. The orbit of a planet is an ellipse with the Sun at one of the twofoci . 2. A line segment joining a planet and the Sun sweeps out equal areas during equal intervals of time.[1] 3. The square of the orbital period of a planet is directly proportional to the cube of the semi-major axis of its orbit. Most planetary orbits are nearly circular, and careful observation and calculation are required in order to establish that they are not perfectly circular. Calculations of the orbit of Mars[2] indicated an elliptical orbit. From this, Johannes Kepler inferred that other bodies in the Solar System, including those farther away from the Sun, also have elliptical orbits. Kepler's work (published between 1609 and 1619) improved the heliocentric theory of Nicolaus Copernicus, explaining how the planets' speeds varied, and using elliptical orbits rather than circular orbits withepicycles .[3] Figure 1: Illustration of Kepler's three laws with two planetary orbits. Isaac Newton showed in 1687 that relationships like Kepler's would apply in the 1. The orbits are ellipses, with focal Solar System to a good approximation, as a consequence of his own laws of motion points F1 and F2 for the first planet and law of universal gravitation. and F1 and F3 for the second planet. The Sun is placed in focal pointF 1. 2. The two shaded sectors A1 and A2 Contents have the same surface area and the time for planet 1 to cover segmentA 1 Comparison to Copernicus is equal to the time to cover segment A . -
The Formation of the Martian Moons Rosenblatt P., Hyodo R
The Final Manuscript to Oxford Science Encyclopedia: The formation of the Martian moons Rosenblatt P., Hyodo R., Pignatale F., Trinh A., Charnoz S., Dunseath K.M., Dunseath-Terao M., & Genda H. Summary Almost all the planets of our solar system have moons. Each planetary system has however unique characteristics. The Martian system has not one single big moon like the Earth, not tens of moons of various sizes like for the giant planets, but two small moons: Phobos and Deimos. How did form such a system? This question is still being investigated on the basis of the Earth-based and space-borne observations of the Martian moons and of the more modern theories proposed to account for the formation of other moon systems. The most recent scenario of formation of the Martian moons relies on a giant impact occurring at early Mars history and having also formed the so-called hemispheric crustal dichotomy. This scenario accounts for the current orbits of both moons unlike the scenario of capture of small size asteroids. It also predicts a composition of disk material as a mixture of Mars and impactor materials that is in agreement with remote sensing observations of both moon surfaces, which suggests a composition different from Mars. The composition of the Martian moons is however unclear, given the ambiguity on the interpretation of the remote sensing observations. The study of the formation of the Martian moon system has improved our understanding of moon formation of terrestrial planets: The giant collision scenario can have various outcomes and not only a big moon as for the Earth. -
Orbital Mechanics Joe Spier, K6WAO – AMSAT Director for Education ARRL 100Th Centennial Educational Forum 1 History
Orbital Mechanics Joe Spier, K6WAO – AMSAT Director for Education ARRL 100th Centennial Educational Forum 1 History Astrology » Pseudoscience based on several systems of divination based on the premise that there is a relationship between astronomical phenomena and events in the human world. » Many cultures have attached importance to astronomical events, and the Indians, Chinese, and Mayans developed elaborate systems for predicting terrestrial events from celestial observations. » In the West, astrology most often consists of a system of horoscopes purporting to explain aspects of a person's personality and predict future events in their life based on the positions of the sun, moon, and other celestial objects at the time of their birth. » The majority of professional astrologers rely on such systems. 2 History Astronomy » Astronomy is a natural science which is the study of celestial objects (such as stars, galaxies, planets, moons, and nebulae), the physics, chemistry, and evolution of such objects, and phenomena that originate outside the atmosphere of Earth, including supernovae explosions, gamma ray bursts, and cosmic microwave background radiation. » Astronomy is one of the oldest sciences. » Prehistoric cultures have left astronomical artifacts such as the Egyptian monuments and Nubian monuments, and early civilizations such as the Babylonians, Greeks, Chinese, Indians, Iranians and Maya performed methodical observations of the night sky. » The invention of the telescope was required before astronomy was able to develop into a modern science. » Historically, astronomy has included disciplines as diverse as astrometry, celestial navigation, observational astronomy and the making of calendars, but professional astronomy is nowadays often considered to be synonymous with astrophysics. -
Roche Limit. Formation of Small Aggregates
