Physical Properties of Trans-Neptunian Binaries (120347) Salacia∓Actaea and (42355) Typhon∓Echidna
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
A Deeper Look at the Colors of the Saturnian Irregular Satellites Arxiv
A deeper look at the colors of the Saturnian irregular satellites Tommy Grav Harvard-Smithsonian Center for Astrophysics, MS51, 60 Garden St., Cambridge, MA02138 and Instiute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, HI86822 [email protected] James Bauer Jet Propulsion Laboratory, California Institute of Technology 4800 Oak Grove Dr., MS183-501, Pasadena, CA91109 [email protected] September 13, 2018 arXiv:astro-ph/0611590v2 8 Mar 2007 Manuscript: 36 pages, with 11 figures and 5 tables. 1 Proposed running head: Colors of Saturnian irregular satellites Corresponding author: Tommy Grav MS51, 60 Garden St. Cambridge, MA02138 USA Phone: (617) 384-7689 Fax: (617) 495-7093 Email: [email protected] 2 Abstract We have performed broadband color photometry of the twelve brightest irregular satellites of Saturn with the goal of understanding their surface composition, as well as their physical relationship. We find that the satellites have a wide variety of different surface colors, from the negative spectral slopes of the two retrograde satellites S IX Phoebe (S0 = −2:5 ± 0:4) and S XXV Mundilfari (S0 = −5:0 ± 1:9) to the fairly red slope of S XXII Ijiraq (S0 = 19:5 ± 0:9). We further find that there exist a correlation between dynamical families and spectral slope, with the prograde clusters, the Gallic and Inuit, showing tight clustering in colors among most of their members. The retrograde objects are dynamically and physically more dispersed, but some internal structure is apparent. Keywords: Irregular satellites; Photometry, Satellites, Surfaces; Saturn, Satellites. 3 1 Introduction The satellites of Saturn can be divided into two distinct groups, the regular and irregular, based on their orbital characteristics. -
" Tnos Are Cool": a Survey of the Trans-Neptunian Region VI. Herschel
Astronomy & Astrophysics manuscript no. classicalTNOsManuscript c ESO 2012 April 4, 2012 “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel⋆/PACS observations and thermal modeling of 19 classical Kuiper belt objects E. Vilenius1, C. Kiss2, M. Mommert3, T. M¨uller1, P. Santos-Sanz4, A. Pal2, J. Stansberry5, M. Mueller6,7, N. Peixinho8,9 S. Fornasier4,10, E. Lellouch4, A. Delsanti11, A. Thirouin12, J. L. Ortiz12, R. Duffard12, D. Perna13,14, N. Szalai2, S. Protopapa15, F. Henry4, D. Hestroffer16, M. Rengel17, E. Dotto13, and P. Hartogh17 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Postfach 1312, Giessenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Konkoly Observatory of the Hungarian Academy of Sciences, 1525 Budapest, PO Box 67, Hungary 3 Deutsches Zentrum f¨ur Luft- und Raumfahrt e.V., Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin, Germany 4 LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, France 5 Stewart Observatory, The University of Arizona, Tucson AZ 85721, USA 6 SRON LEA / HIFI ICC, Postbus 800, 9700AV Groningen, Netherlands 7 UNS-CNRS-Observatoire de la Cˆote d’Azur, Laboratoire Cassiope´e, BP 4229, 06304 Nice Cedex 04, France 8 Center for Geophysics of the University of Coimbra, Av. Dr. Dias da Silva, 3000-134 Coimbra, Portugal 9 Astronomical Observatory of the University of Coimbra, Almas de Freire, 3040-04 Coimbra, Portugal 10 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris, France 11 Laboratoire d’Astrophysique de Marseille, CNRS & Universit´ede Provence, 38 rue Fr´ed´eric Joliot-Curie, 13388 Marseille Cedex 13, France 12 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Camino Bajo de Hu´etor 50, 18008 Granada, Spain 13 INAF – Osservatorio Astronomico di Roma, via di Frascati, 33, 00040 Monte Porzio Catone, Italy 14 INAF - Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy 15 University of Maryland, College Park, MD 20742, USA 16 IMCCE, Observatoire de Paris, 77 av. -
