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![Arxiv:1912.09192V2 [Astro-Ph.EP] 24 Feb 2020](https://docslib.b-cdn.net/cover/2925/arxiv-1912-09192v2-astro-ph-ep-24-feb-2020-2925.webp)
Arxiv:1912.09192V2 [Astro-Ph.EP] 24 Feb 2020
Draft version February 25, 2020 Typeset using LATEX preprint style in AASTeX62 Photometric analyses of Saturn's small moons: Aegaeon, Methone and Pallene are dark; Helene and Calypso are bright. M. M. Hedman,1 P. Helfenstein,2 R. O. Chancia,1, 3 P. Thomas,2 E. Roussos,4 C. Paranicas,5 and A. J. Verbiscer6 1Department of Physics, University of Idaho, Moscow, ID 83844 2Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca NY 14853 3Center for Imaging Science, Rochester Institute of Technology, Rochester NY 14623 4Max Planck Institute for Solar System Research, G¨ottingen,Germany 37077 5APL, John Hopkins University, Laurel MD 20723 6Department of Astronomy, University of Virginia, Charlottesville, VA 22904 ABSTRACT We examine the surface brightnesses of Saturn's smaller satellites using a photometric model that explicitly accounts for their elongated shapes and thus facilitates compar- isons among different moons. Analyses of Cassini imaging data with this model reveals that the moons Aegaeon, Methone and Pallene are darker than one would expect given trends previously observed among the nearby mid-sized satellites. On the other hand, the trojan moons Calypso and Helene have substantially brighter surfaces than their co-orbital companions Tethys and Dione. These observations are inconsistent with the moons' surface brightnesses being entirely controlled by the local flux of E-ring par- ticles, and therefore strongly imply that other phenomena are affecting their surface properties. The darkness of Aegaeon, Methone and Pallene is correlated with the fluxes of high-energy protons, implying that high-energy radiation is responsible for darkening these small moons. Meanwhile, Prometheus and Pandora appear to be brightened by their interactions with nearby dusty F ring, implying that enhanced dust fluxes are most likely responsible for Calypso's and Helene's excess brightness. -
Lab 7: Gravity and Jupiter's Moons
Lab 7: Gravity and Jupiter's Moons Image of Galileo Spacecraft Gravity is the force that binds all astronomical structures. Clusters of galaxies are gravitationally bound into the largest structures in the Universe, Galactic Superclusters. The galaxies themselves are held together by gravity, as are all of the star systems within them. Our own Solar System is a collection of bodies gravitationally bound to our star, Sol. Cutting edge science requires the use of Einstein's General Theory of Relativity to explain gravity. But the interactions of the bodies in our Solar System were understood long before Einstein's time. In chapter two of Chaisson McMillan's Astronomy Today, you went over Kepler's Laws. These laws of gravity were made to describe the interactions in our Solar System. P2=a3/M Where 'P' is the orbital period in Earth years, the time for the body to make one full orbit. 'a' is the length of the orbit's semi-major axis, for nearly circular orbits the orbital radius. 'M' is the total mass of the system in units of Solar Masses. Jupiter System Montage picture from NASA ID = PIA01481 Jupiter has over 60 moons at the last count, most of which are asteroids and comets captured from Written by Meagan White and Paul Lewis Page 1 the Asteroid Belt. When Galileo viewed Jupiter through his early telescope, he noticed only four moons: Io, Europa, Ganymede, and Callisto. The Jupiter System can be thought of as a miniature Solar System, with Jupiter in place of the Sun, and the Galilean moons like planets. -
Galileo and the Telescope
