Lecture 12 Overview of the Solar System Chapter 6
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Astrometric Reduction of Cassini ISS Images of the Saturnian Satellites Mimas and Enceladus? R
A&A 551, A129 (2013) Astronomy DOI: 10.1051/0004-6361/201220831 & c ESO 2013 Astrophysics Astrometric reduction of Cassini ISS images of the Saturnian satellites Mimas and Enceladus? R. Tajeddine1;3, N. J. Cooper1;2, V. Lainey1, S. Charnoz3, and C. D. Murray2 1 IMCCE, Observatoire de Paris, UMR 8028 du CNRS, UPMC, Université de Lille 1, 77 av. Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] 2 Astronomy Unit, School of Physics and Astronomy, Queen Mary University of London, Mile End Road, London E1 4NS, UK 3 Laboratoire AIM, UMR 7158, Université Paris Diderot – CEA IRFU – CNRS, Centre de l’Orme les Merisiers, 91191 Gif-sur-Yvette Cedex, France Received 2 December 2012 / Accepted 6 February 2013 ABSTRACT Aims. We provide astrometric observations of two of Saturn’s main satellites, Mimas and Enceladus, using high resolution Cassini ISS Narrow Angle Camera images. Methods. We developed a simplified astrometric reduction model for Cassini ISS images as an alternative to the one proposed by the Jet Propulsion Labratory (JPL). The particular advantage of the new model is that it is easily invertible, with only marginal loss in accuracy. We also describe our new limb detection and fitting technique. Results. We provide a total of 1790 Cassini-centred astrometric observations of Mimas and Enceladus, in right ascension (α) and declination (δ) in the International Celestial Reference Frame (ICRF). Mean residuals compared to JPL ephemerides SAT317 and SAT351 of about one kilometre for Mimas and few hundreds of metres for Enceladus were obtained, in α cos δ and δ, with a standard deviation of a few kilometres for both satellites. -
RADIAL VELOCITIES in the ZODIACAL DUST CLOUD
A SURVEY OF RADIAL VELOCITIES in the ZODIACAL DUST CLOUD Brian Harold May Astrophysics Group Department of Physics Imperial College London Thesis submitted for the Degree of Doctor of Philosophy to Imperial College of Science, Technology and Medicine London · 2007 · 2 Abstract This thesis documents the building of a pressure-scanned Fabry-Perot Spectrometer, equipped with a photomultiplier and pulse-counting electronics, and its deployment at the Observatorio del Teide at Izaña in Tenerife, at an altitude of 7,700 feet (2567 m), for the purpose of recording high-resolution spectra of the Zodiacal Light. The aim was to achieve the first systematic mapping of the MgI absorption line in the Night Sky, as a function of position in heliocentric coordinates, covering especially the plane of the ecliptic, for a wide variety of elongations from the Sun. More than 250 scans of both morning and evening Zodiacal Light were obtained, in two observing periods – September-October 1971, and April 1972. The scans, as expected, showed profiles modified by components variously Doppler-shifted with respect to the unshifted shape seen in daylight. Unexpectedly, MgI emission was also discovered. These observations covered for the first time a span of elongations from 25º East, through 180º (the Gegenschein), to 27º West, and recorded average shifts of up to six tenths of an angstrom, corresponding to a maximum radial velocity relative to the Earth of about 40 km/s. The set of spectra obtained is in this thesis compared with predictions made from a number of different models of a dust cloud, assuming various distributions of dust density as a function of position and particle size, and differing assumptions about their speed and direction. -
Abstracts of the 50Th DDA Meeting (Boulder, CO)
Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011). -
Ice& Stone 2020
Ice & Stone 2020 WEEK 33: AUGUST 9-15 Presented by The Earthrise Institute # 33 Authored by Alan Hale About Ice And Stone 2020 It is my pleasure to welcome all educators, students, topics include: main-belt asteroids, near-Earth asteroids, and anybody else who might be interested, to Ice and “Great Comets,” spacecraft visits (both past and Stone 2020. This is an educational package I have put future), meteorites, and “small bodies” in popular together to cover the so-called “small bodies” of the literature and music. solar system, which in general means asteroids and comets, although this also includes the small moons of Throughout 2020 there will be various comets that are the various planets as well as meteors, meteorites, and visible