Contents 2 Jan

Total Page:16

File Type:pdf, Size:1020Kb

Contents 2 Jan Mars shines brilliantly and looms large through a telescope this year as it puts on its best display in more than 10 years. NASA/JPL/USGS By Martin Ratcliffe Skyand Richard Talcott Guide 2016 contents 2 Jan. 2016 A stellar year for Aldebaran 3 Feb. 2016 Jupiter blazes across Leo 4 March 2016 Eclipse over Indonesia 5 April 2016 The Red Planet returns to glory 6 May 2016 Mercury transits the Sun 7 June 2016 Saturn’s summer splendor 8 July 2016 Tracking a recently exposed planet 9 Aug. 2016 The Perseids in prime time 10 Sept. 2016 Ice giants come in from the cold 11 Oct. 2016 Brilliant Venus rules the evening sky 12 Nov. 2016 The Sun’s dynamic face 13 Dec. 2016 A fleeting glimpse of Mercury 14 2017 Preview Looking ahead to next year . Martin Ratcliffe provides professional planetarium development for Sky-Skan, Inc. 15 Spacecraft A year of exploration Richard Talcott is a senior editor of Astronomy. 618329 A supplement to Astronomy magazine 2016 Jan S M T W T F S A stellar year for 1 3 4 5 6 7 8 10 11 12 13 14 15 Aldebaran 17 18 19 20 21 22 24 25 26 27 28 29 30 uring its monthly out. The star’s orbit around decline may be pro- Earth, the Moon longed if you live passes in front where the occul- 3 The Moon passes of thousands of tation occurs near 1.5° north of Mars, stars. Most of these distant suns the Moon’s curved 2 P.M. EST D are faint, however, and the so- northern or south- 4 Quadrantid meteor shower peaks called occultations that result ern limb. pass with little notice. Just four A few people 5 Pluto is in conjunc- tion with the Sun, 1st-magnitude stars — Aldeba- will get to witness a 10 P.M. EST ran, Antares, Regulus, and drama-filled grazing 6 Venus passes 6° Spica — lie close enough to the occultation. If you north of Antares, Moon’s path to get in on the view from a line that noon EST action. Aldebaran is 2016’s runs across north- The Moon passes clear winner, with the Moon ern Mexico and the 3° north of Venus, occulting it a dozen times. U.S. Gulf Coast (see 7 P.M. EST Ruddy Aldebaran sat to the upper right of a The best event for North the map below), crescent Moon August 9, 2015. A gibbous Moon The Moon passes American observers occurs the Aldebaran will skim occults the same star January 19. Tunç Tezel 3° north of Saturn, midnight EST evening of January 19. Resi- the Moon’s southern dents across Canada, most of limb, ducking behind though not all of these events 8 Venus passes 0.09° north of Saturn, the United States, and north- mountain ranges and reappear- are created equal. Some of the 11 P.M. EST western Mexico will see an ing in lunar valleys. This graze occultations occur when the 13 The Moon passes occultation. Set up early and track is only a few miles wide, Moon and star lie below the 2° north of Nep- center Aldebaran in your tele- but serious observers often horizon, and others when the tune, 10 A.M. EST scope’s eyepiece. Gradually, the travel large distances to be in Sun shares the sky and reduces 16 The Moon passes dark limb of the waxing gib- the path. Accurately timing the drama. 1.5° south of Ura- bous Moon will approach the when the star disappears and North American observers nus, 1 A.M. EST star. Although most stars dis- reappears gives astronomers have seven opportunities to 19 The Moon passes appear from view instanta- precise information about the see Aldebaran pass behind the 0.5° north of Aldeb- aran, 10 P.M. EST neously, Aldebaran is a red Moon’s limb profile. Moon during 2016. Events giant and likely will take a The Moon occults Aldeba- occur January 19, February 27 The Moon passes 1.4° south of Jupi- tenth of a second or so to fade ran once each orbit this year, 15/16 (western U.S. only), ter, 8 P.M. EST April 10 (daylight), July 29, CANADA August 25 (daylight), October Moon Phases 18/19, and December 12/13. Because the Moon’s orbit First Quarter lies close to the path of the Full Moon UNITED STATES solar system’s planets, Luna also occasionally occults one Last Quarter n of Earth’s neighbors. The best Aldebara New Moon cults n oc planetary occultation this year oo ble e M on visi The Moon’s comes September 2 when a Th ltati u southern limb Jaeger and Kellie : Roen Kelly occ No grazes Aldebaran 1.5-day-old Moon hides Jupi- Events that can be viewed M ter during daylight. Along with the naked eye E Astronomy X a track from Oregon to the Events that can be viewed I C 0 250 miles O Texas coast, the planet grazes with binoculars 0 500 km the northern lunar limb; peo- Events that can be viewed illustrations: All ple south of this line can view with a telescope People north of a line that runs across northern Mexico and southern Texas to the Georgia coast CIR-PB-618329_20will see the Moon occult Aldebaran on January 19. a complete occultation. 