Earth's Minimoons: Opportunities for Science and Technology
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The Surrender Software
Scientific image rendering for space scenes with the SurRender software Scientific image rendering for space scenes with the SurRender software R. Brochard, J. Lebreton*, C. Robin, K. Kanani, G. Jonniaux, A. Masson, N. Despré, A. Berjaoui Airbus Defence and Space, 31 rue des Cosmonautes, 31402 Toulouse Cedex, France [email protected] *Corresponding Author Abstract The autonomy of spacecrafts can advantageously be enhanced by vision-based navigation (VBN) techniques. Applications range from manoeuvers around Solar System objects and landing on planetary surfaces, to in -orbit servicing or space debris removal, and even ground imaging. The development and validation of VBN algorithms for space exploration missions relies on the availability of physically accurate relevant images. Yet archival data from past missions can rarely serve this purpose and acquiring new data is often costly. Airbus has developed the image rendering software SurRender, which addresses the specific challenges of realistic image simulation with high level of representativeness for space scenes. In this paper we introduce the software SurRender and how its unique capabilities have proved successful for a variety of applications. Images are rendered by raytracing, which implements the physical principles of geometrical light propagation. Images are rendered in physical units using a macroscopic instrument model and scene objects reflectance functions. It is specially optimized for space scenes, with huge distances between objects and scenes up to Solar System size. Raytracing conveniently tackles some important effects for VBN algorithms: image quality, eclipses, secondary illumination, subpixel limb imaging, etc. From a user standpoint, a simulation is easily setup using the available interfaces (MATLAB/Simulink, Python, and more) by specifying the position of the bodies (Sun, planets, satellites, …) over time, complex 3D shapes and material surface properties, before positioning the camera. -
Monte Carlo Methods to Calculate Impact Probabilities⋆
A&A 569, A47 (2014) Astronomy DOI: 10.1051/0004-6361/201423966 & c ESO 2014 Astrophysics Monte Carlo methods to calculate impact probabilities? H. Rickman1;2, T. Wisniowski´ 1, P. Wajer1, R. Gabryszewski1, and G. B. Valsecchi3;4 1 P.A.S. Space Research Center, Bartycka 18A, 00-716 Warszawa, Poland e-mail: [email protected] 2 Dept. of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden 3 IAPS-INAF, via Fosso del Cavaliere 100, 00133 Roma, Italy 4 IFAC-CNR, via Madonna del Piano 10, 50019 Sesto Fiorentino (FI), Italy Received 9 April 2014 / Accepted 28 June 2014 ABSTRACT Context. Unraveling the events that took place in the solar system during the period known as the late heavy bombardment requires the interpretation of the cratered surfaces of the Moon and terrestrial planets. This, in turn, requires good estimates of the statistical impact probabilities for different source populations of projectiles, a subject that has received relatively little attention, since the works of Öpik(1951, Proc. R. Irish Acad. Sect. A, 54, 165) and Wetherill(1967, J. Geophys. Res., 72, 2429). Aims. We aim to work around the limitations of the Öpik and Wetherill formulae, which are caused by singularities due to zero denominators under special circumstances. Using modern computers, it is possible to make good estimates of impact probabilities by means of Monte Carlo simulations, and in this work, we explore the available options. Methods. We describe three basic methods to derive the average impact probability for a projectile with a given semi-major axis, eccentricity, and inclination with respect to a target planet on an elliptic orbit. -
Can Moons Have Moons?
