George C. Marshall Space Flight Center, Huntsville, Alabama NASA-GEORGE C
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 3, A.D. 2009 JULY-SEPTEMBER 77. PHOTOMETRIC MEASUREMENTS OF 343 OSTARA Our data can be obtained from http://www.uwec.edu/physics/ AND OTHER ASTEROIDS AT HOBBS OBSERVATORY asteroid/. Lyle Ford, George Stecher, Kayla Lorenzen, and Cole Cook Acknowledgements Department of Physics and Astronomy University of Wisconsin-Eau Claire We thank the Theodore Dunham Fund for Astrophysics, the Eau Claire, WI 54702-4004 National Science Foundation (award number 0519006), the [email protected] University of Wisconsin-Eau Claire Office of Research and Sponsored Programs, and the University of Wisconsin-Eau Claire (Received: 2009 Feb 11) Blugold Fellow and McNair programs for financial support. References We observed 343 Ostara on 2008 October 4 and obtained R and V standard magnitudes. The period was Binzel, R.P. (1987). “A Photoelectric Survey of 130 Asteroids”, found to be significantly greater than the previously Icarus 72, 135-208. reported value of 6.42 hours. Measurements of 2660 Wasserman and (17010) 1999 CQ72 made on 2008 Stecher, G.J., Ford, L.A., and Elbert, J.D. (1999). “Equipping a March 25 are also reported. 0.6 Meter Alt-Azimuth Telescope for Photometry”, IAPPP Comm, 76, 68-74. We made R band and V band photometric measurements of 343 Warner, B.D. (2006). A Practical Guide to Lightcurve Photometry Ostara on 2008 October 4 using the 0.6 m “Air Force” Telescope and Analysis. Springer, New York, NY. located at Hobbs Observatory (MPC code 750) near Fall Creek, Wisconsin. -
Elements of Astronomy
^ ELEMENTS ASTRONOMY: DESIGNED AS A TEXT-BOOK uabemws, Btminwcus, anb families. BY Rev. JOHN DAVIS, A.M. FORMERLY PROFESSOR OF MATHEMATICS AND ASTRONOMY IN ALLEGHENY CITY COLLEGE, AND LATE PRINCIPAL OF THE ACADEMY OF SCIENCE, ALLEGHENY CITY, PA. PHILADELPHIA: PRINTED BY SHERMAN & CO.^ S. W. COB. OF SEVENTH AND CHERRY STREETS. 1868. Entered, according to Act of Congress, in the year 1867, by JOHN DAVIS, in the Clerk's OlBce of the District Court of the United States for the Western District of Pennsylvania. STEREOTYPED BY MACKELLAR, SMITHS & JORDAN, PHILADELPHIA. CAXTON PRESS OF SHERMAN & CO., PHILADELPHIA- PREFACE. This work is designed to fill a vacuum in academies, seminaries, and families. With the advancement of science there should be a corresponding advancement in the facilities for acquiring a knowledge of it. To economize time and expense in this department is of as much importance to the student as frugality and in- dustry are to the success of the manufacturer or the mechanic. Impressed with the importance of these facts, and having a desire to aid in the general diffusion of useful knowledge by giving them some practical form, this work has been prepared. Its language is level to the comprehension of the youthful mind, and by an easy and familiar method it illustrates and explains all of the principal topics that are contained in the science of astronomy. It treats first of the sun and those heavenly bodies with which we are by observation most familiar, and advances consecutively in the investigation of other worlds and systems which the telescope has revealed to our view. -
(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. -
ASTRONOMY and ASTROPHYSICS the Hipparcos Solar System Objects Catalogues?
