Interaction Mechanism and Response of Tidal Effect on the Shallow Geology of Europa Yifei Wang 1 ABSTRACT 1. INTRODUCTION 2
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Constraints on the Habitability of Extrasolar Moons
Formation, Detection, and Characterization of Extrasolar Habitable Planets Proceedings IAU Symposium No. 293, 2012 c International Astronomical Union 2014 N. Haghighipour, ed. doi:10.1017/S1743921313012738 Constraints on the Habitability of Extrasolar Moons Ren´e Heller1 and Rory Barnes2,3 1 Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam email: [email protected] 2 University of Washington, Dept. of Astronomy, Seattle, WA 98195, USA 3 Virtual Planetary Laboratory, NASA, USA email: [email protected] Abstract. Detections of massive extrasolar moons are shown feasible with the Kepler space telescope. Kepler’s findings of about 50 exoplanets in the stellar habitable zone naturally make us wonder about the habitability of their hypothetical moons. Illumination from the planet, eclipses, tidal heating, and tidal locking distinguish remote characterization of exomoons from that of exoplanets. We show how evaluation of an exomoon’s habitability is possible based on the parameters accessible by current and near-future technology. Keywords. celestial mechanics – planets and satellites: general – astrobiology – eclipses 1. Introduction The possible discovery of inhabited exoplanets has motivated considerable efforts towards estimating planetary habitability. Effects of stellar radiation (Kasting et al. 1993; Selsis et al. 2007), planetary spin (Williams & Kasting 1997; Spiegel et al. 2009), tidal evolution (Jackson et al. 2008; Barnes et al. 2009; Heller et al. 2011), and composition (Raymond et al. 2006; Bond et al. 2010) have been studied. Meanwhile, Kepler’s high precision has opened the possibility of detecting extrasolar moons (Kipping et al. 2009; Tusnski & Valio 2011) and the first dedicated searches for moons in the Kepler data are underway (Kipping et al. -
Rare Astronomical Sights and Sounds
Jonathan Powell Rare Astronomical Sights and Sounds The Patrick Moore The Patrick Moore Practical Astronomy Series More information about this series at http://www.springer.com/series/3192 Rare Astronomical Sights and Sounds Jonathan Powell Jonathan Powell Ebbw Vale, United Kingdom ISSN 1431-9756 ISSN 2197-6562 (electronic) The Patrick Moore Practical Astronomy Series ISBN 978-3-319-97700-3 ISBN 978-3-319-97701-0 (eBook) https://doi.org/10.1007/978-3-319-97701-0 Library of Congress Control Number: 2018953700 © Springer Nature Switzerland AG 2018 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. The use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. The publisher, the authors, and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made. -
18Th EANA Conference European Astrobiology Network Association
18th EANA Conference European Astrobiology Network Association Abstract book 24-28 September 2018 Freie Universität Berlin, Germany Sponsors: Detectability of biosignatures in martian sedimentary systems A. H. Stevens1, A. McDonald2, and C. S. Cockell1 (1) UK Centre for Astrobiology, University of Edinburgh, UK ([email protected]) (2) Bioimaging Facility, School of Engineering, University of Edinburgh, UK Presentation: Tuesday 12:45-13:00 Session: Traces of life, biosignatures, life detection Abstract: Some of the most promising potential sampling sites for astrobiology are the numerous sedimentary areas on Mars such as those explored by MSL. As sedimentary systems have a high relative likelihood to have been habitable in the past and are known on Earth to preserve biosignatures well, the remains of martian sedimentary systems are an attractive target for exploration, for example by sample return caching rovers [1]. To learn how best to look for evidence of life in these environments, we must carefully understand their context. While recent measurements have raised the upper limit for organic carbon measured in martian sediments [2], our exploration to date shows no evidence for a terrestrial-like biosphere on Mars. We used an analogue of a martian mudstone (Y-Mars[3]) to investigate how best to look for biosignatures in martian sedimentary environments. The mudstone was inoculated with a relevant microbial community and cultured over several months under martian conditions to select for the most Mars-relevant microbes. We sequenced the microbial community over a number of transfers to try and understand what types microbes might be expected to exist in these environments and assess whether they might leave behind any specific biosignatures. -
Pluto and Charon