Galileo and the Telescope A Discussion of Galileo Galilei and the Beginning of Modern Observational Astronomy ___________________________ Billy Teets, Ph.D. Acting Director and Outreach Astronomer, Vanderbilt University Dyer Observatory Tuesday, October 20, 2020 Image Credit: Giuseppe Bertini General Outline • Telescopes/Galileo’s Telescopes • Observations of the Moon • Observations of Jupiter • Observations of Other Planets • The Milky Way • Sunspots Brief History of the Telescope – Hans Lippershey • Dutch Spectacle Maker • Invention credited to Hans Lippershey (c. 1608 - refracting telescope) • Late 1608 – Dutch gov’t: “ a device by means of which all things at a very great distance can be seen as if they were nearby” • Is said he observed two children playing with lenses • Patent not awarded Image Source: Wikipedia Galileo and the Telescope • Created his own – 3x magnification. • Similar to what was peddled in Europe. • Learned magnification depended on the ratio of lens focal lengths. • Had to learn to grind his own lenses. Image Source: Britannica.com Image Source: Wikipedia Refracting Telescopes Bend Light Refracting Telescopes Chromatic Aberration Chromatic aberration limits ability to distinguish details Dealing with Chromatic Aberration - Stop Down Aperture Galileo used cardboard rings to limit aperture – Results were dimmer views but less chromatic aberration Galileo and the Telescope • Created his own (3x, 8-9x, 20x, etc.) • Noted by many for its military advantages August 1609 Galileo and the Telescope • First observed the -
Water Masers in the Saturnian System
A&A 494, L1–L4 (2009) Astronomy DOI: 10.1051/0004-6361:200811186 & c ESO 2009 Astrophysics Letter to the Editor Water masers in the Saturnian system S. V. Pogrebenko1,L.I.Gurvits1, M. Elitzur2,C.B.Cosmovici3,I.M.Avruch1,4, S. Montebugnoli5 , E. Salerno5, S. Pluchino3,5, G. Maccaferri5, A. Mujunen6, J. Ritakari6, J. Wagner6,G.Molera6, and M. Uunila6 1 Joint Institute for VLBI in Europe, PO Box 2, 7990 AA Dwingeloo, The Netherlands e-mail: [pogrebenko;lgurvits]@jive.nl 2 Department of Physics and Astronomy, University of Kentucky, 600 Rose Street, Lexington, KY 40506-0055, USA e-mail: [email protected] 3 Istituto Nazionale di Astrofisica (INAF) – Istituto di Fisica dello Spazio Interplanetario (IFSI), via del Fosso del Cavaliere, 00133 Rome, Italy e-mail: [email protected] 4 Science & Technology BV, PO 608 2600 AP Delft, The Netherlands e-mail: [email protected] 5 Istituto Nazionale di Astrofisica (INAF) – Istituto di Radioastronomia (IRA) – Stazione Radioastronomica di Medicina, via Fiorentina 3508/B, 40059 Medicina (BO), Italy e-mail: [s.montebugnoli;e.salerno;g.maccaferri]@ira.inaf.it; [email protected] 6 Helsinki University of Technology TKK, Metsähovi Radio Observatory, 02540 Kylmälä, Finland e-mail: [amn;jr;jwagner;gofrito;minttu]@kurp.hut.fi Received 18 October 2008 / Accepted 4 December 2008 ABSTRACT Context. The presence of water has long been seen as a key condition for life in planetary environments. The Cassini spacecraft discovered water vapour in the Saturnian system by detecting absorption of UV emission from a background star. Investigating other possible manifestations of water is essential, one of which, provided physical conditions are suitable, is maser emission. -
Cassini Update
Cassini Update Dr. Linda Spilker Cassini Project Scientist Outer Planets Assessment Group 22 February 2017 Sols%ce Mission Inclina%on Profile equator Saturn wrt Inclination 22 February 2017 LJS-3 Year 3 Key Flybys Since Aug. 2016 OPAG T124 – Titan flyby (1584 km) • November 13, 2016 • LAST Radio Science flyby • One of only two (cf. T106) ideal bistatic observations capturing Titan’s Northern Seas • First and only bistatic observation of Punga Mare • Western Kraken Mare not explored by RSS before T125 – Titan flyby (3158 km) • November 29, 2016 • LAST Optical Remote Sensing targeted flyby • VIMS high-resolution map of the North Pole looking for variations at and around the seas and lakes. • CIRS last opportunity for vertical profile determination of gases (e.g. water, aerosols) • UVIS limb viewing opportunity at the highest spatial resolution