2 Sky Guide 2016 2016 Feb Jupiter blazes S M T W T F S 1 2 3 4 5 6 7 9 10 11 12 13 across Leo 14 16 17 18 19 20 21 23 24 25 26 27 28 29 upiter puts on an the star, impressive show and Jupiter throughout this appears as winter and spring. if it has Although it doesn’t gained a 1 The Moon passes 3° north of Mars, reach opposition and peak moon. J 4 A.M. EST visibility until March 8, few Jupiter 3 The Moon passes observers will notice any reaches oppo- 3° north of Saturn, difference in its appearance sition March 8, 2 P.M. EST during the longer nights of when it shines 6 The Moon passes January and February. brightest (magnitude 4° north of Venus, As 2016 opens, Jupiter –2.5) and remains visible all 3 A.M. EST Jupiter will look striking through dominates the late evening night. It is unmistakable in the amateur telescopes in the first The Moon passes sky. It rises before 11 p.m. local east as soon as night starts to half of 2016. The planet’s banded 4° north of Mer- time January 1 when it stands fall. The world also appears atmosphere and Great Red Spot cury, noon EST stand out in this image, captured Mercury is at in eastern Leo next to that largest at opposition, span- in December 2000 by the Cassini greatest western spacecraft. NASA/JPL/University of Arizona constellation’s border with ning 44" across its equator, elongation (26°), Virgo. The planet starts mov- though it stays above 43" from 8 P.M. EST ing westward relative to the early February to early April. near the planet, it means one 9 The Moon passes background stars just a week Any telescope delivers stun- or more of the moons is hiding 2° north of Nep- later, however, which carries it ning views of the giant planet. behind Jupiter’s disk or passing tune, 7 P.M. EST into the sparsely lit region of The smallest instruments in front of it. 12 The Moon passes southeastern Leo. Shining reveal two dark equatorial Larger scopes reveal finer 1.7° south of Ura- brighter than magnitude –2, belts straddling a brighter zone detail in the jovian atmosphere. nus, 9 A.M. EST Jupiter is the lone standout. that coincides with the planet’s A series of alternating bright 16 The Moon passes The giant world’s path has equator. Also look for Jupiter’s zones and darker belts comes 0.3° north of Aldeb- aran, 3 A.M. EST it heading straight for 4th- four biggest moons, which into view as do turbulent fea- σ 23 The Moon passes magnitude Sigma ( ) Leonis. change positions from night to tures in the swirl of clouds near 1.7° south of Jupi- On the night of March 2/3, the night and often by the hour. If the borders of these bands. ter, 11 P.M. EST planet passes just 14' south of you don’t see four bright dots Jupiter remains a fasci- 28 Neptune is in con- nating target throughout the junction with the N spring. On April 7/8, it slides Sun, 11 A.M. EST 7' north of 5th-magnitude Chi 29 The Moon passes (χ) Leonis. And it remains on 4° north of Mars, 1 P.M. EST LEO May 10 view past midnight local day- April 10 light time as late as early July. χ Although it dips lower as March 10 summer progresses, keep an E σ eye on Jupiter. On August 27, it has a fine conjunction with Feb 10 Jupiter reaches opposition March 8 Venus. The sky’s two brightest Jan 10 points of light then lie 5' apart and stand 5° above the western τ horizon 30 minutes after sun- 1° set. Jupiter passes behind the Sun in late September and a few weeks later returns to view The solar system’s biggest planet shines brilliantly nearly all night this winter and spring. It spendsCIR-PB-618329_21 this peak period in southeastern Leo, not far before dawn, where it remains from the border with Virgo.