ROYAL OBSERVATORY OF BELGIUM On the formation of the Martian moons from a circum-Mars accretion disk Rosenblatt P. and Charnoz S. 46th ESLAB Symposium: Formation and evolution of moons Session 2 – Mechanism of formation: Moons of terrestrial planets June 26th 2012 – ESTEC, Noordwijk, the Netherlands. The origin of the Martian moons ? Deimos (Viking image) Phobos (Viking image)Phobos (MEX/HRSC image) Size: 7.5km x 6.1km x 5.2km Size: 13.0km x 11.39km x 9.07km Unlike the Moon of the Earth, the origin of Phobos & Deimos is still an open issue. Capture or in-situ ? 1. Arguments for in-situ formation of Phobos & Deimos • Near-equatorial, near-circular orbits around Mars ( formation from a circum-Mars accretion disk) • Mars Express flybys of Phobos • Surface composition: phyllosilicates (Giuranna et al. 2011) => body may have formed in-situ (close to Mars’ orbit) • Low density => high porosity (Andert, Rosenblatt et al., 2010) => consistent with gravitational-aggregates 2. A scenario of in-situ formation of Phobos and Deimos from an accretion disk Adapted from Craddock R.A., Icarus (2011) Giant impact Accretion disk on Proto-Mars Mass: ~1018-1019 kg Gravitational instabilities formed moonlets Moonlets fall Two moonlets back onto Mars survived 4 Gy later elongated craters Physical modelling never been done. What modern theories of accretion can tell us about that scenario? 3. Purpose of this work: Origin of Phobos & Deimos consistent with theories of accretion? Modern theories of accretion : 2 main regimes of accretion. • (a) The strong tide regime => close to the planet ~ Roche Limit Background : Accretion of Saturn’s small moons (Charnoz et al., 2010) Accretion of the Earth’s moon (Canup 2004, Kokubo et al., 2000) • (b) The weak tide regime => farther from the planet Background : Accretion of big satellites of Jupiter & Saturn Accretion of planetary embryos (Lissauer 1987, Kokubo 2007, and works from G. -
On the Origin of the Ring System of (10199) Chariklo
On the origin of the ring system of (10199) Chariklo M. D. Melita1, Duffard, R.2, Ortiz J.L.2 [email protected] 1 IAFE (UBA-CONICET) y FCAG (UNLP). 2 Instituto de Astrof´ısica de Andaluc´ıa (CSIC). Granada. Espana.˜ Melita et al. Fof 2016. – p. 1 Layout Astrophysical Background: . (10199) Chariklo . The Centaurs . (10199) Chariklo Ring System Formation scenarios: . Classical Roche limit & Tidal evolution . Material ejected by a collision on the body of the asteoriod . Breakup of a satellite of (10199) Chariklo due to a catastrophic collision . Cometary-like activity (Pan & Wu 2016, arXiv:1602.01769) . Discussion Melita et al. Fof 2016. – p. 2 Centaur asteroids Melita et al. Fof 2016. – p. 3 The Centaurs Features and Peculiarities . It is a transitinal population (Levison & Duncan 1997) with dynamical lifetimes between the planets of ∼ 104 − 105 yr. The observed surface properties are not a simple juxtaposition of the properties of the bodies at the origin (TNOs) or as end-states (JFCs), i.e. The color distribution is bimodal (Tegler & Romanishin 2003, Melita & Licandro 2012), as observed in small TNOs (Peixinho 2014). Cometary-like comas have been observed on some members. e.g. (2060) Chiron, sometimes attributed to phase changes of water-ice (Jewitt 2009). Only class of asteroids where rings have been detected. Melita et al. Fof 2016. – p. 4 (10199) Chariklo . H = 6.6 . mV = 18.5 . p = 4.5 % . a = 15.75 AU . e = 0.15 . i=23deg . R1 = R2 = 122 km . R3 = 117 km . M(ρ = 1g/cm3)= 7 1018 kg . Colors: | B-V | = 0.86 (Grey) Melita et al. -
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Journal of Physics Special Topics P5_7 Put a Ring on it P. Hicks, B. Irwin, H. Lerman Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH. October 23, 2013 Abstract This article investigates if a scaled replica of the rings around Saturn could be formed around the Earth and the Moon by considering moving Moon-rock or water ice into their Roche limits. It is found that a rigid satellite made from Moon-rock would not form the desired ring system around either the Earth or the Moon, though a liquid satellite of either Moon-rock or water ice would. Introduction where is the distance from the surface of It is very easy for inhabitants of Earth the satellite to the centre of mass of the to be envious of the magnificent ring system primary mass, is the radius of the primary of Saturn. Neglecting all possible downsides mass, is the density of the primary mass and practicalities, such as disruptions to and is the density of the satellite. sunlight and life on Earth or physical A rigid satellite* would require construction, this article investigates whether stronger tidal forces to pull it apart, and hence it is possible to have a replica of Saturn’s main the Roche limit for a rigid satellite is less than rings around the Earth or the Moon. The that for a liquid satellite and is given by proposed method is moving satellites made of Moon-rock or water into the Roche limit ( ) where it will be broken apart by tidal forces into smaller particles to make the ring. -
Discovering Exoplanets Transiting Bright and Unusual Stars with K2
Discovering Exoplanets Transiting Bright and Unusual Stars with K2 ! ! PhD Thesis Proposal, Department of Astronomy, Harvard University ! ! Andrew Vanderburg! Advised by David! Latham ! ! ! April 18, 2015 After four years of surveying one field of view, the Kepler space telescope suffered a mechanical failure which ended its original planet-hunting mission, but has enabled a new mission (called K2) where Kepler surveys different fields across the sky. The K2 mission will survey 15 to 20 times more sky than the original Kepler mission, and in this wider field of view will be able to detect more planets orbiting rare objects. For my research exam, I developed a method to analyze K2 data that removes strong systematics from the light curves and enables planet detection. In my thesis, I propose to do the science enabled by my research exam work. I have already taken the work I completed for my research exam, upgraded and improved the method, and developed an automatic pipeline to search for transiting planets. I have searched K2 light curves for planets, produced a catalog of candidates, identified interesting planet candidates, and organized follow- up observations to confirm the discoveries. I propose to continue improving my software pipeline to detect even more planets, and produce a new catalog, and I propose to measure the mass of at least one of the resulting discoveries with the HARPS-N spectrograph. The resulting catalog will be a resource for astronomers studying these planets, and the investigations on interesting single objects will help us understand topics ranging from planet composition to the !evolution of planetary systems.