National Aeronautics and Space Administration 0 300,000,000 900,000,000 1,500,000,000 2,100,000,000 2,700,000,000 3,300,000,000 3,900,000,000 4,500,000,000 5,100,000,000 5,700,000,000 kilometers Pluto and Charon www.nasa.gov Pluto is classified as a dwarf planet and is also a member of a Charon’s orbit around Pluto takes 6.4 Earth days, and one Pluto SIGNIFICANT DATES group of objects that orbit in a disc-like zone beyond the orbit of rotation (a Pluto day) takes 6.4 Earth days. Charon neither rises 1930 — Clyde Tombaugh discovers Pluto. Neptune called the Kuiper Belt. This distant realm is populated nor sets but “hovers” over the same spot on Pluto’s surface, 1977–1999 — Pluto’s lopsided orbit brings it slightly closer to with thousands of miniature icy worlds, which formed early in the and the same side of Charon always faces Pluto — this is called the Sun than Neptune. It will be at least 230 years before Pluto history of the solar system. These icy, rocky bodies are called tidal locking. Compared with most of the planets and moons, the moves inward of Neptune’s orbit for 20 years. Kuiper Belt objects or transneptunian objects. Pluto–Charon system is tipped on its side, like Uranus. Pluto’s 1978 — American astronomers James Christy and Robert Har- rotation is retrograde: it rotates “backwards,” from east to west Pluto’s 248-year-long elliptical orbit can take it as far as 49.3 as- rington discover Pluto’s unusually large moon, Charon. -
Solar System
Lecture 2 Solar system Beibei Liu (刘倍⻉) Introduction to Astrophysics, 2019 What is planet? Definition of planet 1. It orbits the sun (central star) 2. It has sufficient mass to have its self-gravity to overcome rigid bodies force, so that in a hydrostatic equilibrium (near round and stable shape) 3. Its perturbations have cleared away other objects in the neighbourhood of its orbit. asteroid, comet, moon, pluto? Moon-Earth system: Tidal force Tidal locking (tidal synchronisation): spin period of the moon is equal to the orbital period of the Earth-Moon system (~28 days). Moon-Earth system: Tidal force Earth rotation is only 24 hours Earth slowly decreases its rotation, and moon’s orbital distance gradually increases Lunar and solar eclipse Blood moon, sun’s light refracted by earth’s atmosphere. Due to Rayleigh scattering, red color is easy to remain Solar system Terrestrial planets Gas giant planets ice giant planets Heat source of the planet 1. Gravitational contraction: release potential energy 2. Decay of radioactive isotope,such as potassium, uranium 3. Giant impacts, planetesimal accretion Melting and differentiation of planet interior Originally homogeneous material begin to segregate into layers of different chemical composition. Heavy elements sink into the centre. Interior of planets Relative core size Interior of planets Metallic hydrogen: high pressure, H2 dissociate into atoms and become electronic conducting. Magnetic field is generated in this layer. Earth interior layers Crust (rigid): granite and basalt Silicate mantle: flow and convection Fe-Ni core: T~4000-9000K Magnetic field is generated by electric currents due to large convective motion of molten metal in outer core and mantle Earth interior layers Tectonics motion Large scale movement of plates in Earth’s lithosphere. -
Tellurium Tellurium N
Experiment Description/Manual Tellurium Tellurium N Table of contents General remarks ............................................................................................................................3 Important parts of the Tellurium and their operation .....................................................................4 Teaching units for working with the Tellurium: Introduction: From one´s own shadow to the shadow-figure on the globe of the Tellurium ...........6 1. The earth, a gyroscope in space ............................................................................................8 2. Day and night ..................................................................................................................... 10 3. Midday line and division of hours ....................................................................................... 13 4. Polar day and polar night .................................................................................................... 16 5. The Tropic of Cancer and Capricorn and the tropics ........................................................... 17 6. The seasons ........................................................................................................................ 19 7. Lengths of day and night in various latitudes ......................................................................22 Working sheet “Lengths of day in various seasons” ............................................................ 24 8. The times of day .................................................................................................................25 -
Lunar Laser Ranging: the Millimeter Challenge