Greek Mythology at the Service of the Portuguese Inquisition: the Case of Hercules and the Hydra of Lerna
Athens Journal of Mediterranean Studies- Volume 1, Issue 1 – Pages 25-44 Greek Mythology at the Service of the Portuguese Inquisition: The Case of Hercules and the Hydra of Lerna By Milton Dias Pacheco Greek mythology has been along the centuries a fruitful source of inspiration to artists and writers, as it possesses the strength of expressing symbolically the most common circumstances of life. Regarding the threats that in every age put in danger human life the most popular figure was maybe the Hydra that infested the region of the Lake of Lerna, in Argolis. This mythical figure may still have an older origin as it is connected with chthonic dangers. Because of its terrifying aspect, reptilian traits and poisonous breath, it was related to the evil and the domains of Hell. Later the Hydra significance became larger and deeper as it represented the heresies that could affect the Christian orthodoxy. According to this point of view, every defender of the Catholic Faith was immediately compared to Hercules, the Greek hero who succeeded in killing the mythological Hydra monster. In this way, it is easy to understand why this representation was often used in connection with the Iberian Habsburg Kings, as it worked as a political strategy of this dynasty, in which the Spanish Habsburgs were faced as the guardians and defenders of the Church of Rome, mainly in times when the Inquisition developed a determinative role. An illustrative example of this was the decoration of the arch built by the Inquisition in Lisbon, when King Philip II of Portugal visited the Portuguese Empire capital. -
With JWST: Science Justification and Observational Requirements
Observing Outer Planet Satellites (except Titan) with JWST: Science Justification and Observational Requirements Laszlo Keszthelyi1, Will Grundy2, John Stansberry3, Anand Sivaramakrishnan3, Deepashri Thatte3, Murthy Gudipati4, Constantine Tsang5, Alexandra Greenbaum6, Chima McGruder7 1U.S. Geological Survey, Astrogeology Science Center, 2255 N. Gemini Dr., Flagstaff, AZ 86001. ([email protected]) 2Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001. ([email protected]) 3Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218. ([email protected]; [email protected]; [email protected]) 4California Institute of Technology, Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109. ([email protected]) 5Southwest Research Institute, Department of Space Studies, 1050 Walnut St., Suite 300, Boulder, CO 80302. ([email protected]) 6 Department of Physics and Astronomy, 3400 N. Charles Street, Baltimore, MD 21218. ([email protected]) 7Department of Physics & Astronomy, 1408 Circle Drive, Knoxville, TN 37996. ([email protected]) ABSTRACT The James Webb Space Telescope (JWST) will allow observations with a unique combination of spectral, spatial, and temporal resolution for the study of outer planet satellites within our Solar System. We highlight the infrared spectroscopy of icy moons and temporal changes on geologically active satellites as two particularly valuable avenues of scientific inquiry. While some care must be taken to avoid saturation issues, JWST has observation modes that should provide excellent infrared data for such studies. KEYWORDS Solar System Astronomical Techniques 1. Introduction Starting in 2018, the James Webb Space Telescope (JWST) is expected to provide a groundbreaking new tool for astronomical observations, including planetary satellites as close as Phobos and Deimos. -
The Blurring Distinction Between Asteroids and Comets