A MNRAS 000, 1–?? (2018) Preprint 23 January 2019 Compiled using MNRAS L TEX style file v3.0 Can Moons Have Moons? Juna A. Kollmeier1⋆ & Sean N. Raymond2† 1 Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 2 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, all´eGeoffroy Saint-Hilaire, 33615 Pessac, France Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Each of the giant planets within the Solar System has large moons but none of these moons have their own moons (which we call submoons). By analogy with studies of moons around short-period exoplanets, we investigate the tidal-dynamical stability of submoons. We find that 10 km-scale submoons can only survive around large (1000 km-scale) moons on wide-separation orbits. Tidal dissipation destabilizes the orbits of submoons around moons that are small or too close to their host planet; this is the case for most of the Solar System’s moons. A handful of known moons are, however, capable of hosting long-lived submoons: Saturn’s moons Titan and Iapetus, Jupiter’s moon Callisto, and Earth’s Moon. Based on its inferred mass and orbital separation, the newly-discovered exomoon candidate Kepler-1625b-I can in principle host a large submoon, although its stability depends on a number of unknown parameters. We discuss the possible habitability of submoons and the potential for subsubmoons. The existence, or lack thereof, of submoons, may yield important constraints on satellite formation and evolution in planetary systems. Key words: planets and satellites – exoplanets – tides 1 INTRODUCTION the planet spins quickly or to shrink if the planet spins slowly (e.g. -
Projekt Brána Do Vesmíru
Projekt Brána do vesmíru Hvězdárna Valašské Meziříčí, p. o. Krajská hvezdáreň v Žiline Súčasnosť a budúcnosť výskumu medziplanetárnej hmoty RNDr. Peter Vereš, PhD. University of Hawaii / Univerzita Komenského Ako sa objavila MPH ● Pôvodne iba nehybná hviezdna sféra ● Mesiac a Slnko ● Bludné planéty viditeľné voľným okom Starovek => novovek Piazzi ● 1.1.1801 ● Objekt pozorovaný 41 dní ● Stratený...predpoklad, medzi Marsom a Jupiterom ● Laplace – nemožné nájsť ● Gauss (24) vynašiel metódu, vypočítal, Ceres bol nájdený... Halley ● Kométy, odjakživa považované za poslov zlých správ, vysvetlené ako atmosferické javy ● ● ● ● Názov Kometes (dlhovlasá) ● 1577 Brahe = paralaxa, ďalej ako Mesiac ● Edmond Halley si všimol periodicitu kométy 1531, 1607, 1682 = návrat v 1758 Meteory ● Zaznamenané v -1809, - 687 (Lyridy) ● Ernst Chladni 1794 Kniha o pôvode Pallasovho železa ● 1798 Brandes, Benzenberg, paralaxa 400 meteorov, 22 spoločných ● 1803 dážď / Paríž, priznanie kozmického pôvodu ● 1833 USA dážď 20/s, LEO ● 1845/46 rozpad kométy Biela, dažde Andromedíd (72, 85, 93, 99) ● 1861 = Kirkwood, súvis rojov s kométami ● 1866 Schiaparelli: Swift-Tuttle (Perzeidy), Tempel (Leonidy) ● 1899 Adams vypočítal, že Jupiter narušil dráhu kométy, dážď nebol 1833, rytina, Leonidy 1998, foto, Leonidy, AGO Modra MPH a Slnečná sústava ● Slnko ● planéty (8) ● trpasličie planéty /Ceres, Pluto, Haumea, Makemake, Eris ● MPH = asteroidy, kométy, prach, plyn, .... Vznik a vývoj asteroidov ● -4571mil. rokov – vznik Sl. sús. ● Akrécia hmoty – nehomogenity, planetesimály, „viskózna -
ISTS-2017-D-074ⅠISSFD-2017-074
A look at the capture mechanisms of the “Temporarily Captured Asteroids” of the Earth By Hodei URRUTXUA1) and Claudio BOMBARDELLI2) 1)Astronautics Group, University of Southampton, United Kingdom 2)Space Dynamics Group, Technical University of Madrid, Spain (Received April 17th, 2017) Temporarily captured asteroids of the Earth are a newly discovered family of asteroids, which become naturally captured in the vicinity of the Earth for a limited time period. Thus, during the temporary capture these asteroids are in energetically favorable condi- tions, which makes them appealing targets for space missions to asteroids. Despite their potential interest, their capture mechanisms are not yet fully understood, and basic questions remain unanswered regarding the taxonomy of this population. The present work looks at gaining