available outside of occultations 22 February 2017 4 Interior of Hexagon Turning “Less Blue” • Bluish to golden haze results from increased production of photochemical hazes as north pole approaches summer solstice. • Hexagon acts as a barrier that prevents haze particles outside hexagon from migrating inward. • 5 Refracting Atmosphere Saturn's• 22unlit February rings appear 2017 to bend as they pass behind the planet’s darkened limb due• 6 to refraction by Saturn's upper atmosphere. (Resolution 5 km/pixel) Dione Harbors A Subsurface Ocean Researchers at the Royal Observatory of Belgium reanalyzed Cassini RSS gravity data• 7 of Dione and predict a crust 100 km thick with a global ocean 10’s of km deep. Titan’s Summer Clouds Pose a Mystery Why would clouds on Titan be visible in VIMS images, but not in ISS images? ISS ISS VIMS High, thin cirrus clouds that are optically thicker than Titan’s atmospheric haze at longer VIMS wavelengths,• 22 February but optically 2017 thinner than the haze at shorter ISS wavelengths, could be• 8 detected by VIMS while simultaneously lost in the haze to ISS. -
Dynamics of Saturn's Small Moons in Coupled First Order Planar Resonances
Dynamics of Saturn's small moons in coupled first order planar resonances Maryame El Moutamid Bruno Sicardy and St´efanRenner LESIA/IMCCE | Paris Observatory 26 juin 2012 Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk Saturn system Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk Very small moons Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk New satellites : Anthe, Methone and Aegaeon (Cooper et al., 2008 ; Hedman et al., 2009, 2010 ; Porco et al., 2005) Very small (0.5 km to 2 km) Vicinity of the Mimas orbit (outside and inside) The aims of the work A better understanding : - of the dynamics of this population of news satellites - of the scenario of capture into mean motion resonances Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk Dynamical structure of the system µ µ´ Mp We consider only : - The resonant terms - The secular terms causing the precessions of the orbit When µ ! 0 ) The symmetry is broken ) different kinds of resonances : - Lindblad Resonance - Corotation Resonance D'Alembert rules : 0 0 c = (m + 1)λ − mλ − $ 0 L = (m + 1)λ − mλ − $ Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk Corotation Resonance - Aegaeon (7/6) : c = 7λMimas − 6λAegaeon − $Mimas - Methone (14/15) : c = 15λMethone − 14λMimas − $Mimas - Anthe (10/11) : c = 11λAnthe − 10λMimas − $Mimas Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk Corotation resonances Mean motion resonance : n1 = m+q n2 m Particular case : Lagrangian Equilibrium Points Maryame El Moutamid ESLAB-2012 | ESA/ESTEC Noordwijk Adam's ring and Galatea Maryame -
JUICE Red Book
ESA/SRE(2014)1 September 2014 JUICE JUpiter ICy moons Explorer Exploring the emergence of habitable worlds around gas giants Definition Study Report European Space Agency 1 This page left intentionally blank 2 Mission Description Jupiter Icy Moons Explorer Key science goals The emergence of habitable worlds around gas giants Characterise Ganymede, Europa and Callisto as planetary objects and potential habitats Explore the Jupiter system as an archetype for gas giants Payload Ten instruments Laser Altimeter Radio Science Experiment Ice Penetrating Radar Visible-Infrared Hyperspectral Imaging Spectrometer Ultraviolet Imaging Spectrograph Imaging System Magnetometer Particle Package Submillimetre Wave Instrument Radio and Plasma Wave Instrument Overall mission profile 06/2022 - Launch by Ariane-5 ECA + EVEE Cruise 01/2030 - Jupiter orbit insertion Jupiter tour Transfer to Callisto (11 months) Europa phase: 2 Europa and 3 Callisto flybys (1 month) Jupiter High Latitude Phase: 9 Callisto flybys (9 months) Transfer to Ganymede (11 months) 09/2032 – Ganymede orbit insertion Ganymede tour Elliptical and high altitude circular phases (5 months) Low altitude (500 km) circular orbit (4 