Answers Research Journal 8 (2015):203–208. www.answersingenesis.org/arj/v8/asteroids-and-comets.pdf The Blurring Distinction between Asteroids and Comets Danny R. Faulkner, Answers in Genesis, PO Box 510, Hebron, Kentucky, 41048. Abstract Asteroids and comets long had been viewed as distinct objects with regards to orbits and composition. However, discoveries made in recent years have blurred those distinctions. Whether there is a continuum on which our older conception of asteroids and comets are extremes or if there still is a gap between them is not entirely clear yet. Some of the newer views of comets and asteroids may challenge the evolutionary theory of the solar system. Additionally, the new information may challenge the idea that the solar system is billions of years old. For readers not versed in nomenclature of small solar system bodies, I discuss that in the appendix. Keywords: small solar system objects, comets, asteroids (minor planets) Introduction the sun, and their orbits frequently are inclined The differences between asteroids and comets considerably to the orbits of the planets. Because of At one time, we thought of asteroids and comets as their highly elliptical orbits, most comets alternately being two very different groups of objects. Comets and are very close to the sun when near perihelion and asteroids certainly looked different. Comets can be very far from the sun when near aphelion. Comets visible to the naked eye, and have been known since spend most of the time near aphelion far from the ancient times. They have a hazy, fuzzy appearance. sun, so that their ices remain frozen. -
Jjmonl 1712.Pmd
alactic Observer John J. McCarthy Observatory G Volume 10, No. 12 December 2017 Holiday Theme Park See page 19 for more information The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue "OUT THE WINDOW ON YOUR LEFT"............................... 3 REFERENCES ON DISTANCES ................................................ 18 SINUS IRIDUM ................................................................ 4 INTERNATIONAL SPACE STATION/IRIDIUM SATELLITES ............. 18 EXTRAGALACTIC COSMIC RAYS ........................................ 5 SOLAR ACTIVITY ............................................................... 18 EQUATORIAL ICE ON MARS? ........................................... -
Mass of the Kuiper Belt · 9Th Planet PACS 95.10.Ce · 96.12.De · 96.12.Fe · 96.20.-N · 96.30.-T
Celestial Mechanics and Dynamical Astronomy manuscript No. (will be inserted by the editor) Mass of the Kuiper Belt E. V. Pitjeva · N. P. Pitjev Received: 13 December 2017 / Accepted: 24 August 2018 The final publication ia available at Springer via http://doi.org/10.1007/s10569-018-9853-5 Abstract The Kuiper belt includes tens of thousands of large bodies and millions of smaller objects. The main part of the belt objects is located in the annular zone between 39.4 au and 47.8 au from the Sun, the boundaries correspond to the average distances for orbital resonances 3:2 and 2:1 with the motion of Neptune. One-dimensional, two-dimensional, and discrete rings to model the total gravitational attraction of numerous belt objects are consid- ered. The discrete rotating model most correctly reflects the real interaction of bodies in the Solar system. The masses of the model rings were determined within EPM2017—the new version of ephemerides of planets and the Moon at IAA RAS—by fitting spacecraft ranging observations. The total mass of the Kuiper belt was calculated as the sum of the masses of the 31 largest trans-neptunian objects directly included in the simultaneous integration and the estimated mass of the model of the discrete ring of TNO. The total mass −2 is (1.97 ± 0.30) · 10 m⊕. The gravitational influence of the Kuiper belt on Jupiter, Saturn, Uranus and Neptune exceeds at times the attraction of the hypothetical 9th planet with a mass of ∼ 10 m⊕ at the distances assumed for it. -
Thermal Measurements