a better understanding of the key features that are relevant to the duration and nature of these asteroids, by analyzing patterns and extracting conclusions from a synthetic population of temporarily captured asteroids. Key Words: Asteroids, temporarily captured asteroids, capture dynamics, asteroid retrieval. Acronyms system. Asteroid 2006 RH120 is so far the only known mem- ber of this population, though statistical studies by Granvik et TCA : Temporarily captured asteroids al.12) support the evidence that such objects are actually com- TCO : Temporarily captured orbiters mon companions of the Earth, and thus it is expected that an TCF : Temporarily captured fly-bys increasing number of them will be found as survey technology improves.13) 1. Introduction During their temporary capture phase these asteroids are technically orbiting the Earth rather than the Sun, since their The origin of planetary satellites in the Solar System has Earth-binding energy is negative. -
Constraints on the Habitability of Extrasolar Moons 3 ¯Glob Its Orbit-Averaged Global Energy flux Fs
Formation, detection, and characterization of extrasolar habitable planets Proceedings IAU Symposium No. 293, 2012 c 2012 International Astronomical Union Nader Haghighipour DOI: 00.0000/X000000000000000X Constraints on the habitability of extrasolar moons Ren´eHeller1 and Rory Barnes2,3 1Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam email: [email protected] 2University of Washington, Dept. of Astronomy, Seattle, WA 98195, USA 3Virtual 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. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 33: AUGUST 9-15 Presented by The Earthrise Institute # 33 Authored by Alan Hale About Ice And Stone 2020 It is my pleasure to welcome all educators, students, topics include: main-belt asteroids, near-Earth asteroids, and anybody else who might be interested, to Ice and “Great Comets,” spacecraft visits (both past and Stone 2020. This is an educational package I have put future), meteorites, and “small bodies” in popular together to cover the so-called “small bodies” of the literature and music. solar system, which in general means asteroids and comets, although this also includes the small moons of Throughout 2020 there will be various comets that are the various planets as well as meteors, meteorites, and visible in our skies and various asteroids passing by Earth interplanetary dust. Although these objects may be -- some of which are already known, some of which “small” compared to the planets of our solar system, will be discovered “in the act” -- and there will also be they are nevertheless of high interest and importance various asteroids of the main asteroid belt that are visible for several reasons, including: as well as “occultations” of stars by various asteroids visible from certain locations on Earth’s surface. Ice a) they are believed to be the “leftovers” from the and Stone 2020 will make note of these occasions and formation of the solar system, so studying them provides appearances as they take place. The “Comet Resource valuable insights into our origins, including Earth and of Center” at the Earthrise web site contains information life on Earth, including ourselves; about the brighter comets that are visible in the sky at any given time and, for those who are interested, I will b) we have learned that this process isn’t over yet, and also occasionally share information about the goings-on that there are still objects out there that can impact in my life as I observe these comets. -
Detecting the Yarkovsky Effect Among Near-Earth Asteroids From
