DOCSLIB.ORG

How GAIA Asteroids Can Improve Planetary Ephemerides ?

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
How GAIA Asteroids Can Improve Planetary Ephemerides ? GREAT-SSO: Solar System science before and after Gaia tugraz How GAIA asteroids can improve planetary ephemerides ? A. Fienga1;2 1Institut UTINAM, Universit´ede Franche-Comt´e,France 2IMCCE, Observatoire de Paris, France A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 1 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz Outline Overview of the planetary ephemerides INPOP and the asteroids Use of GAIA asteroid observations to improve Jupiter orbit A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 2 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz JPL DE/IAA EMP/INPOP Direct numerical integration of equations of motion 9 planets + Moon + asteroids, GR, J2 Sun, TDB/TCB Fitted to observations Fit of asteroid masses and densities INPOP: www.imcce.fr/inpop Numerical integration with extended precision 80b Earth and Moon Rotations INPOP(TCB) for GAIA and INPOP(TDB) from IAU 2006 INPOP10a (Fienga et al. 2011), INPOP06 (Fienga et al. 2008), INPOP08 (Fienga et al. 2009), Tests of fundamental physics / Use for paleoclimats A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 3 / 19 INPOP10a 40 35 GREAT-SSO: Solar30 System science before and after Gaia Passive range VEX Viking 25 MGS % MEX n i t Stellar occultations i f 20 e Optical h t Flybys n i t 15 VLBI c a JPL DE, EPM,p INPOP m I 10 Same modellingOverview expect for of the planetary ephemerides the asteroids 5 rely mainly on (Mars) 0 e ry s s r e s n u u r e n u u c n a it r n t o spacecraft data r e p tu a p t e V M u a r e lu M J S U N P Lack of Jupiter good observations Cassini: good constraints on Saturn 1 Poor accuracy of the Jupiter orbit A. Fienga2 May 4th, 2011 How GAIA can improve planetary ephemerides ? Crucial role of the asteroids tugraz 4 / 19 INPOP10a 40 35 GREAT-SSO: Solar30 System science before and after Gaia Passive range VEX Viking 25 MGS % MEX n i t Stellar occultations i f 20 e Optical h t Flybys n i t 15 VLBI c a JPL DE, EPM,p INPOP m I 10 Same modellingOverview expect for of the planetary ephemerides the asteroids 5 rely mainly on (Mars) 0 e ry s s r e s n u u r e n u u c n a it r n t o spacecraft data r e p tu a p t e V M u a r e lu M J S U N P Lack of Jupiter good observations Cassini: good constraints on Saturn 1 Poor accuracy of the Jupiter orbit A. Fienga2 May 4th, 2011 How GAIA can improve planetary ephemerides ? Crucial role of the asteroids tugraz 4 / 19 GREAT-SSO: Solar System science before and after Gaia A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? Internal accuracies of planetary ephemerides INPOP10A−DE421 INPOP10A−INPOP08 INPOP10A−INPOP06 0 0 0 ] ] ] 1 0 s s s 3 a a a m m m [ [ [ e e 5 0 d d − u u 0 t t i i 0 g g 1 n n 0 o o 1 0 L L − 1 − 0 0 1 0 2 − − 1900 1940 1980 2020 1900 1940 1980 2020 1900 1940 1980 2020 date date date 0 0 0 0 3 1 2 ] ] ] 0 s s s 0 5 a 0 a a 1 1 m m m [ [ [ e e 0 d d 0 u u t t 0 i i t t 1 a a − L L 5 − 0 0 3 0 0 − 1 2 − − 1900 1940 1980 2020 1900 1940 1980 2020 1900 1940 1980 2020 date date date 0 0 3 0 2 1 ] ] 5 0 1 m m 0 k k 1 [ [ 0 e e 0 c c 0 n n 5 a a t t − s s 1 i i − d d 0 2 0 2 − 5 1 − − 5 / 19 Geocentric distance [km] distance Geocentric 1900 1940 1980 2020 1900 1940 1980 2020 1900 1940 1980 2020 date date date tugraz GREAT-SSO: Solar System science before and after Gaia tugraz Planets Umin Umax α δ ρ α δ ρ mas mas km mas mas km Mercury 5 6 1.5 9 4 1.5 Venus83 0.4 8 6 1.0 Mars* 40 15 10 75 30 15 Jupiter 20 30 15 400 200 300 Saturne 0.8 0.43 40 60 100 Uranus 300 120 1200 220 100 1500 Neptune 400 100 3500 160 150 5000 Pluto 3000 1000 80000 6000 2000 140000 long lat ρ long lat ρ Earth3 1.5 0.04 6 3 0.10 A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 6 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz INPOP and the asteroids Asteroids are highly important in planetary ephemerides for: Mars with more than 30 years of very accurate (< 5 meters) spacecraft tracking global fit for all the planets: more than 35 % are Mars data INPOP10a (Fienga et al. 2011) 24635 asteroid orbits (astorb database) integrated in INPOP planets $ asteroids, asteroids $ asteroids, EIH Kuchynka et al. 2010: List of the most probable perturbers of inner planets (287) + ring Mass estimations with BVLS algorithm Study of correlations A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 7 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz INPOP and the asteroids Asteroids are highly important in planetary ephemerides for: Mars with more than 30 years of very accurate (< 5 meters) spacecraft tracking global fit for all the planets: more than 35 % are Mars data INPOP10a (Fienga et al. 2011) 24635 asteroid orbits (astorb database) integrated in INPOP planets $ asteroids, asteroids $ asteroids, EIH Kuchynka et al. 2010: List of the most probable perturbers of inner planets (287) + ring Mass estimations with BVLS algorithm Study of correlations A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 7 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz INPOP10a (Fienga et al. 2011) List of the most probable perturbers + ring (Kuchynka et al. 2010) Mass estimations with BVLS algorithm Study of correlations ! Fixed masses (15) A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 8 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz INPOP and the asteroids Uncertainties of ≈ 10% on the 3 Big mass determinations A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 9 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz INPOP and the asteroids 324 Bamberga ● ● INPOP10a 94 m Other 3 Juno ● 56 m K11 ● 704 Interamnia INPOP08 34 m 532 Herculina ● 33 m 7 Iris ● 28 m 29 Amphitrite ● 27 m 24 Themis ● 26 m 15 Eunomia ● 22 m 6 Hebe ● 21 m 11 Parthenope ● 17 m 139 Juewa ● 17 m 747 Winchester ● 16 m 8 Flora ● 13 m 41 Daphne ● 12 m 511 Davida ● 10 m 52 Europa ● 10 m 16 Psyche ● 10 m 130 Elektra ● 7 m 107 Camilla ● 5 m 65 Cybele ● 5 m 21 Lutetia ● 5 m 216 Kleopatra ● 3 m 804 Hispania ● 2 m 0 2 4 6 8 10 12 14 Density [g.cm^−3] A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 10 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz How GAIA can help ? GAIA asteroid mass determinations great improvement in the masses for the biggest improvement for the mass determinations with INPOP Satellites small Jovian satellites Neptune and Uranus satellites Satellites are not yet implemented in INPOP Asteroid orbits 24635 asteroids already implemented in INPOP Big picture: mass + orbit + planets A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 11 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz How GAIA can help ? GAIA asteroid mass determinations great improvement in the masses for the biggest improvement for the mass determinations with INPOP Satellites small Jovian satellites Neptune and Uranus satellites Satellites are not yet implemented in INPOP Asteroid orbits 24635 asteroids already implemented in INPOP Big picture: mass + orbit + planets A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 11 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz How GAIA can help ? GAIA asteroid mass determinations great improvement in the masses for the biggest improvement for the mass determinations with INPOP Satellites small Jovian satellites Neptune and Uranus satellites Satellites are not yet implemented in INPOP Asteroid orbits 24635 asteroids already implemented in INPOP Big picture: mass + orbit + planets A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 11 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz Do GAIA asteroid observations can give better informations on Jupiter orbit compared to the present accuracy of Jupiter observations ? Present observation accuracy over 6 years VLBI Galileo observations + Flybys normal points ≈ 10 mas in geocentric (α,δ) and 2 km in geocentric distances ≈ 8 mas in barycentric longitudes and latitudes impact on the Jupiter orbit over 6 years 10−9 AU for a 10−8 for the angles 10−7 for e A. Fienga May 4th, 2011 How GAIA can improve planetary ephemerides ? 12 / 19 GREAT-SSO: Solar System science before and after Gaia tugraz questions: What are the impacts of such uncertainties on asteroid orbits ? Are they observable at the level of accuracy of the GAIA observations ? method Integrate asteroid orbit with different Jupiter orbits Fit of the asteroid orbit to a reference orbit Measurement of the differences in barycentric longitudes and latitudes of the asteroid 3 cases 1 of the 3 Bigs: 4 Vesta an asteroid with a close approach with Jupiter: 86 Semele a Troyen: 588 Achilles A.