Recommended publications
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • What Is the Color of Pluto? - Universe Today
    What is the Color of Pluto? - Universe Today space and astronomy news Universe Today Home Members Guide to Space Carnival Photos Videos Forum Contact Privacy Login NASA’s New Horizons spacecraft captured this high-resolution enhanced color view of http://www.universetoday.com/13866/color-of-pluto/[29-Mar-17 13:18:37] What is the Color of Pluto? - Universe Today Pluto on July 14, 2015. Credit: NASA/JHUAPL/SwRI WHAT IS THE COLOR OF PLUTO? Article Updated: 28 Mar , 2017 by Matt Williams When Pluto was first discovered by Clybe Tombaugh in 1930, astronomers believed that they had found the ninth and outermost planet of the Solar System. In the decades that followed, what little we were able to learn about this distant world was the product of surveys conducted using Earth-based telescopes. Throughout this period, astronomers believed that Pluto was a dirty brown color. In recent years, thanks to improved observations and the New Horizons mission, we have finally managed to obtain a clear picture of what Pluto looks like. In addition to information about its surface features, composition and tenuous atmosphere, much has been learned about Pluto’s appearance. Because of this, we now know that the one-time “ninth planet” of the Solar System is rich and varied in color. Composition: With a mean density of 1.87 g/cm3, Pluto’s composition is differentiated between an icy mantle and a rocky core. The surface is composed of more than 98% nitrogen ice, with traces of methane and carbon monoxide. Scientists also suspect that Pluto’s internal structure is differentiated, with the rocky material having settled into a dense core surrounded by a mantle of water ice.
    [Show full text]
  • Jjmonl 1710.Pmd
    alactic Observer John J. McCarthy Observatory G Volume 10, No. 10 October 2017 The Last Waltz Cassini’s final mission and dance of death with Saturn more on page 4 and 20 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 INTERNATIONAL OBSERVE THE MOON NIGHT ...................... 4 SOLAR ACTIVITY ........................................................... 19 MONTE APENNINES AND APOLLO 15 .................................. 5 COMMONLY USED TERMS ............................................... 19 FAREWELL TO RING WORLD ............................................ 5 FRONT PAGE ...............................................................
    [Show full text]
  • Chemical Evolution of the Galactic Bulge As Traced by Microlensed Dwarf and Subgiant Stars: II
    UvA-DARE (Digital Academic Repository) Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars: II. Ages, metallicities, detailed elemental abundances, and connections to the Galactic thick disc Bensby, T.; Feltzing, S.; Johnson, J.A.; Gould, A.; Adén, D.; Asplund, M.; Meléndez, J.; Gal- Yam, A.; Lucatello, S.; Sana, H.; Sumi, T.; Miyake, N.; Suzuki, D.; Han, C.; Bond, I.; Udalski, A. DOI 10.1051/0004-6361/200913744 Publication date 2010 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Bensby, T., Feltzing, S., Johnson, J. A., Gould, A., Adén, D., Asplund, M., Meléndez, J., Gal- Yam, A., Lucatello, S., Sana, H., Sumi, T., Miyake, N., Suzuki, D., Han, C., Bond, I., & Udalski, A. (2010). Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars: II. Ages, metallicities, detailed elemental abundances, and connections to the Galactic thick disc. Astronomy & Astrophysics, 512, A41. https://doi.org/10.1051/0004- 6361/200913744 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material UvA-DAREinaccessible is a serviceand/or provided remove by it the from library the of website.