Detecting the Yarkovsky effect among near-Earth asteroids from astrometric data Alessio Del Vignaa,b, Laura Faggiolid, Andrea Milania, Federica Spotoc, Davide Farnocchiae, Benoit Carryf aDipartimento di Matematica, Universit`adi Pisa, Largo Bruno Pontecorvo 5, Pisa, Italy bSpace Dynamics Services s.r.l., via Mario Giuntini, Navacchio di Cascina, Pisa, Italy cIMCCE, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universits, UPMC Univ. Paris 06, Univ. Lille, 77 av. Denfert-Rochereau F-75014 Paris, France dESA SSA-NEO Coordination Centre, Largo Galileo Galilei, 1, 00044 Frascati (RM), Italy eJet Propulsion Laboratory/California Institute of Technology, 4800 Oak Grove Drive, Pasadena, 91109 CA, USA fUniversit´eCˆote d’Azur, Observatoire de la Cˆote d’Azur, CNRS, Laboratoire Lagrange, Boulevard de l’Observatoire, Nice, France Abstract We present an updated set of near-Earth asteroids with a Yarkovsky-related semi- major axis drift detected from the orbital fit to the astrometry. We find 87 reliable detections after filtering for the signal-to-noise ratio of the Yarkovsky drift esti- mate and making sure the estimate is compatible with the physical properties of the analyzed object. Furthermore, we find a list of 24 marginally significant detec- tions, for which future astrometry could result in a Yarkovsky detection. A further outcome of the filtering procedure is a list of detections that we consider spurious because unrealistic or not explicable with the Yarkovsky effect. Among the smallest asteroids of our sample, we determined four detections of solar radiation pressure, in addition to the Yarkovsky effect. As the data volume increases in the near fu- ture, our goal is to develop methods to generate very long lists of asteroids with reliably detected Yarkovsky effect, with limited amounts of case by case specific adjustments. -
Journal of Physics Special Topics an Undergraduate Physics Journal
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by University of Leicester Open Journals Journal of Physics Special Topics An undergraduate physics journal P5 1 Conditions for Lunar-stationary Satellites Clear, H; Evan, D; McGilvray, G; Turner, E Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH November 5, 2018 Abstract This paper will explore what size and mass of a Moon-like body would have to be to have a Hill Sphere that would allow for lunar-stationary satellites to exist in a stable orbit. The radius of this body would have to be at least 2500 km, and the mass would have to be at least 2:1 × 1023 kg. Introduction orbital period of 27 days. We can calculate the Geostationary satellites are commonplace orbital radius of the satellite using the following around the Earth. They are useful in provid- equation [3]: ing line of sight over the entire planet, excluding p 3 the polar regions [1]. Due to the Earth's gravi- T = 2π r =GMm; (1) tational influence, lunar-stationary satellites are In equation 1, r is the orbital radius, G is impossible, as the Moon's smaller size means it the gravitational constant, MM is the mass of has a small Hill Sphere [2]. This paper will ex- the Moon, and T is the orbital period. Solving plore how big the Moon would have to be to allow for r gives a radius of around 88000 km. When for lunar-stationary satellites to orbit it. -
Abstract Volume
T I I II I II I I I rl I Abstract Volume LPI LPI Contribution No. 1097 II I II III I • • WORKSHOP ON MERCURY: SPACE ENVIRONMENT, SURFACE, AND INTERIOR The Field Museum Chicago, Illinois October 4-5, 2001 Conveners Mark Robinbson, Northwestern University G. Jeffrey Taylor, University of Hawai'i Sponsored by Lunar and Planetary Institute The Field Museum National Aeronautics and Space Administration Lunar and Planetary Institute 3600 Bay Area Boulevard Houston TX 77058-1113 LPI Contribution No. 1097 Compiled in 2001 by LUNAR AND PLANETARY INSTITUTE The Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. Material in this volume may be copied without restraint for library, abstract service, education, or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as the appropriate acknowledgment of this publication .... This volume may be cited as Author A. B. (2001)Title of abstract. In Workshop on Mercury: Space Environment, Surface, and Interior, p. xx. LPI Contribution No. 1097, Lunar and Planetary Institute, Houston. This report is distributed by ORDER DEPARTMENT Lunar and Planetary institute 3600 Bay Area Boulevard Houston TX 77058-1113, USA Phone: 281-486-2172 Fax: 281-486-2186 E-mail: order@lpi:usra.edu Please contact the Order Department for ordering information, i,-J_,.,,,-_r ,_,,,,.r pA<.><--.,// ,: Mercury Workshop 2001 iii / jaO/ Preface This volume contains abstracts that have been accepted for presentation at the Workshop on Mercury: Space Environment, Surface, and Interior, October 4-5, 2001. -