months) 06/2033 – End of nominal mission Spacecraft 3-axis stabilised Power: solar panels: ~900 W HGA: ~3 m, body fixed X and Ka bands Downlink ≥ 1.4 Gbit/day High Δv capability (2700 m/s) Radiation tolerance: 50 krad at equipment level Dry mass: ~1800 kg Ground TM stations ESTRAC network Key mission drivers Radiation tolerance and technology Power budget and solar arrays challenges Mass budget Responsibilities ESA: manufacturing, launch, operations of the spacecraft and data archiving PI Teams: science payload provision, operations, and data analysis 3 Foreword The JUICE (JUpiter ICy moon Explorer) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015–2025, will provide the most comprehensive exploration to date of the Jovian system in all its complexity, with particular emphasis on Ganymede as a planetary body and potential habitat. -
Transit Timing Analysis of the Hot Jupiters WASP-43B and WASP-46B and the Super Earth Gj1214b
Transit timing analysis of the hot Jupiters WASP-43b and WASP-46b and the super Earth GJ1214b Mathias Polfliet Promotors: Michaël Gillon, Maarten Baes 1 Abstract Transit timing analysis is proving to be a promising method to detect new planetary partners in systems which already have known transiting planets, particularly in the orbital resonances of the system. In these resonances we might be able to detect Earth-mass objects well below the current detection and even theoretical (due to stellar variability) thresholds of the radial velocity method. We present four new transits for WASP-46b, four new transits for WASP-43b and eight new transits for GJ1214b observed with the robotic telescope TRAPPIST located at ESO La Silla Observatory, Chile. Modelling the data was done using several Markov Chain Monte Carlo (MCMC) simulations of the new transits with old data and a collection of transit timings for GJ1214b from published papers. For the hot Jupiters this lead to a general increase in accuracy for the physical parameters of the system (for the mass and period we found: 2.034±0.052 MJup and 0.81347460±0.00000048 days and 2.03±0.13 MJup and 1.4303723±0.0000011 days for WASP-43b and WASP-46b respectively). For GJ1214b this was not the case given the limited photometric precision of TRAPPIST. The additional timings however allowed us to constrain the period to 1.580404695±0.000000084 days and the RMS of the TTVs to 16 seconds. We investigated given systems for Transit Timing Variations (TTVs) and variations in the other transit parameters and found no significant (3sv) deviations. -
Privacy Policy
Privacy Policy Culmia Privacy Policy Culmia Desarrollos Inmobiliarios, S.L.U. (hereinafter, “the manager”), with headquarters in Madrid, Calle Génova, 27, Company Tax No. B-67186999, is an integral manager of property assets and a member of a Property Group to which it provides its services. The manager provides its services to the following property developers who are members of its Group: Company Company Company Company Tax Tax No. No. Saturn Holdco S.A.U. A88554100 Antea Activos Inmobiliarios B88554324 S.L.U. Thrym Activos Inmobiliarios S.L.U. B88554142 Redes Promotora 1 Ma, B88093117 S.L.U. Erriap Activos Inmobiliarios S.L.U. B88554159 Redes Promotora 2 Ma, B88093174 S.L.U. Daphne Activos Inmobiliarios S.L.U. B88554167 Redes Promotora 3 Ma, B88093265 S.L.U. Dione Activos Inmobiliarios S.L.U. B88554183 Redes Promotora 4 Ma, B88093356 S.L.U. Fornjot Activos Inmobiliarios S.L.U. B88554191 Redes Promotora 5 Ma, B88093471 S.L.U. Greip Activos Inmobiliarios S.L.U. B88554217 Redes Promotora 6 Ma, B88145073 S.L.U. Hiperion Activos Inmobiliarios B88554233 Redes Promotora 7 Ma, B88145123 S.L.U. S.L.U. Loge Activos Inmobiliarios S.L.U. B88554241 Redes Promotora 8 Ma, B88145263 S.L.U. Kiviuq Activos Inmobiliarios S.L.U. B88554258 Redes Promotora 9, S.L.U. B88159728 Narvi Activos Inmobiliarios S.L.U. B88554266 Redes 2 2018 Iberica 2 B88160221 S.L.U. Polux Activos Inmobiliarios S.L.U. B88554282 Redes 2 2018 Iberica 3 B88160239 S.L.U. Siarnaq Activos Inmobiliarios S.L.U. B88554290 Redes 2 Promotora B88160247 Inversiones 2018 IV S.L.U. -