    [Show full text]
  • 16Th HEAD Meeting Session Table of Contents
    16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113
    [Show full text]
  • Astronomy with Small Telescopes
    Astronomy With Small Telescopes Bohdan Paczy´nski Princeton University Observatory, Princeton, NJ 08544 [email protected] ABSTRACT The All Sky Automated Survey (ASAS) is monitoring all sky to about 14 mag with a cadence of about 1 day; it has discovered about 105 variable stars, most of them new. The instrument used for the survey had aperture of 7 cm. A search for planetary transits has lead to the discovery of about a dozen confirmed planets, so called ’hot Jupiters’, providing the information of planetary masses and radii. Most discoveries were done with telescopes with aperture of 10 cm. We propose a search for optical transients covering all sky with a cadence of 10 - 30 minutes and the limit of 12 - 14 mag, with an instant verification of all candidate events. The search will be made with a large number of 10 cm instruments, and the verification will be done with 30 cm instruments. We also propose a system to be located at the L1 point of the Earth - Sun system to detect ’killer asteroids’. With a limiting magnitude of about 18 mag it could detect 10 m boulders several hours prior to their impact, provide warning against Tunguska-like events, as well as to provide news about spectacular but harmless more modest impacts. Subject headings: techniques: photometric — surveys — celestial mechanics — mete- oroids — stars: variable — gamma rays: bursts arXiv:astro-ph/0609161v3 7 Nov 2006 1. Introduction The goal of this paper is to point out that there are many tasks for which small and even very small telescopes are not only useful, but even indispensable.
    [Show full text]
  • Cosmological Narrative in the Synagogues of Late Roman-Byzantine Palestine
    COSMOLOGICAL NARRATIVE IN THE SYNAGOGUES OF LATE ROMAN-BYZANTINE PALESTINE Bradley Charles Erickson A dissertation submitted to the faculty of the University of North Carolina at Chapel Hill in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Religious Studies. Chapel Hill 2020 Approved by: Jodi Magness Zlatko Plese David Lambert Jennifer Gates-Foster Maurizio Forte © 2020 Bradley Charles Erickson ALL RIGHTS RESERVED ii ABSTRACT Bradley Charles Erickson: Cosmological Narrative in the Synagogues of Late Roman-Byzantine Palestine (Under the Direction of Jodi Magness) The night sky provided ancient peoples with a visible framework through which they could view and experience the divine. Ancient astronomers looked to the night sky for practical reasons, such as the construction of calendars by which time could evenly be divided, and for prognosis, such as the foretelling of future events based on the movements of the planets and stars. While scholars have written much about the Greco-Roman understanding of the night sky, few studies exist that examine Jewish cosmological thought in relation to the appearance of the Late Roman-Byzantine synagogue Helios-zodiac cycle. This dissertation surveys the ways that ancient Jews experienced the night sky, including literature of the Second Temple (sixth century BCE – 70 CE), rabbinic and mystical writings, and Helios-zodiac cycles in synagogues of ancient Palestine. I argue that Judaism joined an evolving Greco-Roman cosmology with ancient Jewish traditions as a means of producing knowledge of the earthly and heavenly realms. iii ACKNOWLEDGEMENTS I wish to express my sincere appreciation to my adviser, Dr.
    [Show full text]
  • GTO Keypad Manual, V5.001
    ASTRO-PHYSICS GTO KEYPAD Version v5.xxx Please read the manual even if you are familiar with previous keypad versions Flash RAM Updates Keypad Java updates can be accomplished through the Internet. Check our web site www.astro-physics.com/software-updates/ November 11, 2020 ASTRO-PHYSICS KEYPAD MANUAL FOR MACH2GTO Version 5.xxx November 11, 2020 ABOUT THIS MANUAL 4 REQUIREMENTS 5 What Mount Control Box Do I Need? 5 Can I Upgrade My Present Keypad? 5 GTO KEYPAD 6 Layout and Buttons of the Keypad 6 Vacuum Fluorescent Display 6 N-S-E-W Directional Buttons 6 STOP Button 6 <PREV and NEXT> Buttons 7 Number Buttons 7 GOTO Button 7 ± Button 7 MENU / ESC Button 7 RECAL and NEXT> Buttons Pressed Simultaneously 7 ENT Button 7 Retractable Hanger 7 Keypad Protector 8 Keypad Care and Warranty 8 Warranty 8 Keypad Battery for 512K Memory Boards 8 Cleaning Red Keypad Display 8 Temperature Ratings 8 Environmental Recommendation 8 GETTING STARTED – DO THIS AT HOME, IF POSSIBLE 9 Set Up your Mount and Cable Connections 9 Gather Basic Information 9 Enter Your Location, Time and Date 9 Set Up Your Mount in the Field 10 Polar Alignment 10 Mach2GTO Daytime Alignment Routine 10 KEYPAD START UP SEQUENCE FOR NEW SETUPS OR SETUP IN NEW LOCATION 11 Assemble Your Mount 11 Startup Sequence 11 Location 11 Select Existing Location 11 Set Up New Location 11 Date and Time 12 Additional Information 12 KEYPAD START UP SEQUENCE FOR MOUNTS USED AT THE SAME LOCATION WITHOUT A COMPUTER 13 KEYPAD START UP SEQUENCE FOR COMPUTER CONTROLLED MOUNTS 14 1 OBJECTS MENU – HAVE SOME FUN!