Physical characterization of Kuiper belt objects from stellar occultations and thermal measurements Pablo Santos-Sanz & the SBNAF team [email protected] Stellar occultations Simple method to: -Obtain high precision sizes/shapes (unc. ~km) -Detect/characterize atmospheres/rings… -Obtain albedo, density… -Improve the orbit of the body …this looks like very nice but...the reality is harder (at least for TNOs and Centaurs) EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations Titan 10 mas Quaoar 0.033 arsec Diameter of 1 Euro (33 mas) Pluto coin at 140 km Eris Charon Makemake Pablo Santos-Sanz EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations ~25 occultations by 15 TNOs (+ Pluto/Charon + Chariklo + Chiron + 2002 GZ32) Namaka Dysnomia Ixion Hi’iaka Pluto Haumea Eris Chiron 2007 UK126 Chariklo Vanth 2014 MU69 2002 GZ32 2003 VS2 2002 KX14 2002 TX300 2003 AZ84 2005 TV189 Stellar occultations: Eris & Chariklo Eris: 6 November 2010 Chariklo: 3 June 2014 • Size ~ Plutón • It has rings! • Albedo= 96% 3 • Density= 2.5 g/cm Danish 1.54-m telescope (La Silla) • Atmosphere < 1nbar (10-4 x Pluto) Eris’ radius Pluto’s radius 1163±6 km 1188.3±1.6 km (Nimmo et al. 2016) Braga-Ribas et al. 2014 (Nature) Sicardy et al. 2011 (Nature) EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations: Makemake 23 April 2011 Geometric Albedo = 77% (betwen Pluto and Eris) Possible local atmosphere! Ortiz et al. 2012 (Nature) EPSC2017, Riga, Latvia, 20 Sep. 2017 Stellar occultations: latest “catches” 2007 UK : 15 November 2014 2003 AZ84: 8 Jan. 2011 single, 3 Feb. 126 2012 multi, 2 Dec. -
The Solar System
5 The Solar System R. Lynne Jones, Steven R. Chesley, Paul A. Abell, Michael E. Brown, Josef Durech,ˇ Yanga R. Fern´andez,Alan W. Harris, Matt J. Holman, Zeljkoˇ Ivezi´c,R. Jedicke, Mikko Kaasalainen, Nathan A. Kaib, Zoran Kneˇzevi´c,Andrea Milani, Alex Parker, Stephen T. Ridgway, David E. Trilling, Bojan Vrˇsnak LSST will provide huge advances in our knowledge of millions of astronomical objects “close to home’”– the small bodies in our Solar System. Previous studies of these small bodies have led to dramatic changes in our understanding of the process of planet formation and evolution, and the relationship between our Solar System and other systems. Beyond providing asteroid targets for space missions or igniting popular interest in observing a new comet or learning about a new distant icy dwarf planet, these small bodies also serve as large populations of “test particles,” recording the dynamical history of the giant planets, revealing the nature of the Solar System impactor population over time, and illustrating the size distributions of planetesimals, which were the building blocks of planets. In this chapter, a brief introduction to the different populations of small bodies in the Solar System (§ 5.1) is followed by a summary of the number of objects of each population that LSST is expected to find (§ 5.2). Some of the Solar System science that LSST will address is presented through the rest of the chapter, starting with the insights into planetary formation and evolution gained through the small body population orbital distributions (§ 5.3). The effects of collisional evolution in the Main Belt and Kuiper Belt are discussed in the next two sections, along with the implications for the determination of the size distribution in the Main Belt (§ 5.4) and possibilities for identifying wide binaries and understanding the environment in the early outer Solar System in § 5.5. -
Occultations of HIP and UCAC2 Stars Downto 15M by Large TNO in 2004
Astronomy Letters, 2004, vol. 30. Translated from Pis’ma v Astronomicheskij Zhurnal. Occultations of HIP and UCAC2 stars downto 15m by large TNO in 2004-2014 © 2004 D.V. Denissenko Space Research Institute (IKI), Moscow, Russia Received 27 February 2004 Occultations of stars brighter than 15m by largest TNOs are predicted. Search was performed using the following catalogues: Hipparcos; Tycho2 with coordinates of 2838666 stars taken from UCAC2 (Herald, 2003); UCAC2 (Zacharias et al., 2003) with 16356096 stars between 12.00 and 14.99 mag to the north from -45 declination. Predictions were made for 17 largest numbered transneptunian asteroids, recently discovered 2004 DW and 4 known binary Kuiper Belt objects. 