Cladistical Analysis of the Jovian and Saturnian Satellite Systems
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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. -
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 -
Astrometric Positions for 18 Irregular Satellites of Giant Planets from 23
Astronomy & Astrophysics manuscript no. Irregulares c ESO 2018 October 20, 2018 Astrometric positions for 18 irregular satellites of giant planets from 23 years of observations,⋆,⋆⋆,⋆⋆⋆,⋆⋆⋆⋆ A. R. Gomes-Júnior1, M. Assafin1,†, R. Vieira-Martins1, 2, 3,‡, J.-E. Arlot4, J. I. B. Camargo2, 3, F. Braga-Ribas2, 5,D.N. da Silva Neto6, A. H. Andrei1, 2,§, A. Dias-Oliveira2, B. E. Morgado1, G. Benedetti-Rossi2, Y. Duchemin4, 7, J. Desmars4, V. Lainey4, W. Thuillot4 1 Observatório do Valongo/UFRJ, Ladeira Pedro Antônio 43, CEP 20.080-090 Rio de Janeiro - RJ, Brazil e-mail: [email protected] 2 Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil e-mail: [email protected] 3 Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil 4 Institut de mécanique céleste et de calcul des éphémérides - Observatoire de Paris, UMR 8028 du CNRS, 77 Av. Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] 5 Federal University of Technology - Paraná (UTFPR / DAFIS), Rua Sete de Setembro, 3165, CEP 80230-901, Curitiba, PR, Brazil 6 Centro Universitário Estadual da Zona Oeste, Av. Manual Caldeira de Alvarenga 1203, CEP 23.070-200 Rio de Janeiro RJ, Brazil 7 ESIGELEC-IRSEEM, Technopôle du Madrillet, Avenue Galilée, 76801 Saint-Etienne du Rouvray, France Received: Abr 08, 2015; accepted: May 06, 2015 ABSTRACT Context. The irregular satellites of the giant planets are believed to have been captured during the evolution of the solar system. Knowing their physical parameters, such as size, density, and albedo is important for constraining where they came from and how they were captured. -
Cassini Observations of Saturn's Irregular Moons
EPSC Abstracts Vol. 12, EPSC2018-103-1, 2018 European Planetary Science Congress 2018 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2018 Cassini Observations of Saturn's Irregular Moons Tilmann Denk (1) and Stefano Mottola (2) (1) Freie Universität Berlin, Germany ([email protected]), (2) DLR Berlin, Germany 1. Introduction two prograde irregulars are slower than ~13 h, while the periods of all but two retrogrades are faster than With the ISS-NAC camera of the Cassini spacecraft, ~13 h. The fastest period (Hati) is much slower than we obtained photometric lightcurves of 25 irregular the disruption rotation barrier for asteroids (~2.3 h), moons of Saturn. The goal was to derive basic phys- indicating that Saturn's irregulars may be rubble piles ical properties of these objects (like rotational periods, of rather low densities, possibly as low as of comets. shapes, pole-axis orientations, possible global color variations, ...) and to get hints on their formation and Table: Rotational periods of 25 Saturnian irregulars evolution. Our campaign marks the first utilization of an interplanetary probe for a systematic photometric Moon Approx. size Rotational period survey of irregular moons. name [km] [h] Hati 5 5.45 ± 0.04 The irregular moons are a class of objects that is very Mundilfari 7 6.74 ± 0.08 distinct from the inner moons of Saturn. Not only are Loge 5 6.9 ± 0.1 ? they more numerous (38 versus 24), but also occupy Skoll 5 7.26 ± 0.09 (?) a much larger volume within the Hill sphere of Suttungr 7 7.67 ± 0.02 Saturn. -
CALCEPH - Fortran 77/90/95 Language Release 3.5.0
CALCEPH - Fortran 77/90/95 language Release 3.5.0 M. Gastineau, J. Laskar, A. Fienga, H. Manche Aug 19, 2021 CONTENTS 1 Introduction 3 2 Installation 5 2.1 Unix-like system (Linux, Mac OS X, BSD, Cygwin, ...)........................5 2.1.1 Quick instructions........................................5 2.1.2 Detailed instructions......................................5 2.2 Windows system.............................................7 2.2.1 Using the Microsoft Visual C++ compiler...........................7 2.2.2 Using the MinGW.......................................9 3 Library interface 11 3.1 A simple example program........................................ 11 3.2 Headers and Libraries.......................................... 11 3.2.1 Compilation on a Unix-like system............................... 12 3.2.2 Compilation on a Windows system............................... 12 3.3 Types................................................... 12 3.4 Constants................................................. 12 4 Multiple file access functions 15 4.1 Thread notes............................................... 15 4.2 Usage................................................... 15 4.3 Functions................................................. 15 4.3.1 calceph_open.......................................... 15 4.3.2 f90calceph_open_array..................................... 16 4.3.3 f90calceph_prefetch....................................... 17 4.3.4 f90calceph_isthreadsafe..................................... 17 4.3.5 f90calceph_compute..................................... -