in our skies and various asteroids passing by Earth interplanetary dust. Although these objects may be -- some of which are already known, some of which “small” compared to the planets of our solar system, will be discovered “in the act” -- and there will also be they are nevertheless of high interest and importance various asteroids of the main asteroid belt that are visible for several reasons, including: as well as “occultations” of stars by various asteroids visible from certain locations on Earth’s surface. Ice a) they are believed to be the “leftovers” from the and Stone 2020 will make note of these occasions and formation of the solar system, so studying them provides appearances as they take place. The “Comet Resource valuable insights into our origins, including Earth and of Center” at the Earthrise web site contains information life on Earth, including ourselves; about the brighter comets that are visible in the sky at any given time and, for those who are interested, I will b) we have learned that this process isn’t over yet, and also occasionally share information about the goings-on that there are still objects out there that can impact in my life as I observe these comets. -
CLARK PLANETARIUM SOLAR SYSTEM FACT SHEET Data Provided by NASA/JPL and Other Official Sources
CLARK PLANETARIUM SOLAR SYSTEM FACT SHEET Data provided by NASA/JPL and other official sources. This handout ©July 2013 by Clark Planetarium (www.clarkplanetarium.org). May be freely copied by professional educators for classroom use only. The known satellites of the Solar System shown here next to their planets with their sizes (mean diameter in km) in parenthesis. The planets and satellites (with diameters above 1,000 km) are depicted in relative size (with Earth = 0.500 inches) and are arranged in order by their distance from the planet, with the closest at the top. Distances from moon to planet are not listed. Mercury Jupiter Saturn Uranus Neptune Pluto • 1- Metis (44) • 26- Hermippe (4) • 54- Hegemone (3) • 1- S/2009 S1 (1) • 33- Erriapo (10) • 1- Cordelia (40.2) (Dwarf Planet) (no natural satellites) • 2- Adrastea (16) • 27- Praxidike (6.8) • 55- Aoede (4) • 2- Pan (26) • 34- Siarnaq (40) • 2- Ophelia (42.8) • Charon (1186) • 3- Bianca (51.4) Venus • 3- Amalthea (168) • 28- Thelxinoe (2) • 56- Kallichore (2) • 3- Daphnis (7) • 35- Skoll (6) • Nix (60?) • 4- Thebe (98) • 29- Helike (4) • 57- S/2003 J 23 (2) • 4- Atlas (32) • 36- Tarvos (15) • 4- Cressida (79.6) • Hydra (50?) • 5- Desdemona (64) • 30- Iocaste (5.2) • 58- S/2003 J 5 (4) • 5- Prometheus (100.2) • 37- Tarqeq (7) • Kerberos (13-34?) • 5- Io (3,643.2) • 6- Pandora (83.8) • 38- Greip (6) • 6- Juliet (93.6) • 1- Naiad (58) • 31- Ananke (28) • 59- Callirrhoe (7) • Styx (??) • 7- Epimetheus (119) • 39- Hyrrokkin (8) • 7- Portia (135.2) • 2- Thalassa (80) • 6- Europa (3,121.6) -
Kuiper Belt Dust Grains As a Source of Interplanetary Dust Particles
z( _R_:s124. 429-441) 11996) NASA-CR-2044q9 _RIIfI.E NO. 220 Kuiper Belt Dust Grains as a Source of Interplanetary Dust Particles JER-CHYI LzOU AND HERBERT A. ZOOK SN3, NASA Johnson Space Center, Houston, Texas 77058 E-mail: liou_'sn3.jsc.nasa.gov. AND STANLEYF. DERMOTT Department of Astronomy. University of Florida, Gainesuille, Florida 3261I Reccwed August 25. 1995: revised May 16. 1996 Solar System interplanetary space (e.g., Leinert and Grtin The recent discovery of the so-called Kuiper belt objects has 1990, Levasseur-Reeourd _" al. 1991 ). However, since the :,rompted the idea that these objects produce dust grains that discovery of the lirst Iran,-neptunian obiect (Jcw'ilt and :na_ contribute significantly to the interplanetary dust popula- Luu 1992. 1993) and the <ill ongoing discoveries of such uon. In this paper, the orbital evolution of dust grains, of objects (see Jewitt and Luu 1995 for an up-to-date sum- diameters 1 to 9 Jam, that originate in the region of the Kuiper mary), it has been proposed that small dust particles pro- belt is studied by means of direct numerical integration. Gravi- duced from these so-called "'Kuiper belt objects" may con- tational forces of the Sun and planets, solar radiation pressure, as well as Poynting-Robertson drag and solar wind drag are tribute significantly to the interplanetary dust population included. The interactions between charged dust grains and that constitutes the zodiacal cloud (e.g., Flynn 1994). They solar magnetic field are not considered in the model. Because may also be an important source of the interplanetary of the effects of drag forces, small dust grains will spiral toward dust particles (IDPs) collected in the stratosphere by high- the Sun once they are released from their large parent bodies. -