Load more

Recommended publications
  • ESO's VLT Sphere and DAMIT
    ESO’s VLT Sphere and DAMIT ESO’s VLT SPHERE (using adaptive optics) and Joseph Durech (DAMIT) have a program to observe asteroids and collect light curve data to develop rotating 3D models with respect to time. Up till now, due to the limitations of modelling software, only convex profiles were produced. The aim is to reconstruct reliable nonconvex models of about 40 asteroids. Below is a list of targets that will be observed by SPHERE, for which detailed nonconvex shapes will be constructed. Special request by Joseph Durech: “If some of these asteroids have in next let's say two years some favourable occultations, it would be nice to combine the occultation chords with AO and light curves to improve the models.” 2 Pallas, 7 Iris, 8 Flora, 10 Hygiea, 11 Parthenope, 13 Egeria, 15 Eunomia, 16 Psyche, 18 Melpomene, 19 Fortuna, 20 Massalia, 22 Kalliope, 24 Themis, 29 Amphitrite, 31 Euphrosyne, 40 Harmonia, 41 Daphne, 51 Nemausa, 52 Europa, 59 Elpis, 65 Cybele, 87 Sylvia, 88 Thisbe, 89 Julia, 96 Aegle, 105 Artemis, 128 Nemesis, 145 Adeona, 187 Lamberta, 211 Isolda, 324 Bamberga, 354 Eleonora, 451 Patientia, 476 Hedwig, 511 Davida, 532 Herculina, 596 Scheila, 704 Interamnia Occultation Event: Asteroid 10 Hygiea – Sun 26th Feb 16h37m UT The magnitude 11 asteroid 10 Hygiea is expected to occult the magnitude 12.5 star 2UCAC 21608371 on Sunday 26th Feb 16h37m UT (= Mon 3:37am). Magnitude drop of 0.24 will require video. DAMIT asteroid model of 10 Hygiea - Astronomy Institute of the Charles University: Josef Ďurech, Vojtěch Sidorin Hygiea is the fourth-largest asteroid (largest is Ceres ~ 945kms) in the Solar System by volume and mass, and it is located in the asteroid belt about 400 million kms away.
    [Show full text]
  • Observations from Orbiting Platforms 219
    Dotto et al.: Observations from Orbiting Platforms 219 Observations from Orbiting Platforms E. Dotto Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino M. A. Barucci Observatoire de Paris T. G. Müller Max-Planck-Institut für Extraterrestrische Physik and ISO Data Centre A. D. Storrs Towson University P. Tanga Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino and Observatoire de Nice Orbiting platforms provide the opportunity to observe asteroids without limitation by Earth’s atmosphere. Several Earth-orbiting observatories have been successfully operated in the last decade, obtaining unique results on asteroid physical properties. These include the high-resolu- tion mapping of the surface of 4 Vesta and the first spectra of asteroids in the far-infrared wave- length range. In the near future other space platforms and orbiting observatories are planned. Some of them are particularly promising for asteroid science and should considerably improve our knowledge of the dynamical and physical properties of asteroids. 1. INTRODUCTION 1800 asteroids. The results have been widely presented and discussed in the IRAS Minor Planet Survey (Tedesco et al., In the last few decades the use of space platforms has 1992) and the Supplemental IRAS Minor Planet Survey opened up new frontiers in the study of physical properties (Tedesco et al., 2002). This survey has been very important of asteroids by overcoming the limits imposed by Earth’s in the new assessment of the asteroid population: The aster- atmosphere and taking advantage of the use of new tech- oid taxonomy by Barucci et al. (1987), its recent extension nologies. (Fulchignoni et al., 2000), and an extended study of the size Earth-orbiting satellites have the advantage of observing distribution of main-belt asteroids (Cellino et al., 1991) are out of the terrestrial atmosphere; this allows them to be in just a few examples of the impact factor of this survey.
    [Show full text]
  • Orbital Stability Zones About Asteroids
    ICARUS 92, 118-131 (1991) Orbital Stability Zones about Asteroids DOUGLAS P. HAMILTON AND JOSEPH A. BURNS Cornell University, Ithaca, New York, 14853-6801 Received October 5, 1990; revised March 1, 1991 exploration program should be remedied when the Galileo We have numerically investigated a three-body problem con- spacecraft, launched in October 1989, encounters the as- sisting of the Sun, an asteroid, and an infinitesimal particle initially teroid 951 Gaspra on October 29, 1991. It is expected placed about the asteroid. We assume that the asteroid has the that the asteroid's surroundings will be almost devoid of following properties: a circular heliocentric orbit at R -- 2.55 AU, material and therefore benign since, in the analogous case an asteroid/Sun mass ratio of/~ -- 5 x 10-12, and a spherical of the satellites of the giant planets, significant debris has shape with radius R A -- 100 km; these values are close to those of never been detected. The analogy is imperfect, however, the minor planet 29 Amphitrite. In order to describe the zone in and so the possibility that interplanetary debris may be which circum-asteroidal debris could be stably trapped, we pay particular attention to the orbits of particles that are on the verge enhanced in the gravitational well of the asteroid must be of escape. We consider particles to be stable or trapped if they considered. If this is the case, the danger of collision with remain in the asteroid's vicinity for at least 5 asteroid orbits about orbiting debris may increase as the asteroid is approached.
    [Show full text]
  • Iso and Asteroids
    r bulletin 108 Figure 1. Asteroid Ida and its moon Dactyl in enhanced colour. This colour picture is made from images taken by the Galileo spacecraft just before its closest approach to asteroid 243 Ida on 28 August 1993. The moon Dactyl is visible to the right of the asteroid. The colour is ‘enhanced’ in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a ‘natural’ colour picture of this asteroid would appear mostly grey. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body, as well as subtle colour variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the centre of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near-infrared light, suggesting a difference Figure 2. This image mosaic of asteroid 253 Mathilde is in the abundance or constructed from four images acquired by the NEAR spacecraft composition of iron-bearing on 27 June 1997. The part of the asteroid shown is about 59 km minerals in these areas. Ida’s by 47 km. Details as small as 380 m can be discerned. The moon also has a deeper near- surface exhibits many large craters, including the deeply infrared absorption and a shadowed one at the centre, which is estimated to be more than different colour in the violet than any 10 km deep.
    [Show full text]
  • Snake River Skies the Newsletter of the Magic Valley Astronomical Society
    Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting MVAS President’s Message June 2018 Saturday, June 9th 2018 7:00pm at the Toward the end of last month I gave two presentations to two very different groups. Herrett Center for Arts & Science College of Southern Idaho. One was at the Sawtooth Botanical Gardens in their central meeting room and covered the spring constellations plus some simple setups for astrophotography. Public Star Party Follows at the The other was for the Sun Valley Company and was a telescope viewing session Centennial Observatory given on the lawn near the outdoor pavilion. The composition of the two groups couldn’t be more different and yet their queries and interests were almost identical. Club Officers Both audiences were genuinely curious about the universe and their questions covered a wide range of topics. How old is the moon? What is a star made of? Tim Frazier, President How many exoplanets are there? And, of course, the big one: Is there life out [email protected] there? Robert Mayer, Vice President The SBG’s observing session was rained out but the skies did clear for the Sun [email protected] Valley presentation. As the SV guests viewed the moon and Jupiter, I answered their questions and pointed out how one of Jupiter’s moons was disappearing Gary Leavitt, Secretary behind the planet and how the mountains on our moon were casting shadows into [email protected] the craters. Regardless of their age, everyone was surprised at the details they 208-731-7476 could see and many expressed their amazement at what was “out there”.
    [Show full text]
  • (2000) Forging Asteroid-Meteorite Relationships Through Reflectance
    Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta.
    [Show full text]
  • Solar System Objects in the ISOPHOT 170 Μm Serendipity Survey
    A&A 389, 665–679 (2002) Astronomy DOI: 10.1051/0004-6361:20020596 & c ESO 2002 Astrophysics Solar system objects in the ISOPHOT 170 µm serendipity survey? T. G. M¨uller1,2, S. Hotzel3, and M. Stickel3 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany 2 ISO Data Centre, Astrophysics Division, Space Science Department of ESA, Villafranca, PO Box 50727, 28080 Madrid, Spain (until Dec. 2001) 3 ISOPHOT Data Centre, Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany Received 14 January 2002 / Accepted 12 March 2002 Abstract. The ISOPHOT Serendipity Survey (ISOSS) covered approximately 15% of the sky at a wavelength of 170 µm while the ISO satellite was slewing from one target to the next. By chance, ISOSS slews went over many solar system objects (SSOs). We identified the comets, asteroids and planets in the slews through a fast and effective search procedure based on N-body ephemeris and flux estimates. The detections were analysed from a calibration and scientific point of view. Through the measurements of the well-known asteroids Ceres, Pallas, Juno and Vesta and the planets Uranus and Neptune it was possible to improve the photometric calibration of ISOSS and to extend it to higher flux regimes. We were also able to establish calibration schemes for the important slew end data. For the other asteroids we derived radiometric diameters and albedos through a recent thermophysical model. The scientific results are discussed in the context of our current knowledge of size, shape and albedos, derived from IRAS observations, occultation measurements and lightcurve inversion techniques.
    [Show full text]
  • Debris About Asteroids: Where and How Much?
    Asteroids, Comets, Meteors 1991, pp. 101-108 Lunar and Planetarylnstitute, Houston, 1992 _ // /-7/0 _7"_ 10l DEBRIS ABOUT ASTEROIDS: WHERE AND HOW MUCH? - Joseph A. Burns and Douglas P. Hamilton Cornell University, Ithaca NY 14853 USA i We summarize several recent findings on the size and shape of the region within which material can ! i ! stably orbit an asteroid. If the asteroid (with assumed density 2.38 g/cm 3) circles the Sun at 2.55 AU, | co-planar prograde material will remain trapped whenever started on unperturbed circular orbits at ! less than about 220 R A (asteroid radii); co-planar retrograde particles are stable out twice as far. Our 3-D stability surface, which encloses several hundred numerically calculated orbits that start with various inclinations, is shaped like a sphere with its top and bottom sliced off; its dimensions scale like the Hill radius =(p./3)1/3R, where p. is the asteroid-to-solar mass ratio and R is the asteroid's orbital radius. If the asteroid moves along an elliptical orbit, a fairly reliable indicator of the dimensions of the hazard zone is the size of its Hill sphere at the orbit's pericenter. Grains with radii less than a few mm will be lost through the action of radiation forces which can induce escape or cause collisions with the asteroid on time scales of a few years; interplanetary micrometeoroids produce collisional break-up of these particles in ~104 yrs. The effects of Jupiter and of asteroids that pass close to the target asteroid allow particles to diffuse from the system, again shrinking the hazard zone.
    [Show full text]
  • General Disclaimer One Or More of the Following Statements May Affect
    https://ntrs.nasa.gov/search.jsp?R=19850022682 2020-03-20T17:45:21+00:00Z General Disclaimer CORE Metadata, citation and similar papers at core.ac.uk Provided by NASA Technical ReportsOne Server or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) i' Ig1F "7 s ^ s, 1 Final Report for(3 2243 1 1 Speckle Interferometry Applied to 1 !!steroids and Other Solar System Objects 1 z August 1981 - July 1984 .Tack D. Drummond and E. Keith Hege I Steward Observatory, University of Arizona Tucson, Arizona 85721 r May 31, 1985 ^c Jut I*' ^ ^ZZ F yE0 t jNAiA-CR-175976) St'ECKL,& IN7Lurc:itu&&THY N85- 30995 APPLIED TO ASTYBOILS 15L CTEffi SOLAR SYSTEM UBJECJS Final REfiott ;,irizCCa tL iv., 1 UnCIdE Z ucson.) 109 a 8L ACC/tf A0 i C:SCL 038 G3/91 216-3-8 Final Report for NAGW 224 Speckle Interferometry Applied to 0 Asteroids and Other Solar System Objects August 1981 - July 1984 Jack D.
    [Show full text]
  • (29075) 1950 Da
    Journal of Physics & Astronomy Short Communication| Vol 6 Iss 3 The Potentially Dangerous Asteroid (29075) 1950 DA Wlodarczyk Ireneusz* Chorzow Astronomical Observatory, 41-500 Chorzow, Poland *Corresponding author: Wlodarczyk, Ireneusz, 41-500 Chorzow, Poland, Tel.: +48627221279; E-Mail: [email protected] Received: July 10 2018; Accepted: August 01 2018; Published: August 08 2018 Abstract I present behavior of the dynamically interesting potentially dangerous asteroid (29075) 1950 DA. Using the public available OrbFit software I studied orbit of asteroid 900 years forward in the future searching for close approaches with the Earth, which lead to possible impact in 2880. Keywords: Asteroids; Dynamic; Celestial mechanic; Near-Earth Objects; Orbit determination Introduction The asteroid (29075) 1950 DA was discovered on February 22, 1950 by the (IAU 662) Lick-Observatory, Mount Hamilton (IAUC 1258). It was observed for 19 days in 1950 till March, 12 and then lost because of the short observational arc [1]. On December 31, 2000, it was observed by J.E. Rogers from (IAU 670) Camarillo Observatory, recovered as 2000 YK66 and 2 hours later was recognized as 1950 DA( MPEC 2001-A-26). Between these dates the asteroid (29075) 1950 DA was observed on September 30, 1981 by Siding Spring Observatory-DSS ( IAU 260). Asteroid (29075) 1950 DA belongs to the Apollo group, comprising 9194 members as of July 5, 2018), and is one of 18345 known Near-Earth Asteroids at this time http://www.minorplanetcenter.net/iau/lists/Unusual.html. According to the JPL NASA: https://ssd.jpl.nasa.gov/sbdb.cgi#top, its absolute magnitude is 17.1, suggesting a diameter of about 2.0 km (see also next Section).