    [Show full text]
  • Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗
    Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗ Mario Mateo1 e-mail: [email protected] Edward W. Olszewski2 e-mail: [email protected] Heather L. Morrison3 e-mail: [email protected] Received ; accepted ∗BasedonobservationsobtainedwiththeBlancoTelescopeatCTIO,whichisoperated by the National Optical Astronomy Observatory, under contract to AURA. 1Department of Astronomy, University of Michigan, 821 Dennison Bldg., Ann Arbor, MI 48109–1090 2Steward Observatory, 933 N. Cherry, University of Arizona, Tucson, AZ 85721-0065 3Cottrell Scholar of Research Corporation, and NSF Career Fellow; Department of Astronomy and Department of Physics, Case Western Reserve University, Cleveland OH 44106 –2– ABSTRACT We have obtained deep photometric data in 24 fields along the southeast extension of the major axis of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy, and in four fields along the northwest extension. Using star counts at the expected position of the Sgr upper main-sequence within the resulting color-magnitude diagrams (CMDs), we unambiguously detect Sgr stars in the southeast over the range 10–34◦ from the galaxy’s center. If Sgr is symmetric, this implies a true major-axis diameter of at least 68◦, or nearly 30 kpc if all portions of Sgr are equally distant from the Sun. Star counts parallel to the galaxy’s minor-axis reveal that Sgr remains quite broad far from its center. This suggests that the outer portions of Sgr resemble a stream rather than an extension of the ellipsoidal inner regions of the galaxy. The inferred V-band surface brightness (SB) profile ranges from 27.3-30.5 mag arcsec−2 over this radial range and exhibits a change in slope ∼ 20◦ from the center of Sgr.
    [Show full text]
  • A Tale of Two Sides: Pluto's Opposition Surge in 2018 and 2019
    EPSC Abstracts Vol. 14, EPSC2020-546, 2020, updated on 27 Sep 2021 https://doi.org/10.5194/epsc2020-546 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. A Tale of Two Sides: Pluto's Opposition Surge in 2018 and 2019 Anne Verbiscer1, Paul Helfenstein2, Mark Showalter3, and Marc Buie4 1University of Virginia, Charlottesville, VA, USA ([email protected]) 2Cornell University, Ithaca, NY, USA ([email protected]) 3SETI Institute, Mountain View, CA, USA ([email protected]) 4Southwest Research Institute, Boulder, CO, USA ([email protected]) Near-opposition photometry employs remote sensing observations to reveal the microphysical properties of regolith-covered surfaces over a wide range of solar system bodies. When aligned directly opposite the Sun, objects exhibit an opposition effect, or surge, a dramatic, non-linear increase in reflectance seen with decreasing solar phase angle (the Sun-target-observer angle). This phenomenon is a consequence of both interparticle shadow hiding and a constructive interference phenomenon known as coherent backscatter [1-3]. While the size of the Earth’s orbit restricts observations of Pluto and its moons to solar phase angles no larger than α = 1.9°, the opposition surge, which occurs largely at α < 1°, can discriminate surface properties [4-6]. The smallest solar phase angles are attainable at node crossings when the Earth transits the solar disk as viewed from the object. In this configuration, a solar system body is at “true” opposition. When combined with observations acquired at larger phase angles, the resulting reflectance measurement can be related to the optical, structural, and thermal properties of the regolith and its inferred collisional history.