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. -
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) -
Observing the Universe
ObservingObserving thethe UniverseUniverse :: aa TravelTravel ThroughThrough SpaceSpace andand TimeTime Enrico Flamini Agenzia Spaziale Italiana Tokyo 2009 When you rise your head to the night sky, what your eyes are observing may be astonishing. However it is only a small portion of the electromagnetic spectrum of the Universe: the visible . But any electromagnetic signal, indipendently from its frequency, travels at the speed of light. When we observe a star or a galaxy we see the photons produced at the moment of their production, their travel could have been incredibly long: it may be lasted millions or billions of years. Looking at the sky at frequencies much higher then visible, like in the X-ray or gamma-ray energy range, we can observe the so called “violent sky” where extremely energetic fenoena occurs.like Pulsar, quasars, AGN, Supernova CosmicCosmic RaysRays:: messengersmessengers fromfrom thethe extremeextreme universeuniverse We cannot see the deep universe at E > few TeV, since photons are attenuated through →e± on the CMB + IR backgrounds. But using cosmic rays we should be able to ‘see’ up to ~ 6 x 1010 GeV before they get attenuated by other interaction. Sources Sources → Primordial origin Primordial 7 Redshift z = 0 (t = 13.7 Gyr = now ! ) Going to a frequency lower then the visible light, and cooling down the instrument nearby absolute zero, it’s possible to observe signals produced millions or billions of years ago: we may travel near the instant of the formation of our universe: 13.7 By. Redshift z = 1.4 (t = 4.7 Gyr) Credits A. Cimatti Univ. Bologna Redshift z = 5.7 (t = 1 Gyr) Credits A. -
Long-Term Evolution and Stability of Saturnian Small Satellites
MNRAS 000, 1–17 (2016) Preprint 30 August 2021 Compiled using MNRAS LATEX style file v3.0 Long-term Evolution and Stability of Saturnian Small Satellites: Aegaeon, Methone, Anthe, and Pallene. M. A. Mun˜oz-Guti´errez,1⋆ and S. Giuliatti Winter1 1Universidade Estadual Paulista - UNESP, Grupo de Dinˆamica Orbital e Planetologia, Av. Ariberto Pereira da Cunha, 333, Guaratinguet´a-SP, 12516-410, Brazil Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Aegaeon, Methone, Anthe, and Pallene are four Saturnian small moons, discovered by the Cassini spacecraft. Although their orbital characterization has been carried on by a number of authors, their long-term evolution has not been studied in detail so far. In this work, we numerically explore the long-term evolution, up to 105 yr, of the small moons in a system formed by an oblate Saturn and the five largest moons close to the region: Janus, Epimetheus, Mimas, Enceladus, and Tethys. By using frequency analysis we determined the stability of the small moons and characterize, through diffusion maps, the dynamical behavior of a wide region of geometric phase space, a vs e, surrounding them. Those maps could shed light on the possible initial number of small bodies close to Mimas, and help to better understand the dynamical origin of the small satellites. We found that the four small moons are long-term stable and no mark of chaos is found for them. Aegaeon, Methone, and Anthe could remain unaltered for at least ∼ 0.5Myr, given the current configuration of the system. They remain well- trapped in the corotation eccentricity resonances with Mimas in which they currently librate. -
THE SATURNIAN G RING: a SHORT NOTE ABOUT ITS FORMATION Revista Mexicana De Astronomía Y Astrofísica, Vol
Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México Maravilla, D.; Leal-Herrera, J. L. THE SATURNIAN G RING: A SHORT NOTE ABOUT ITS FORMATION Revista Mexicana de Astronomía y Astrofísica, vol. 50, núm. 2, octubre, 2014, pp. 341- 347 Instituto de Astronomía Distrito Federal, México Available in: http://www.redalyc.org/articulo.oa?id=57148278016 How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative Revista Mexicana de Astronom´ıa y Astrof´ısica, 50, 341–347 (2014) THE SATURNIAN G RING: A SHORT NOTE ABOUT ITS FORMATION D. Maravilla and J. L. Leal-Herrera Departamento de Ciencias Espaciales, Instituto de Geof´ısica, UNAM, Mexico Received March 21 2014; accepted August 18 2014 RESUMEN En este trabajo se estudia la formaci´on del anillo G de Saturno considerando que el sat´elite Ege´on es la fuente de part´ıculas de polvo. El polvo que forma el anillo se produce por impactos entre los micrometeoroides interplanetarios que ingresan en la magnet´osfera Saturniana y la superficie de Ege´on. Para explicar c´omo se forma el anillo se usa un modelo gravito-electrodin´amico suponiendo que las fuerzas gravitacional y electromagn´etica son las ´unicas fuerzas que modulan el comportamiento din´amico de las part´ıculas de polvo. Las soluciones del modelo muestran que existen reg´ımenes de confinamiento (captura) as´ıcomo reg´ımenes de escape de polvo en la vecindad de Ege´on.