Astrodynamics of Moving Asteroids
Astrodynamics of Moving Asteroids Damon Landau, Nathan Strange, Gregory Lantoine, Tim McElrath NASA-JPL/CalTech Copyright 2014 California Institute of Technology. Government sponsorship acknowledged. Capture a NEA into Earth orbit Redirect asteroid for a close approach of the Moon natural Most of the DV is to speed up/slow down the NEA to close approach encounter Earth near their MOID (typically a node) of NEA DB Moon Lunar gravity assist captures NEA during Earth flyby 2 2 Capture C3, km /s DV ≈ DB/DT 2 2 Single flyby captures objects from up to ~3 km /s C3 2008 HU4 example, return leg only Double flyby up to ~5 km2/s2, depends on declination Natural approach of 0.15 AU, 1.3 km2/s2 4/8/2014 2 Asteroids and DV and Mass (oh my!) Returnable mass from (10,776) currently known NEAs Returnable Mass, t Returnable Earth-Sun Lunar Earth flybys Number of NEAs Mass, t Lagrange Pts Flyby & “backflips” 2 2 C3 <1 km /s C3 <2.5 C3 <25 10–50 653 NEAs 2564 4067 50–150 62 207 827 150–300 10 16 190 300–500 6 10 75 500–1000 4 8 40 1000+ 0* 0* 10 Minimum DV (km/s) between NEA & Lunar Flyby Phase-free, circular Earth orbit*, 6 t Xe, 5 t SEP, 2000 s Isp Deimos is ~7 km/s, Phobos is ~8 km/s *circular Earth orbit → up to 300 m/s DV errors 2006 RH120 is the known exception for 1000+ t to Lagrange Pts and 2000 SG344 > 1000 t for Lunar flyby Close approaches no longer factor into the equation for high-DV NEAs 4/8/2014 3 Potential Return Opportunities, 2020s Abbreviated List • Atlas 551 Launch to Asteroid Max Return Earth Return Asteroid Return C 200 x 11k km alt., Diameter 3 Capability Escape Date Launch ~1.5 yr before 2007 UN12 4–11 m 2.2 km2/s2 500 t Jun ’17 Sep ’20 escape 2009 BD 5–13 1.7 900 Jun ‘17 Jun ’23 • 40 kW array 2009 BD 5–13 1.7 500 Jan ‘19 Jun ’23 • 3000 s Isp, 60 % eff. -
Week 5: January 26-February 1, 2020
5# Ice & Stone 2020 Week 5: January 26-February 1, 2020 Presented by The Earthrise Institute About Ice And Stone 2020 It is my pleasure to welcome all educators, students, topics include: main-belt asteroids, near-Earth asteroids, and anybody else who might be interested, to Ice and “Great Comets,” spacecraft visits (both past and Stone 2020. This is an educational package I have put future), meteorites, and “small bodies” in popular together to cover the so-called “small bodies” of the literature and music. solar system, which in general means asteroids and comets, although this also includes the small moons of Throughout 2020 there will be various comets that are the various planets as well as meteors, meteorites, and visible in our skies and various asteroids passing by Earth interplanetary dust. Although these objects may be -- some of which are already known, some of which “small” compared to the planets of our solar system, will be discovered “in the act” -- and there will also be they are nevertheless of high interest and importance various asteroids of the main asteroid belt that are visible for several reasons, including: as well as “occultations” of stars by various asteroids visible from certain locations on Earth’s surface. Ice a) they are believed to be the “leftovers” from the and Stone 2020 will make note of these occasions and formation of the solar system, so studying them provides appearances as they take place. The “Comet Resource valuable insights into our origins, including Earth and of Center” at the Earthrise web site contains information life on Earth, including ourselves; about the brighter comets that are visible in the sky at any given time and, for those who are interested, I will b) we have learned that this process isn’t over yet, and also occasionally share information about the goings-on that there are still objects out there that can impact in my life as I observe these comets.