    [Show full text]
  • Triaxial Ellipsoid Dimensions and Poles of Asteroids
    Icarus 202 (2009) 147–159 Contents lists available at ScienceDirect Icarus www.elsevier.com/locate/icarus Triaxial ellipsoid dimensions and poles of asteroids from AO observations at the Keck-II telescope ∗ Jack Drummond a, , Julian Christou b,1,JerryNelsonb a Starfire Optical Range, Directed Energy Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117-5776, United States b University of California Observatories, Center for Adaptive Optics, University of California, Santa Cruz, CA 95064-1077, United States article info abstract Article history: Five main belt asteroids, 2 Pallas, 129 Antigone, 409 Aspasia, 532 Herculina, and 704 Interamnia were Received 8 May 2008 imaged with the adaptive optics system on the 10 m Keck-II telescope in the near infrared on one night, Revised 11 February 2009 August 16, 2006. The three axis dimensions and rotational poles were determined for Pallas, Antigone, Accepted 12 February 2009 Aspasia, and Interamnia, from their changing apparent sizes and shapes as measured with parametric Available online 26 February 2009 blind deconvolution. The rotational pole found for Interamnia is much different from all previous work, Keywords: including our own at Lick Observatory the previous month. Although images of Herculina were obtained Asteroids at only two rotational phases, its rotation appears to be opposite to that predicted from the lightcurve Adaptive optics inversion model of M. Kaasalainen, J. Torppa, and J. Piironen [2002. Icarus 159, 369–395]. A search for satellites was made in all of the asteroid images, with negative results, but three trailing stars around Herculina (200 km diameter), down to 8.9 magnitudes fainter and between 1 and 115 asteroid radii (100 to 11,500 km) from the asteroid, establishes an upper limit of 3.3 km for any object with the same albedo near Herculina.
    [Show full text]
  • The Composition of Centaur 5145 Pholus
    ICARUS 135, 389±407 (1998) ARTICLE NO. IS985997 The Composition of Centaur 5145 Pholus D. P. Cruikshank1 NASA Ames Research Center, MS 245±6, Moffett Field, California 94035-1000 E-mail: [email protected] T. L. Roush NASA Ames Research Center, MS 245-3, Moffett Field, California 94035-1000 M. J. Bartholomew Sterling Software and NASA Ames Research Center, MS 245-3, Moffett Field, California 94035-1000 T. R. Geballe Joint Astronomy Centre, 660 North A'ohoku Place, University Park, Hilo, Hawaii 96720 Y. J. Pendleton NASA Ames Research Center, MS 245±3, Moffett Field, California 94035-1000 S. M. White NASA Ames Research Center, MS 234-1, Moffett Field, California 94035-1000 J. F. Bell, III CRSR, Cornell University, Ithaca, New York 14853 J. K. Davies Joint Astronomy Centre, 660 N. A'ohoku Place, University Park, Hilo, Hawaii 96720 T. C. Owen1 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, Hawaii 96822 C. de Bergh1 Observatoire de Paris, 5 Place Jules Jannsen, 92195 Meudon Cedex, France D. J. Tholen1 Institute for Astronomy, 2680 Woodlawn Dr., Honolulu, Hawaii 96822 M. P. Bernstein SETI Institute and NASA Ames Research Center, MS 245±6, Moffett Field, California 94035-1000 R. H. Brown Lunar and Planetary Laboratory, Univ. of Arizona, Tucson, Arizona 85721 1 Guest observer at the United Kingdom Infared Telescope (UKIRT). UKIRT is operated by the Joint Astronomy Centre on behalf of the United Kingdom Particle Physics and Astronomical Research Council. 389 0019-1035/98 $25.00 Copyright 1998 by Academic Press All rights of reproduction in any form reserved.
    [Show full text]