64 events occuring at solar elongation of 30° and more are selected, including exceptionally rare occultation m of 6.5 star by double (66652) 1999 RZ253 on 2007 October 4th. Observations of these events by all available means are extremely important since they can provide unique information about the size of TNOs and improve their orbits dramatically. INTRODUCTION OCCULTATIONS BY TNO Over 800 Transneptunian Objects (TNO) are TNOs are typically at 30-50 AU distances discovered since 1992 with 67 of them being from the Earth corresponding to 0.2"-0.3" numbered and 7 having proper names as of parallax. This means that occultation will February 2004. No reliable measurements only happen somewhere on the Earth if the of their sizes have been obtained so far. geocentric path of the object passes within Angular sizes even of the largest objects are 200-300 mas from the star. Combined with arXiv:astro-ph/0403002 28 Feb 2004 about 0.04"±0.01" (Quaoar) which is at the a very slow angular motion of TNO (0.1-1 limit of Hubble Space Telescope resolution. -
Hesiod Theogony.Pdf
Hesiod (8th or 7th c. BC, composed in Greek) The Homeric epics, the Iliad and the Odyssey, are probably slightly earlier than Hesiod’s two surviving poems, the Works and Days and the Theogony. Yet in many ways Hesiod is the more important author for the study of Greek mythology. While Homer treats cer- tain aspects of the saga of the Trojan War, he makes no attempt at treating myth more generally. He often includes short digressions and tantalizes us with hints of a broader tra- dition, but much of this remains obscure. Hesiod, by contrast, sought in his Theogony to give a connected account of the creation of the universe. For the study of myth he is im- portant precisely because his is the oldest surviving attempt to treat systematically the mythical tradition from the first gods down to the great heroes. Also unlike the legendary Homer, Hesiod is for us an historical figure and a real per- sonality. His Works and Days contains a great deal of autobiographical information, in- cluding his birthplace (Ascra in Boiotia), where his father had come from (Cyme in Asia Minor), and the name of his brother (Perses), with whom he had a dispute that was the inspiration for composing the Works and Days. His exact date cannot be determined with precision, but there is general agreement that he lived in the 8th century or perhaps the early 7th century BC. His life, therefore, was approximately contemporaneous with the beginning of alphabetic writing in the Greek world. Although we do not know whether Hesiod himself employed this new invention in composing his poems, we can be certain that it was soon used to record and pass them on. -
Journal Pre-Proof
Journal Pre-proof A statistical review of light curves and the prevalence of contact binaries in the Kuiper Belt Mark R. Showalter, Susan D. Benecchi, Marc W. Buie, William M. Grundy, James T. Keane, Carey M. Lisse, Cathy B. Olkin, Simon B. Porter, Stuart J. Robbins, Kelsi N. Singer, Anne J. Verbiscer, Harold A. Weaver, Amanda M. Zangari, Douglas P. Hamilton, David E. Kaufmann, Tod R. Lauer, D.S. Mehoke, T.S. Mehoke, J.R. Spencer, H.B. Throop, J.W. Parker, S. Alan Stern, the New Horizons Geology, Geophysics, and Imaging Team PII: S0019-1035(20)30444-9 DOI: https://doi.org/10.1016/j.icarus.2020.114098 Reference: YICAR 114098 To appear in: Icarus Received date: 25 November 2019 Revised date: 30 August 2020 Accepted date: 1 September 2020 Please cite this article as: M.R. Showalter, S.D. Benecchi, M.W. Buie, et al., A statistical review of light curves and the prevalence of contact binaries in the Kuiper Belt, Icarus (2020), https://doi.org/10.1016/j.icarus.2020.114098 This is a PDF file of an article that has undergone enhancements after acceptance, such as the addition of a cover page and metadata, and formatting for readability, but it is not yet the definitive version of record. This version will undergo additional copyediting, typesetting and review before it is published in its final form, but we are providing this version to give early visibility of the article. Please note that, during the production process, errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain.