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BENNU from OSIRIS-Rex APPROACH and PRELIMINARY SURVEY OBSERVATIONS
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1956.pdf VNIR AND TIR SPECTRAL CHARACTERISTICS OF (101955) BENNU FROM OSIRIS-REx APPROACH AND PRELIMINARY SURVEY OBSERVATIONS. V. E. Hamilton1, A. A. Simon2, P. R. Christensen3, D. C. Reuter2, D. N. Della Giustina4, J. P. Emery5, R. D. Hanna6, E. Howell4, H. H. Kaplan1, B. E. Clark7, B. Rizk4, D. S. Lauretta4, and the OSIRIS-REx Team, 1Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302 ([email protected]), 2NASA Goddard Space Flight Center, Greenbelt, MD, 3School of Earth & Space Ex- ploration, Arizona State University, Tempe, AZ 85287, 4Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, 5Dept. Earth & Planetary Science, University of Tennessee, Knoxville, TN 37996, 6University of Texas, Austin, TX, 78712, 7Dept. Physics & Astronomy, Ithaca College, Ithaca, NY 14850. Introduction: Visible to near infrared (VNIR) and generation and application of a photometric model, thermal infrared (TIR) spectrometers onboard the Ori- production of bolometric Bond albedo, reflectance gins, Spectral Interpretation, Resource Identification, factor spectra, and the calculation of spectral indices. Security–Regolith Explorer (OSIRIS-REx) spacecraft For OTES, this includes deriving emissivity spectra have revealed evidence of hydrated phases across the and temperature information with emissivity being an surface of asteroid (101955) Bennu. Here we describe input into a linear least squares mixing model and a spectral features identified -
AAS SFMC Manuscript Format Template
AAS 13-484 PASSIVE SORTING OF ASTEROID MATERIAL USING SOLAR RADIATION PRESSURE D. García Yárnoz,* J. P. Sánchez Cuartielles,† and C. R. McInnes ‡ Understanding dust dynamics in asteroid environments is key for future science missions to asteroids and, in the long-term, also for asteroid exploitation. This paper proposes a novel way of manipulating asteroid material by means of solar radiation pressure (SRP). We envisage a method for passively sorting material as a function of its grain size where SRP is used as a passive in-situ ‘mass spec- trometer’. The analysis shows that this novel method allows an effective sorting of regolith material. This has immediate applications for sample return, and in- situ resource utilisation to separate different regolith particle sizes INTRODUCTION Asteroids have lately become prime targets for space exploration missions. This interest is jus- tified as asteroids are among the least evolved bodies in the Solar System and they can provide a better understanding of its formation from the solar nebula. Under NASA’s flexible path plan,1 asteroids have also become one of the feasible “planetary” surfaces to be visited by crewed mis- sions, with the benefit of not requiring the capability to land and take-off from a deep gravity well. In addition, they may well be the most affordable source of in-situ resources to underpin future space exploration ventures. Considerable efforts have been made in the study of the perturbing forces and space environ- ment around cometary and asteroid bodies.2, 3 These forces and harsh environments need to be considered and will have direct implications for the operations of spacecraft around and on small bodies. -
Bennu: Implications for Aqueous Alteration History
RESEARCH ARTICLES Cite as: H. H. Kaplan et al., Science 10.1126/science.abc3557 (2020). Bright carbonate veins on asteroid (101955) Bennu: Implications for aqueous alteration history H. H. Kaplan1,2*, D. S. Lauretta3, A. A. Simon1, V. E. Hamilton2, D. N. DellaGiustina3, D. R. Golish3, D. C. Reuter1, C. A. Bennett3, K. N. Burke3, H. Campins4, H. C. Connolly Jr. 5,3, J. P. Dworkin1, J. P. Emery6, D. P. Glavin1, T. D. Glotch7, R. Hanna8, K. Ishimaru3, E. R. Jawin9, T. J. McCoy9, N. Porter3, S. A. Sandford10, S. Ferrone11, B. E. Clark11, J.-Y. Li12, X.-D. Zou12, M. G. Daly13, O. S. Barnouin14, J. A. Seabrook13, H. L. Enos3 1NASA Goddard Space Flight Center, Greenbelt, MD, USA. 2Southwest Research Institute, Boulder, CO, USA. 3Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA. 4Department of Physics, University of Central Florida, Orlando, FL, USA. 5Department of Geology, School of Earth and Environment, Rowan University, Glassboro, NJ, USA. 6Department of Astronomy and Planetary Sciences, Northern Arizona University, Flagstaff, AZ, USA. 7Department of Geosciences, Stony Brook University, Stony Brook, NY, USA. 8Jackson School of Geosciences, University of Texas, Austin, TX, USA. 9Smithsonian Institution National Museum of Natural History, Washington, DC, USA. 10NASA Ames Research Center, Mountain View, CA, USA. 11Department of Physics and Astronomy, Ithaca College, Ithaca, NY, USA. 12Planetary Science Institute, Tucson, AZ, Downloaded from USA. 13Centre for Research in Earth and Space Science, York University, Toronto, Ontario, Canada. 14John Hopkins University Applied Physics Laboratory, Laurel, MD, USA. *Corresponding author. E-mail: Email: [email protected] The composition of asteroids and their connection to meteorites provide insight into geologic processes that occurred in the early Solar System. -
(101955) Bennu from OSIRIS-Rex Imaging and Thermal Analysis
ARTICLES https://doi.org/10.1038/s41550-019-0731-1 Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis D. N. DellaGiustina 1,26*, J. P. Emery 2,26*, D. R. Golish1, B. Rozitis3, C. A. Bennett1, K. N. Burke 1, R.-L. Ballouz 1, K. J. Becker 1, P. R. Christensen4, C. Y. Drouet d’Aubigny1, V. E. Hamilton 5, D. C. Reuter6, B. Rizk 1, A. A. Simon6, E. Asphaug1, J. L. Bandfield 7, O. S. Barnouin 8, M. A. Barucci 9, E. B. Bierhaus10, R. P. Binzel11, W. F. Bottke5, N. E. Bowles12, H. Campins13, B. C. Clark7, B. E. Clark14, H. C. Connolly Jr. 15, M. G. Daly 16, J. de Leon 17, M. Delbo’18, J. D. P. Deshapriya9, C. M. Elder19, S. Fornasier9, C. W. Hergenrother1, E. S. Howell1, E. R. Jawin20, H. H. Kaplan5, T. R. Kareta 1, L. Le Corre 21, J.-Y. Li21, J. Licandro17, L. F. Lim6, P. Michel 18, J. Molaro21, M. C. Nolan 1, M. Pajola 22, M. Popescu 17, J. L. Rizos Garcia 17, A. Ryan18, S. R. Schwartz 1, N. Shultz1, M. A. Siegler21, P. H. Smith1, E. Tatsumi23, C. A. Thomas24, K. J. Walsh 5, C. W. V. Wolner1, X.-D. Zou21, D. S. Lauretta 1 and The OSIRIS-REx Team25 Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the for- mation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo. -
Twenty Years of Toutatis
EPSC Abstracts Vol. 6, EPSC-DPS2011-297, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Twenty Years of Toutatis M.W. Busch (1), L.A.M. Benner (2), D.J. Scheeres (3), J.-L. Margot (1), C. Magri (4), M.C. Nolan (5), and J.D. Giorgini (2) (1) Department of Earth and Space Sciences, UCLA, Los Angeles, California, USA (2) Jet Propulsion Laboratory, Pasadena, California, USA (3) Aerospace Engineering Sciences, University of Colorado, Boulder, Colorado, USA (4) University of Maine at Farmington, Farmington, Maine, USA (5) Arecibo Observatory, Arecibo, Puerto Rico, USA Abstract Near-Earth asteroid 4179 Toutatis is near a particularly if the moments of inertia are 4:1 orbital resonance with the Earth. consistent with a uniform internal density. Following its discovery in 1989, Toutatis Toutatis’ last close-Earth-approach for was observed extensively with the Arecibo several decades will be in December 2012, and Goldstone radars during flybys in 1992, when it will be 0.046 AU away. We will 1996, 2000, 2004, and 2008. The 1992 and make predictions for what radar 1996 data show that Toutatis is a bifurcated observations at that time should see. object with overall dimensions of 4.6 x 2.3 x 1.9 km and a surface marked with prominent impact craters. Most significantly, Toutatis References is in a non-principal-axis tumbling rotation [1] Hudson, R.S. and Ostro, S.J.: Shape and non-principal state, spinning about its long axis with a axis spin state of asteroid 4179 Toutatis, Science 270 84-86, period of 5.41 days while that axis precesses 1995. -
Thermophysical Modeling of 99942 Apophis: Estimations of Surface Temperature During the April 2029 Close Approach
Apophis T–9 Years 2020 (LPI Contrib. No. 2242) 2069.pdf THERMOPHYSICAL MODELING OF 99942 APOPHIS: ESTIMATIONS OF SURFACE TEMPERATURE DURING THE APRIL 2029 CLOSE APPROACH. K. C. Sorli1 and P. O. Hayne1, 1Laboratory for Atmospheric and Space Physics – University of Colorado Boulder, CO 80303 ([email protected]) Introduction: The April 13, 2029 close approach purposes of calculating temperatures and thermal IR of the ~350-meter asteroid 99942 Apophis offers an fluxes. Our predictions for surface temperatures and unprecedented opportunity to observe a large near-Earth dynamical effects will be directly testable during the asteroid in detail with ground-based observatories. As Janus mission, with an anticipated launch date of 2022. one of the best-studied hazardous objects, with Though the model was constructed with the intent of additional near-miss flybys in coming decades, it is categorizing binary thermal and dynamical behaviors, crucial to planetary defense to understand its properties including binary YORP [5][6], it is easily adaptable to and potential perturbations to its orbit. solitary asteroids. Apophis has been the subject of extensive study, and This model begins by coupling a 1-d thermophysical will continue to be so for years to come. This existing model [7] to a 3-d shape model and computing facet-by- knowledge and the promise of new data makes it an facet temperatures of the surface and near subsurface excellent candidate for modeling subject to during the time period of Apophis’s 2029 close observational constraints. The 2029 close approach will approach. To calculate temperatures, the model is given have a sizable amplifying effect on Apophis’ orbital information about the incoming solar flux on each facet uncertainty, so small dynamical perturbations will be as a function of solar distance and is set to equilibrate required to understand both the conditions of the 2029 for 1 year to allow for subsurface temperature settling. -
Planetary Defence Activities Beyond NASA and ESA
Planetary Defence Activities Beyond NASA and ESA Brent W. Barbee 1. Introduction The collision of a significant asteroid or comet with Earth represents a singular natural disaster for a myriad of reasons, including: its extraterrestrial origin; the fact that it is perhaps the only natural disaster that is preventable in many cases, given sufficient preparation and warning; its scope, which ranges from damaging a city to an extinction-level event; and the duality of asteroids and comets themselves---they are grave potential threats, but are also tantalising scientific clues to our ancient past and resources with which we may one day build a prosperous spacefaring future. Accordingly, the problems of developing the means to interact with asteroids and comets for purposes of defence, scientific study, exploration, and resource utilisation have grown in importance over the past several decades. Since the 1980s, more and more asteroids and comets (especially the former) have been discovered, radically changing our picture of the solar system. At the beginning of the year 1980, approximately 9,000 asteroids were known to exist. By the beginning of 2001, that number had risen to approximately 125,000 thanks to the Earth-based telescopic survey efforts of the era, particularly the emergence of modern automated telescopic search systems, pioneered by the Massachusetts Institute of Technology’s (MIT’s) LINEAR system in the mid-to-late 1990s.1 Today, in late 2019, about 840,000 asteroids have been discovered,2 with more and more being found every week, month, and year. Of those, approximately 21,400 are categorised as near-Earth asteroids (NEAs), 2,000 of which are categorised as Potentially Hazardous Asteroids (PHAs)3 and 2,749 of which are categorised as potentially accessible.4 The hazards posed to us by asteroids affect people everywhere around the world. -
An Estimate of the Flux of Apophis-Particle Meteors at Earth
Apophis T–9 Years 2020 (LPI Contrib. No. 2242) 2075.pdf An Estimate of the Flux of Apophis-Particle Meteors at Earth 1 1 2 Robert Melikyan , Beth Ellen Clark , Carl Hergenrother 1 D epartment of Physics and Astronomy, Ithaca College, Ithaca, NY, USA. 2 L unar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA. Near-Earth asteroid (99942) Apophis is meteoroid stream is propagated between 1900 - predicted to make a close encounter with Earth 2029 using an Apophis ephemeris that places the on April 13, 2029. This close encounter will asteroid at its most likely position for the 2029 bring Apophis within 6 Earth radii from our encounter. Unlike most meteoroid stream geocenter providing an excellent opportunity to evolution studies, our simulations release study and observe the asteroid and any particles from Apophis at a regular (~weekly) subsequent effects of the interaction. Here, we rate around its entire orbit, consistent with the bring to your attention the possibility that the Bennu observations. passage of Apophis will not be the only event worth observing. We predict a rain of Apophis Assuming similar particle production meteors that may be detectable to Earth’s meteor mechanisms at Apophis as observed at Bennu, monitoring systems. Apophis could be producing on order of 104 grams of material continuously throughout its NASA’s OSIRIS-REx mission has orbit. Of that material, we assume 30% will recently shown that near-Earth asteroid (101955) escape on hyperbolic trajectories [6]. This Bennu has been continuously producing results in roughly 3500 grams of new material 4 cm-sized ejecta at rates of ~10 grams per orbit entering the Apophis meteoroid stream annually. -
Introduction 101955 Bennu Speed Variations Variations of Bennu's
Deflect an hazardous asteroid through kinetic impact 51st Annual Meeting of the Division on Dynamical Astronomy Bruno Chagas1, Antonio F.B. de A. Prado1;2, Othon Winter1 S~aoPaulo State University (UNESP), School of Engineering, Guaratinguet´a-SP, Brazil1 National Institute for Space Research, INPE, S~aoJos´edos Campos-SP, Brazil2 Introduction Asteroids are the smallest bodies in the solar system, usually with diameters on the order of a few hundred's, or even only tens of kilometers. The total mass of all asteroids in the solar system must be less than the mass of the Earth's Moon. Despite this fact, they are objects of great importance. They must contain information about the formation of the solar system, since its chemical and physical compositions remain practically constant over time. These bodies also pose a danger to Earth, as many of these bodies are on a trajectory that passes close to Earth. There is also the possibility of mining on asteroids, in order to extract precious metals and other natural resources. Within this context, the present work intends to focus on the application aimed at the deflect an hazardous asteroid through kinetic impact. The asteroid's orbit behavior will be analyzed to determined the accuracy of the technique. To do this, we will be measure the deviation and displacement obtained at the point of maximum approximation between the body and the Earth. 101955 Bennu Variations of Bennu's orbit The asteroid 101955 Bennu is part of the group of NEOs that can become objects with a The Mercury integrator package was used and the integrator used was Bulirsch-Stoer. -
Small Satellite Rendezvous and Characterization of Asteroid 99942 Apophis
SSC09-IV-3 Small Satellite Rendezvous and Characterization of Asteroid 99942 Apophis James Chartres Carnegie Mellon Innovations Laboratory, Carnegie Mellon University Silicon Valley Small Spacecraft Office, NASA Ames Research Center Building 202, Moffett Field, CA 94035; (650) 604-6347 [email protected] David Dunham, Bobby Williams Space Navigation and Flight Dynamics, KinetX, Inc. 2050 E. ASU Circle, Suite 107, Tempe, AZ 85284; (480) 829-6600 [email protected], [email protected] Anthony Genova, Anthony Colaprete, Ronald Johnson, Belgacem Jaroux Small Spacecraft Office, NASA Ames Research Center Building 202, Moffett Field, CA 94035; (650) 604-6347, (650) 604-2918, (650) 604-6699, (650) 604-6312 [email protected], [email protected], [email protected], [email protected] ABSTRACT The Measurement and Analysis of Apophis Trajectory (MAAT) concept study investigated a low-cost characterization mission to the asteroid 99942 Apophis that leverage small spacecraft architectures and technologies. The mission goals were to perform physical characterization and improve the orbital model. The MAAT mission uses a small spacecraft free flyer and a bi-propellant transfer stage that can be incorporated as a secondary payload on Evolved Expendable Launch Vehicles (EELVs), Atlas V or Delta IV launches. Using the innovative secondary architecture allows the system to be launched on numerous GTO or LTO opportunities such as NASA science missions or commercial communication satellites. The trajectory takes advantage of the reduced Delta-V requirement during the 2012- 2015 time frame, with a large flexible launch opportunity, from January to November 2012 and heliocentric injection occurs in April 2013. -
Orbital Stability Assessments of Satellites Orbiting Small Solar System Bodies a Case Study of Eros
Delft University of Technology, Faculty of Aerospace Engineering Thesis report Orbital stability assessments of satellites orbiting Small Solar System Bodies A case study of Eros Author: Supervisor: Sjoerd Ruevekamp Jeroen Melman, MSc 1012150 August 17, 2009 Preface i Contents 1 Introduction 2 2 Small Solar System Bodies 4 2.1 Asteroids . .5 2.1.1 The Tholen classification . .5 2.1.2 Asteroid families and belts . .7 2.2 Comets . 11 3 Celestial Mechanics 12 3.1 Principles of astrodynamics . 12 3.2 Many-body problem . 13 3.3 Three-body problem . 13 3.3.1 Circular restricted three-body problem . 14 3.3.2 The equations of Hill . 16 3.4 Two-body problem . 17 3.4.1 Conic sections . 18 3.4.2 Elliptical orbits . 19 4 Asteroid shapes and gravity fields 21 4.1 Polyhedron Modelling . 21 4.1.1 Implementation . 23 4.2 Spherical Harmonics . 24 4.2.1 Implementation . 26 4.2.2 Implementation of the associated Legendre polynomials . 27 4.3 Triaxial Ellipsoids . 28 4.3.1 Implementation of method . 29 4.3.2 Validation . 30 5 Perturbing forces near asteroids 34 5.1 Third-body perturbations . 34 5.1.1 Implementation of the third-body perturbations . 36 5.2 Solar Radiation Pressure . 36 5.2.1 The effect of solar radiation pressure . 38 5.2.2 Implementation of the Solar Radiation Pressure . 40 6 About the stability disturbing effects near asteroids 42 ii CONTENTS 7 Integrators 44 7.1 Runge-Kutta Methods . 44 7.1.1 Runge-Kutta fourth-order integrator . 45 7.1.2 Runge-Kutta-Fehlberg Method . -
User Provided Data Product Upload of Herschel/PACS Near-Earth Asteroid Observations (Release Note)
Small Bodies: Near and Far NEA HSA UPDP upload User Provided Data Product upload of Herschel/PACS near-Earth asteroid observations (release note) Small Bodies: Near and Far; 687378 – SBNAF – RIA Cs. Kiss1, T.G. M¨uller2, and the SBNAF team 1Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly Thege 15-17, H-1121 Budapest, Hungary 2Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany Version 1.0 (as of December 29, 2016) Contents 1 Introduction 2 2 Herschel Space Observatory 2 3 Near-Earth asteroid observations 2 4 Data reduction and calibration 3 5Results 3 5.1 (101955) Bennu . 5 5.2 175706 (1996 FG 3) . 5 5.3 308635 (2005 YU 55) . 5 5.4 (162173) Ryugu . 6 5.5 (99942) Apophis . 6 References 7 Appendix 8 Summary of uploaded data products . 8 Summary of additional FITS keywords . 11 Page 1 Small Bodies: Near and Far NEA HSA UPDP upload 1 Introduction SMALL BODIES: NEAR AND FAR is a Horizon 2020 project (project number: 687378) that addresses critical points in reconstructing physical and thermal properties of near- Earth, main-belt, and trans-Neptunian objects (see the project webpage for details: http://www.mpe.mpg.de/ tmueller/sbnaf/). One of the goals of the SBNAF project is to produce a set of high-quality data products for Herschel observations of Solar System objects for an upload to the Herschel Science Archive (HSA). These new products will then be available for the entire scientific community, in parallel to the standard pipeline-processed Herschel archive data.