A Physically-Based Night Sky Model Henrik Wann Jensen1 Fredo´ Durand2 Michael M
To appear in the SIGGRAPH conference proceedings A Physically-Based Night Sky Model Henrik Wann Jensen1 Fredo´ Durand2 Michael M. Stark3 Simon Premozeˇ 3 Julie Dorsey2 Peter Shirley3 1Stanford University 2Massachusetts Institute of Technology 3University of Utah Abstract 1 Introduction This paper presents a physically-based model of the night sky for In this paper, we present a physically-based model of the night sky realistic image synthesis. We model both the direct appearance for image synthesis, and demonstrate it in the context of a Monte of the night sky and the illumination coming from the Moon, the Carlo ray tracer. Our model includes the appearance and illumi- stars, the zodiacal light, and the atmosphere. To accurately predict nation of all significant sources of natural light in the night sky, the appearance of night scenes we use physically-based astronomi- except for rare or unpredictable phenomena such as aurora, comets, cal data, both for position and radiometry. The Moon is simulated and novas. as a geometric model illuminated by the Sun, using recently mea- The ability to render accurately the appearance of and illumi- sured elevation and albedo maps, as well as a specialized BRDF. nation from the night sky has a wide range of existing and poten- For visible stars, we include the position, magnitude, and temper- tial applications, including film, planetarium shows, drive and flight ature of the star, while for the Milky Way and other nebulae we simulators, and games. In addition, the night sky as a natural phe- use a processed photograph. Zodiacal light due to scattering in the nomenon of substantial visual interest is worthy of study simply for dust covering the solar system, galactic light, and airglow due to its intrinsic beauty. -
Zodiacal Cloud Complexes
Earth Planets Space, 50, 465–471, 1998 Zodiacal Cloud Complexes Ingrid Mann MPI fur¨ Aeronomie, D-37191 Katlenburg-Lindau, Germany (Received October 7, 1997; Revised March 17, 1998; Accepted March 17, 1998) We discuss some aspects of the study of the Zodiacal cloud based on brightness observations. The discussion of optical properties as well as the spatial distribution of the dust cloud show that the description of the dust cloud as a homogeneous cloud is reasonable for the regions near the Earth orbit, but fails in the description of the dust in the inner solar system. The reasons for this are that different components of the dust cloud may have different types of orbital evolution depending on the parameters of their initial orbits. Also the collisional evolution of dust in the inner solar system may have some influence. As far as perspectives for future observations are concerned, the study of Doppler shifts of the Fraunhofer lines in the Zodiacal light will provide further knowledge about the orbital distribution of dust particles, as well as advanced infrared observations will help towards a better understanding of the outer solar system dust cloud beyond the asteroid belt. 1. Introduction properties per volume element. A common method of data Small bodies in our solar system cover a broad size range analysis applies forward calculations of the line of sight inte- from asteroids and comets to dust particles of micrometer gral under reasonable assumptions about particle properties size and below. Brightness observations do mainly cover a and spatial distribution. Detailed descriptions of the line of range of particles of 1 to 100 micron in size, i.e. -
The Three-Dimensional Structure of the Zodiacal Dust Bands