    [Show full text]
  • Pluto's Far Side
    Pluto’s Far Side S.A. Stern Southwest Research Institute O.L. White SETI Institute P.J. McGovern Lunar and Planetary Institute J.T. Keane California Institute of Technology J.W. Conrad, C.J. Bierson University of California, Santa Cruz C.B. Olkin Southwest Research Institute P.M. Schenk Lunar and Planetary Institute J.M. Moore NASA Ames Research Center K.D. Runyon Johns Hopkins University, Applied Physics Laboratory and The New Horizons Team 1 Abstract The New Horizons spacecraft provided near-global observations of Pluto that far exceed the resolution of Earth-based datasets. Most Pluto New Horizons analysis hitherto has focused on Pluto’s encounter hemisphere (i.e., the anti-Charon hemisphere containing Sputnik Planitia). In this work, we summarize and interpret data on Pluto’s “far side” (i.e., the non-encounter hemisphere), providing the first integrated New Horizons overview of Pluto’s far side terrains. We find strong evidence for widespread bladed deposits, evidence for an impact crater about as large as any on the “near side” hemisphere, evidence for complex lineations approximately antipodal to Sputnik Planitia that may be causally related, and evidence that the far side maculae are smaller and more structured than Pluto’s encounter hemisphere maculae. 2 Introduction Before the 2015 exploration of Pluto by New Horizons (e.g., Stern et al. 2015, 2018 and references therein) none of Pluto’s surface features were known except by crude (though heroically derived) albedo maps, with resolutions of 300-500 km obtainable from the Hubble Space Telescope (e.g., Buie et al. 1992, 1997, 2010) and Pluto-Charon mutual event techniques (e.g., Young & Binzel 1993, Young et al.
    [Show full text]
  • OGLE 2004-BLG-254: a K3 III Galactic Bulge Giant Spatially Resolved by A
    Astronomy & Astrophysics manuscript no. 4414arti c ESO 2018 January 9, 2018 OGLE 2004–BLG–254: a K3 III Galactic Bulge Giant spatially resolved by a single microlens⋆ A. Cassan1,2,3, J.-P. Beaulieu1,3, P. Fouqu´e1,4, S. Brillant1,5, M. Dominik1,6, J. Greenhill1,7, D. Heyrovsk´y8, K. Horne1,6, U.G. Jørgensen1,9, D. Kubas1,5, H.C. Stempels6, C. Vinter1,9, M.D. Albrow1,12, D. Bennett1,13, J.A.R. Caldwell1,14,15, J.J. Calitz1,16, K. Cook1,17, C. Coutures1,18, D. Dominis1,19, J. Donatowicz1,20, K. Hill1,7, M. Hoffman1,16, S. Kane1,21, J.-B. Marquette1,3, R. Martin1,22, P. Meintjes1,16, J. Menzies1,23, V.R. Miller12, K.R. Pollard1,12, K.C. Sahu1,14, J. Wambsganss1,2, A. Williams1,22, A. Udalski10,11, M.K. Szyma´nski10,11, M. Kubiak10,11, G. Pietrzy´nski10,11,24, I. Soszy´nski10,11,24, K. Zebru´n˙ 10,11, O. Szewczyk10,11, and Ł. Wyrzykowski10,11,25 (Affiliations can be found after the references) Received ¡date¿ / Accepted ¡date¿ ABSTRACT Aims. We present an analysis of OGLE 2004–BLG–254, a high-magnification (A 60) and relatively short duration (tE 13.2 days) microlensing event in which the source star, a Bulge K-giant, has been spatially resolved◦ ≃ by a point-like lens. We seek to determine≃ the lens and source distance, and provide a measurement of the linear limb-darkening coefficients of the source star in the I and R bands. We discuss the derived values of the latter and compare them to the classical theoretical laws, and furthermore examine the cases of already published microlensed GK-giants limb-darkening measurements.
    [Show full text]