The Effect of Jupiter\'S Mass Growth on Satellite Capture
A&A 414, 727–734 (2004) Astronomy DOI: 10.1051/0004-6361:20031645 & c ESO 2004 Astrophysics The effect of Jupiter’s mass growth on satellite capture Retrograde case E. Vieira Neto1;?,O.C.Winter1, and T. Yokoyama2 1 Grupo de Dinˆamica Orbital & Planetologia, UNESP, CP 205 CEP 12.516-410 Guaratinguet´a, SP, Brazil e-mail: [email protected] 2 Universidade Estadual Paulista, IGCE, DEMAC, CP 178 CEP 13.500-970 Rio Claro, SP, Brazil e-mail: [email protected] Received 13 June 2003 / Accepted 12 September 2003 Abstract. Gravitational capture can be used to explain the existence of the irregular satellites of giants planets. However, it is only the first step since the gravitational capture is temporary. Therefore, some kind of non-conservative effect is necessary to to turn the temporary capture into a permanent one. In the present work we study the effects of Jupiter mass growth for the permanent capture of retrograde satellites. An analysis of the zero velocity curves at the Lagrangian point L1 indicates that mass accretion provides an increase of the confinement region (delimited by the zero velocity curve, where particles cannot escape from the planet) favoring permanent captures. Adopting the restricted three-body problem, Sun-Jupiter-Particle, we performed numerical simulations backward in time considering the decrease of M . We considered initial conditions of the particles to be retrograde, at pericenter, in the region 100 R a 400 R and 0 e 0:5. The results give Jupiter’s mass at the X moment when the particle escapes from the planet. -
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). -
The Sources and Dynamical Mechanisms Responsible for Differing Regolith Cover on Satellites Embedded in Saturn’S E Ring
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 2790.pdf WHY SO MUTED? THE SOURCES AND DYNAMICAL MECHANISMS RESPONSIBLE FOR DIFFERING REGOLITH COVER ON SATELLITES EMBEDDED IN SATURN’S E RING. S. J. Morrison1 and S. G. Zaidi1, 1Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State Uni- versity, University Park, PA, 16802, USA ([email protected]) Introduction: Saturn’s E ring, sourced primarily by resonances with Tethys and Dione. We also numerically cryovolcanic material erupted from Enceladus, extends integrate E ring particle trajectories including these outward from Enceladus’ orbit to beyond Dione’s orbit forces using the integrator package REBOUND and RE- [1][2]. Amongst the satellites embedded in this ring, BOUNDx [10-12]. We use initial orbits for the Satur- there are observed differences in regolith cover. In par- nian System from [13] and estimated masses for the tad- ticular, the small satellites Telesto, Calypso, Helene, pole moons from [7] that assume an average density of and Polydeuces have more muted surfaces, an absence 0.6 g/cc. We include Saturn’s gravitational harmonics of small craters, and downslope transport of regolith up to J4 and plasma drag forces arising from collisions within large craters than observed on Tethys and Dione with co-rotating O+ ions, the primary constituent of on similar distance scales [3][4]. However, these small plasma in the region of the Saturnian system of interest. satellites orbit in a different dynamical environment: Results: To provide insight into whether outwardly Telesto and Calypso are on leading and trailing tadpole drifting E ring particles should accumulate in the 1:1 orbits about the L4 and L5 Lagrange points in the co- resonances with Tethys and Dione, we compare the orbital 1:1 mean motion resonance with Tethys, respec- timescale for a particle of a given size to drift across the tively, as are Helene and Polydeuces tadpoles of Dione maximum libration width of this resonance to the corre- [e.g.