REVIEW ARTICLE Lunar Laser Ranging: The Millimeter Challenge T. W. Murphy, Jr. Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0424, USA E-mail: [email protected] Abstract. Lunar laser ranging has provided many of the best tests of gravitation since the first Apollo astronauts landed on the Moon. The march to higher precision continues to this day, now entering the millimeter regime, and promising continued improvement in scientific results. This review introduces key aspects of the technique, details the motivations, observables, and results for a variety of science objectives, summarizes the current state of the art, highlights new developments in the field, describes the modeling challenges, and looks to the future of the enterprise. PACS numbers: 95.30.Sf, 04.80.-y, 04.80.Cc, 91.4g.Bg arXiv:1309.6294v1 [gr-qc] 24 Sep 2013 CONTENTS 2 Contents 1 The LLR concept 3 1.1 Current Science Results . 4 1.2 A Quantitative Introduction . 5 1.3 Reflectors and Divergence-Imposed Requirements . 5 1.4 Fundamental Measurement and World Lines . 10 2 Science from LLR 12 2.1 Relativity and Gravity . 12 2.1.1 Equivalence Principle . 13 2.1.2 Time-rate-of-change of G ....................... 14 2.1.3 Gravitomagnetism, Geodetic Precession, and other PPN Tests . 14 2.1.4 Inverse Square Law, Extra Dimensions, and other Frontiers . 16 2.2 Lunar and Earth Physics . 16 2.2.1 The Lunar Interior . 16 2.2.2 Earth Orientation, Precession, and Coordinate Frames . 18 3 LLR Capability across Time 20 3.1 Brief LLR History . -
Moon-Earth-Sun: the Oldest Three-Body Problem
Moon-Earth-Sun: The oldest three-body problem Martin C. Gutzwiller IBM Research Center, Yorktown Heights, New York 10598 The daily motion of the Moon through the sky has many unusual features that a careful observer can discover without the help of instruments. The three different frequencies for the three degrees of freedom have been known very accurately for 3000 years, and the geometric explanation of the Greek astronomers was basically correct. Whereas Kepler’s laws are sufficient for describing the motion of the planets around the Sun, even the most obvious facts about the lunar motion cannot be understood without the gravitational attraction of both the Earth and the Sun. Newton discussed this problem at great length, and with mixed success; it was the only testing ground for his Universal Gravitation. This background for today’s many-body theory is discussed in some detail because all the guiding principles for our understanding can be traced to the earliest developments of astronomy. They are the oldest results of scientific inquiry, and they were the first ones to be confirmed by the great physicist-mathematicians of the 18th century. By a variety of methods, Laplace was able to claim complete agreement of celestial mechanics with the astronomical observations. Lagrange initiated a new trend wherein the mathematical problems of mechanics could all be solved by the same uniform process; canonical transformations eventually won the field. They were used for the first time on a large scale by Delaunay to find the ultimate solution of the lunar problem by perturbing the solution of the two-body Earth-Moon problem. -
The Moon and Eclipses
Lecture 10 The Moon and Eclipses Jiong Qiu, MSU Physics Department Guiding Questions 1. Why does the Moon keep the same face to us? 2. Is the Moon completely covered with craters? What is the difference between highlands and maria? 3. Does the Moon’s interior have a similar structure to the interior of the Earth? 4. Why does the Moon go through phases? At a given phase, when does the Moon rise or set with respect to the Sun? 5. What is the difference between a lunar eclipse and a solar eclipse? During what phases do they occur? 6. How often do lunar eclipses happen? When one is taking place, where do you have to be to see it? 7. How often do solar eclipses happen? Why are they visible only from certain special locations on Earth? 10.1 Introduction The moon looks 14% bigger at perigee than at apogee. The Moon wobbles. 59% of its surface can be seen from the Earth. The Moon can not hold the atmosphere The Moon does NOT have an atmosphere and the Moon does NOT have liquid water. Q: what factors determine the presence of an atmosphere? The Moon probably formed from debris cast into space when a huge planetesimal struck the proto-Earth. 10.2 Exploration of the Moon Unmanned exploration: 1950, Lunas 1-3 -- 1960s, Ranger -- 1966-67, Lunar Orbiters -- 1966-68, Surveyors (first soft landing) -- 1966-76, Lunas 9-24 (soft landing) -- 1989-93, Galileo -- 1994, Clementine -- 1998, Lunar Prospector Achievement: high-resolution lunar surface images; surface composition; evidence of ice patches around the south pole. -
L1 Lunar Lander Element Conceptual Design Report