ICARUS 127, 461±484 (1997) ARTICLE NO. IS975704 The Three-Dimensional Structure of the Zodiacal Dust Bands William T. Reach Universities Space Research Association and NASA Goddard Space Flight Center, Code 685, Greenbelt, Maryland 20771, and Institut d'Astrophysique Spatiale, BaÃtiment 121, Universite Paris XI, 91405 Orsay Cedex, France E-mail: [email protected] Bryan A. Franz General Sciences Corporation, NASA Goddard Space Flight Center, Code 970.1, Greenbelt, Maryland 20771 and Janet L. Weiland Hughes STX, NASA Goddard Space Flight Center, Code 685.9, Greenbelt, Maryland 20771 Received July 18, 1996; revised January 2, 1997 model, the dust is distributed among the asteroid family mem- Using observations of the infrared sky brightness by the bers with the same distributions of proper orbital inclination Cosmic Background Explorer (COBE)1 Diffuse Infrared Back- and semimajor axis but a random ascending node. In the mi- ground Experiment (DIRBE) and Infrared Astronomical Satel- grating model, particles are presumed to be under the in¯uence lite (IRAS), we have created maps of the surface brightness of Poynting±Robertson drag, so that they are distributed Fourier-®ltered to suppress the smallest (, 18) structures and throughout the inner Solar System. The migrating model is the large-scale background (.158). Dust bands associated with better able to match the parallactic variation of dust-band lati- the Themis, Koronis, and Eos families are readily evident. A tude as well as the 12- to 60-mm spectrum of the dust bands. dust band associated with the Maria family is also present. The The annual brightness variations can be explained only by the parallactic distances to the emitting regions of the Koronis, migrating model. -
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. -
The Kuiper Belt: What We Know and What We Don’T
The Kuiper Belt: What We Know and What We Don’t David Jewitt, UCLA, September 2012 The best indication of the significance of the Kuiper belt lies in its multiple connections to other aspects of the Solar system. The dust in the Zodiacal cloud, the rocks in the meteor streams, the nuclei of comets, the Centaurs, perhaps also the irregular moons of the planets and the Trojans that lead and trail planets in their orbits, are all related to the parent population in the Kuiper belt. Further afield, the dusty debris disks of other stars are likely produced by collisional shattering of parent bodies in unseen Kuiper belts about them. Because of these many connections, Kuiper belt science has already had significant impact on the study of the contents, origin and evolution of the Solar system, and on understanding the Solar system in the context set by other stars. While we know much more than we used to, we still don’t know many things about the Kuiper belt. The Solar system formed from a flattened, rotating disk of gas and dust, itself produced by gravitational collapse from the interstellar medium. The explosion of a nearby massive star, a “supernova”, may have provided the initial compression causing the cloud to collapse, as suggested by the products of decay of short-lived radioactive elements (esp. 26Al) embedded in meteorites (Lee et al. 1977, Dauphas and Chaussidon 2011). Planets formed quickly in the dense inner portions of this disk but the process of growth in the rarefied outer regions was very slow. -
Colours of Minor Bodies in the Outer Solar System II - a Statistical Analysis, Revisited
Astronomy & Astrophysics manuscript no. MBOSS2 c ESO 2012 April 26, 2012 Colours of Minor Bodies in the Outer Solar System II - A Statistical Analysis, Revisited O. R. Hainaut1, H. Boehnhardt2, and S. Protopapa3 1 European Southern Observatory (ESO), Karl Schwarzschild Straße, 85 748 Garching bei M¨unchen, Germany e-mail: [email protected] 2 Max-Planck-Institut f¨ur Sonnensystemforschung, Max-Planck Straße 2, 37 191 Katlenburg- Lindau, Germany 3 Department of Astronomy, University of Maryland, College Park, MD 20 742-2421, USA Received —; accepted — ABSTRACT We present an update of the visible and near-infrared colour database of Minor Bodies in the outer Solar System (MBOSSes), now including over 2000 measurement epochs of 555 objects, extracted from 100 articles. The list is fairly complete as of December 2011. The database is now large enough that dataset with a high dispersion can be safely identified and rejected from the analysis. The method used is safe for individual outliers. Most of the rejected papers were from the early days of MBOSS photometry. The individual measurements were combined so not to include possible rotational artefacts. The spectral gradient over the visible range is derived from the colours, as well as the R absolute magnitude M(1, 1). The average colours, absolute magnitude, spectral gradient are listed for each object, as well as their physico-dynamical classes using a classification adapted from Gladman et al., 2008. Colour-colour diagrams, histograms and various other plots are presented to illustrate and in- vestigate class characteristics and trends with other parameters, whose significance are evaluated using standard statistical tests.