Astron. Astrophys. 334, 325–336 (1998) ASTRONOMY AND ASTROPHYSICS The Hipparcos solar system objects catalogues? D.Hestroffer1,2, B. Morando2??,E.Høg3, J. Kovalevsky4, L. Lindegren5, and F. Mignard4 1 Astrophysics Division, Space Science Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands 2 Bureau Des Longitudes, URA CNRS 707, 77 Avenue Denfert Rochereau, F-75014 Paris, France 3 Copenhagen University Observatory, Juliane Maries Vej 30, DK-2100 Copenhagen O., Denmark 4 Observatoire de la Coteˆ d’Azur, Departement´ CERGA, UMR CNRS 6527, Av. N. Copernic, F-06130 Grasse, France 5 Lund Observatory, Box 43, S-22100 Lund, Sweden Received 15 October 1997 / Accepted 28 January 1998 Abstract. Astrometric and photometric measurements of a Sun or major planets. Nonetheless, the theoretical precision esti- number of solar system objects were performed by the Hip- mated by Clemence (1948) has never been reached; hence such parcos satellite in both the Hipparcos main mission and the Ty- observations of minor planets enter for instance in the solution cho experiment. The results concern mainly asteroids but also derived by Fricke (1982) for the FK5 with a relatively modest the planetary satellites Europa, Ganymede, Callisto, Titan and weight. Hipparcos should dramatically improve the situation Iapetus, and the major planets Uranus and Neptune. The spe- (e.g. Hestroffer et al. 1995; Bec-Borsenberger et al. 1995), and cific aspects of the Tycho/Hipparcos observations and reduction yield a link between the dynamical system and the ICRS with process implemented for the solar system objects are presented. a precision of the same order of magnitude as the best result Special attention is paid to the error budget of the reduction obtained so far by other means (Folkner et al. -
Observer's Handbook 1980
OBSERVER’S HANDBOOK 1980 EDITOR: JOHN R. PERCY ROYAL ASTRONOMICAL SOCIETY OF CANADA CONTRIBUTORS AND ADVISORS A l a n H. B a t t e n , Dominion Astrophysical Observatory, Victoria, B.C., Canada V 8 X 3X3 (The Nearest Stars). Terence Dickinson, R.R. 3, Odessa, Ont., Canada K0H 2H0 (The Planets). M arie Fidler, Royal Astronomical Society of Canada, 124 Merton St., Toronto, Ont., Canada M4S 2Z2 (Observatories and Planetariums). V ictor Gaizauskas, Herzberg Institute of Astrophysics, National Research Council, Ottawa, Ont., Canada K1A 0R6 (Sunspots). J o h n A. G a l t , Dominion Radio Astrophysical Observatory, Penticton, B.C., Canada V2A 6K3 (Radio Sources). Ian Halliday, Herzberg Institute of Astrophysics, National Research Council, Ottawa, Ont., Canada K1A 0R6 (Miscellaneous Astronomical Data). H e le n S. H o g g , David Dunlap Observatory, University of Toronto, Richmond Hill, Ont., Canada L4C 4Y6 (Foreword). D o n a l d A. M a c R a e , David Dunlap Observatory, University of Toronto, Richmond Hill, Ont., Canada L4C 4Y6 (The Brightest Stars). B r ia n G. M a r s d e n , Smithsonian Astrophysical Observatory, Cambridge, Mass., U.S.A. 02138 (Comets). Janet A. M attei, American Association o f Variable Star Observers, 187 Concord Ave., Cambridge, Mass. U.S.A. 02138 (Variable Stars). P e t e r M. M illm a n , Herzberg Institute o f Astrophysics, National Research Council, Ottawa, Ont., Canada K1A 0R6 (Meteors, Fireballs and Meteorites). A n t h o n y F. J. M o f f a t , D épartement de Physique, Université de Montréal, Montréal, P.Q., Canada H3C 3J7 (Star Clusters). -
A Radar Survey of Main-Belt Asteroids: Arecibo Observations of 55 Objects During 1999–2003
Icarus 186 (2007) 126–151 www.elsevier.com/locate/icarus A radar survey of main-belt asteroids: Arecibo observations of 55 objects during 1999–2003 Christopher Magri a,∗, Michael C. Nolan b,StevenJ.Ostroc, Jon D. Giorgini d a University of Maine at Farmington, 173 High Street—Preble Hall, Farmington, ME 04938, USA b Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA c 300-233, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA d 301-150, Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA Received 3 June 2006; revised 10 August 2006 Available online 24 October 2006 Abstract We report Arecibo observations of 55 main-belt asteroids (MBAs) during 1999–2003. Most of our targets had not been detected previously with radar, so these observations more than double the number of radar-detected MBAs. Our bandwidth estimates constrain our targets’ pole directions in a manner that is geometrically distinct from optically derived constraints. We present detailed statistical analyses of the disk-integrated properties (radar albedo and circular polarization ratio) of the 84 MBAs observed with radar through March 2003; all of these observations are summarized in the online supplementary information. Certain conclusions reached in previous studies are strengthened: M asteroids have higher mean radar albedos and a wider range of albedos than do other MBAs, suggesting that both metal-rich and metal-poor M-class objects exist; and C- and S-class MBAs have indistinguishable radar albedo distributions, suggesting that most S-class objects are chondritic. Also in accord with earlier results, there is evidence that primitive asteroids from outside the C taxon (F, G, P, and D) are not as radar-bright as C and S objects, but a convincing statistical test must await larger sample sizes. -
I(NASA-CR-154510') ASTEROID SURFACE
REFLECTANCE S PECV A By Michael J. Gaffey Thomas B. McCord (NASA-CR-154510') ASTEROID SURFACE N8-'10992 iMATERIALS: MINERALOGICAL.CHARACTERIZATIONS FROM REFLECTANCE SPECTRA (Hawaii Univ.), 147 p HC -A07/MF A01 CSCL 03B Unclas G , to University of Hawaii at Manoa Institute for Astronomy 2680 Woodlawn Drive * Honolulu, Hawaii 96822 Telex: 723-8459 * UHAST HR November 18, 1977 NASA Scientific and Technical Information Facility P.O. Box 8757 Baltimore/Washington Int. Airport Maryland 21240 Gentlemen: RE: Spectroscopy of Asteroids, NSG 7310 Enclosed are two copies of an article entitled "Asteroid Surface Materials: Mineralogical Characterist±cs from Reflectance Spectra," by Dr. Michael J. Gaffey and Dr. Thomas B. McCord, which we have recently submitted for publication to Space Science Reviews. We submit these copies in accordance with the requirements of our NASA grants. Sincerely yours, Thomas B. McCord Principal Investigator TBM:zc Enclosures AN EQUAL OPPORTUNITY EMPLOYER ASTEROID SURFACE MATERIALS: MINERALOGICAL CHARACTERIZATIONS FROM REFLECTANCE SPECTRA By Michael J. Gaffey Thomas B. McCord Institute for Astronomy University of Hawaii at Manoa 2680 Woodlawn Drive Honolulu, Hawaii 96822 Submitted to Space Science Reviews Publication #151 of the Remote Sensing Laboratory Abstract The interpretation of diagnostic parameters in the spectral reflectance data for asteroids provides a means of characterizing the mineralogy and petrology of asteroid surface materials. An interpretive technique based on a quantitative understanding of the functional relationship between the optical properties of a mineral assemblage and its mineralogy, petrology and chemistry can provide a considerably more sophisticated characterization of a surface material than any matching or classification technique. for those objects bright enough to allow spectral reflectance measurements. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) .................. -
Obliquity, Precession Rate, and Nutation Coefficients for a Set of 100 Asteroids
A&A 556, A8 (2013) Astronomy DOI: 10.1051/0004-6361/201321205 & c ESO 2013 Astrophysics Obliquity, precession rate, and nutation coefficients for a set of 100 asteroids C. Lhotka1, J. Souchay2, and A. Shahsavari2 1 Department of Mathematics, University of Rome Tor Vergata, 00133 Rome, Italy 2 Observatoire de Paris, SYRTE/UMR-8630 CNRS, 75014 Paris, France e-mail: [email protected] Received 31 January 2013 / Accepted 18 April 2013 ABSTRACT Context. Thanks to various space missions and the progress of ground-based observational techniques, the knowledge of asteroids has considerably increased in the recent years. Aims. Due to this increasing database that accompanies this evolution, we compute for a set of 100 asteroids their rotational parame- ters: the moments of inertia along the principal axes of the object, the obliquity of the axis of rotation with respect to the orbital plane, the precession rates, and the nutation coefficients. Methods. We select 100 asteroids for which the parameters for the study are well-known from observations or space missions. For each asteroid, we determine the moments of inertia, assuming an ellipsoidal shape. We calculate their obliquity from their orbit (instead of the ecliptic) and the orientation of the spin-pole. Finally, we calculate the precession rates and the largest nutation compo- nents. The number of asteroids concerned leads to some statistical studies of the output. Results. We provide a table of rotational parameters for our set of asteroids. The table includes the obliquity, their axes ratio, their dynamical ellipticity Hd, and the scaling factor K. We compute the precession rate ψ˙ and the leading nutation coefficients Δψ and Δε. -
February 1988
WARREN ASTRONOMICAL SOCIETY The Warren Astronomical Society is a local, non-profit organization of amateur astronomers. The Society holds meetings on the first and third Thursdays of each month, starting at 7:30 P.M., as follows: 1st. Thursday 3rd. Thursday Cranbrook Institute of Science Macomb County Community College 500 Lone Pine Rd. South Campus Bloomfield Hills, MI Building B, Room 216 14500 Twelve Mile Rd. Warren, MI Membership is open to those interested in astronomy and its related fields. Dues are as follows: Student...$8 College...$12 Senior Citizen...$12 Individual...$17 Family...$22 Sky and Telescope Magazine is available for $16.00 per year, and Astronomy Magazine for $14.00 per year. Send membership applications and dues to Russ Patten, 31300 John R. Apt. D, Madison Hgts., MI 48071. Make checks payable to the Warren Astronomical Society. OFFICERS MAILING ADDRESS President : Riyad Matti 548-7511 Warren Astronomical Society lst. V.P. : Ken Strom 977-9489 P.O. Box 474 2nd. V.P. : Clyde Burdette 749-3295 East Detroit, MI 48021 Secretary : Bev Bakanowicz 573-4071 Treasurer : Russ Patten 588-0799 Librarian : Tom MacLaney 541-8198 Deep Sky Group: Doug Bock 750-9369 - Meets at Northern Cross Observatory, Fenton, MI Lunar Group : Alan Rothenberg 355-5844 - Meets at Stargate Observatory, Ray Center, MI WARREN ASTRONOMICAL SOCIETY PAPER Editor: Ken Kelly / 839-7250 Send all articles to THE WASP, 19209 Mapleview, Detroit, MI 48205. The W.A.S.P. is the official publication of the Warren Astronomical Society and is available free to all club members. NEWSLETTER EXCHANGES: Send your Newsletters to: THE WASP, P.O. -
The Minor Planet Bulletin (Warner Et Al., 2011)
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 39, NUMBER 1, A.D. 2012 JANUARY-MARCH 1. LIGHTCURVE ANALYSIS OF 0.00006 h and amplitude of 0.30 ± 0.03 mag. 918 ITHA AND 2008 KONSTITUTSIYA 2008 Konstitutsiya. Observations of this asteroid were started Julian Oey when Oey selected this target from in the CALL website (Warner Kingsgrove Observatory 2011). A request for collaboration was placed on that website. 23 Monaro Ave. Kingsgrove, NSW AUSTRALIA Mazzone and Colazo, who had each independently observed the [email protected] asteroid target for a number of nights, responded. Carlos Colazo We could find no previously reported lightcurve parameters for Observatorio El Gato Gris 2008 Konstitutsiya. Initial observations showed that the lightcurve San Luis 145, Tanti, ARGENTINA was very shallow with a relatively long period that was nearly- commensurate to an Earth day. Mazzone used his Matlab language Fernando Mazzone script software to initially reduce his and Colazo’s data. These Observatorio Río Cuarto scripts incorporate a Fourier algorithm and simultaneously adjust Achalay 1469, Río Cuarto, ARGENTINA any off-set among sessions. He found a period of 11.2688 h. However when the data were pooled with those from Oey, two Andrés Chapman periods emerged: 9.7520 ± 0.0003 h and 11.2694 ± 0.0004 h. Observatorio Cruz del Sur 2556 Chañar St., San Justo, Buenos Aires, ARGENTINA The Mazzone group’s data were also reduced in MPO Canopus v10.4.0.2 using differential photometry to facilitate easy (Received: 12 August) exportation. -
Download This Article in PDF Format
A&A 624, A121 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834541 & © ESO 2019 Astrophysics The shape of (7) Iris as evidence of an ancient large impact??,?? J. Hanuš1, M. Marsset2,3, P. Vernazza4, M. Viikinkoski5, A. Drouard4, M. Brož1, B. Carry6, R. Fetick4,7, F. Marchis8, L. Jorda4, T. Fusco4,7, M. Birlan9, T. Santana-Ros10, E. Podlewska-Gaca10,11, E. Jehin12, M. Ferrais12, J. Grice6,13, P. Bartczak10, J. Berthier9, J. Castillo-Rogez14, F. Cipriani15, F. Colas9, G. Dudzinski´ 10, C. Dumas16, J. Durechˇ 1, M. Kaasalainen5, A. Kryszczynska10, P. Lamy4, H. Le Coroller4, A. Marciniak10, T. Michalowski10, P. Michel6, M. Pajuelo9,17, P. Tanga6, F. Vachier9, A. Vigan4, O. Witasse15, and B. Yang18 1 Institute of Astronomy, Charles University, Prague, V Holešovickáchˇ 2, 18000 Prague 8, Czech Republic e-mail: [email protected]; [email protected] 2 Department of Earth, Atmospheric and Planetary Sciences, MIT, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 3 Astrophysics Research Centre, Queen’s University, Belfast BT7 1NN, UK 4 Aix Marseille Université, CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France 5 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland 6 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France 7 ONERA, The French Aerospace Lab BP72, 29 avenue de la Division Leclerc, 92322 Chatillon Cedex, France 8 SETI Institute, Carl Sagan Center, 189 Bernado Avenue, Mountain View, CA 94043, USA 9 IMCCE, Observatoire