EX15-01-092 L1 Lunar Lander Element Conceptual Design Report Engineering Directorate November 2000 National Aeronautics and Space Administration Lyndon B. Johnson Space Center Houston, Texas 77058 Table Of Contents i List of Figures………………………………………………………………………….……………iv ii List of Tables……………………………………………………………………………….………. v iii Contact Information………………………………………………………………………………..vi iv Introduction……………...………………………………………………………………………….vii 1.0 Element Description……………………………………………………………………….………..1 1.1 Design Objectives, Constraints & Requirements……………………………….…………..1 1.2 Vehicle Configuration Trades………………………………………………….……………3 1.3 Operations Concept…………………………………………………………….……………5 1.4 Vehicle Mass Statement…………………………………………………..………………. 9 1.5 Power Profile………………………………………………………………..……………. 10 2.0 Propulsion System…………………………………………………………………..…………….. 12 2.1 Functional Description and Design Requirements…………………………..……………. 12 2.2 Trades Considered and Results……………………………………………..……………... 12 2.3 Reference Design Description………………………………………………..…………… 12 2.4 Technology Needs and Design Challenges…………………………………..…………….13 3.0 Structure..……………………………………………………………….………….……………….14 3.1 Functional Description and Design Requirements………………………………...……….14 3.2 Trades Considered and Results……………………………………………………………..15 3.3 Reference Design Description……………………………………………………...………15 3.4 Technology Needs and Design Challenges…………………………………………………16 4.0 Electrical Power System…………………………………………………………………………….17 4.1 Functional Description and Design Requirements………………………………………….17 4.2 Trades -
Analytical Formulation of Lunar Cratering Asymmetries Nan Wang (王楠) and Ji-Lin Zhou (周济林)
A&A 594, A52 (2016) Astronomy DOI: 10.1051/0004-6361/201628598 & c ESO 2016 Astrophysics Analytical formulation of lunar cratering asymmetries Nan Wang (王`) and Ji-Lin Zhou (hN林) School of Astronomy and Space Science and Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education, Nanjing University, 210046 Nanjing, PR China e-mail: [email protected] Received 28 March 2016 / Accepted 3 July 2016 ABSTRACT Context. The cratering asymmetry of a bombarded satellite is related to both its orbit and impactors. The inner solar system im- pactor populations, that is, the main-belt asteroids (MBAs) and the near-Earth objects (NEOs), have dominated during the late heavy bombardment (LHB) and ever since, respectively. Aims. We formulate the lunar cratering distribution and verify the cratering asymmetries generated by the MBAs as well as the NEOs. Methods. Based on a planar model that excludes the terrestrial and lunar gravitations on the impactors and assuming the impactor encounter speed with Earth venc is higher than the lunar orbital speed vM, we rigorously integrated the lunar cratering distribution, and derived its approximation to the first order of vM=venc. Numerical simulations of lunar bombardment by the MBAs during the LHB were performed with an Earth–Moon distance aM = 20−60 Earth radii in five cases. Results. The analytical model directly proves the existence of a leading/trailing asymmetry and the absence of near/far asymmetry. The approximate form of the leading/trailing asymmetry is (1+A1 cos β), which decreases as the apex distance β increases. The numer- ical simulations show evidence of a pole/equator asymmetry as well as the leading/trailing asymmetry, and the former is empirically described as (1 + A2 cos 2'), which decreases as the latitude modulus j'j increases. -
Iaa-Pdc-15-04-17 from Sail to Soil – Getting Sailcraft out of the Harbour on a Visit to One of Earth’S Nearest Neighbours
4th IAA Planetary Defense Conference – PDC 2015 13-17 April 2015, Frascati, Roma, Italy IAA-PDC-15-04-17 FROM SAIL TO SOIL – GETTING SAILCRAFT OUT OF THE HARBOUR ON A VISIT TO ONE OF EARTH’S NEAREST NEIGHBOURS Jan Thimo Grundmann(1,2), Waldemar Bauer(1,3), Jens Biele(8,9), Federico Cordero(11), Bernd Dachwald(12), Alexander Koncz(13,14), Christian Krause(8,10), Tobias Mikschl(16,17), Sergio Montenegro(16,18), Dominik Quantius(1,4), Michael Ruffer(16,19), Kaname Sasaki (1,5), Nicole Schmitz(13,15), Patric Seefeldt (1,6), Norbert Tóth(1,7), Elisabet Wejmo(1,8) (1)DLR Institute of Space Systems, Robert-Hooke-Strasse 7, 28359 Bremen (2)+49-(0)421-24420-1107, (3)+49-(0)421-24420-1197, (4)+49-(0)421-24420-1109, (5)+49-(0)421-24420-1150, (6)+49-(0)421-24420-1609, (7)+49-(0)421-24420-1186, (8)+49-(0)421-24420-1107, (11)DLR Space Operations and Astronaut Training – MUSC, 51147 Köln, Germany (9)+49-2203-601-4563, (10)+49-2203-601-3048, (11)Telespazio-VEGA, Darmstadt, Germany, [email protected] (12) Faculty of Aerospace Engineering, FH Aachen University of Applied Sciences, Hohenstaufenallee 6, 52064 Aachen, Germany, +49-241-6009-52343 / -52854, (13)DLR Institute of Planetary Research, Rutherfordstr. 2, 12489 Berlin (14)+49-(0)30 67055-575, (15)+49-(0)30 67055-456, (16)Informatik 8, Universität Würzburg, Am Hubland, 97074 Würzburg, Germany Keywords: small spacecraft, solar sail, GOSSAMER roadmap, MASCOT, co-orbital asteroid ABSTRACT The DLR-ESTEC GOSSAMER roadmap envisages the development of solar sailing by successive low-cost technology demonstrators towards first science missions.