DOCSLIB.ORG

Appendix 1 1311 Discoverers in Alphabetical Order

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Appendix 1 1311 Discoverers in Alphabetical Order Appendix 1 1311 Discoverers in Alphabetical Order Abe, H. 28 (8) 1993-1999 Bernstein, G. 1 1998 Abe, M. 1 (1) 1994 Bettelheim, E. 1 (1) 2000 Abraham, M. 3 (3) 1999 Bickel, W. 443 1995-2010 Aikman, G. C. L. 4 1994-1998 Biggs, J. 1 2001 Akiyama, M. 16 (10) 1989-1999 Bigourdan, G. 1 1894 Albitskij, V. A. 10 1923-1925 Billings, G. W. 6 1999 Aldering, G. 4 1982 Binzel, R. P. 3 1987-1990 Alikoski, H. 13 1938-1953 Birkle, K. 8 (8) 1989-1993 Allen, E. J. 1 2004 Birtwhistle, P. 56 2003-2009 Allen, L. 2 2004 Blasco, M. 5 (1) 1996-2000 Alu, J. 24 (13) 1987-1993 Block, A. 1 2000 Amburgey, L. L. 2 1997-2000 Boattini, A. 237 (224) 1977-2006 Andrews, A. D. 1 1965 Boehnhardt, H. 1 (1) 1993 Antal, M. 17 1971-1988 Boeker, A. 1 (1) 2002 Antolini, P. 4 (3) 1994-1996 Boeuf, M. 12 1998-2000 Antonini, P. 35 1997-1999 Boffin, H. M. J. 10 (2) 1999-2001 Aoki, M. 2 1996-1997 Bohrmann, A. 9 1936-1938 Apitzsch, R. 43 2004-2009 Boles, T. 1 2002 Arai, M. 45 (45) 1988-1991 Bonomi, R. 1 (1) 1995 Araki, H. 2 (2) 1994 Borgman, D. 1 (1) 2004 Arend, S. 51 1929-1961 B¨orngen, F. 535 (231) 1961-1995 Armstrong, C. 1 (1) 1997 Borrelly, A. 19 1866-1894 Armstrong, M. 2 (1) 1997-1998 Bourban, G. 1 (1) 2005 Asami, A. 7 1997-1999 Bourgeois, P. 1 1929 Asher, D. J. 10 1994-1995 Bowell, E. 571 (7) 1977-1994 Augustesen, K. 26 (26) 1982-1987 Boyer, L. 40 1930-1952 Brady, J. L. 1 1952 Baade, W. 10 1920-1949 Brady, N. 7 (3) 1999-2001 Babiakov´a, U. 13 (13) 1998-2001 Brady, S. 2 1999 Bailey, S. I. 1 1902 Brandeker, A. 4 2000 Balam, D. D. 32 (1) 1987-2007 Brcic, V. 2 (2) 1995 Ball, L. 89 2000-2004 Broughton, J. 1031 1997-2008 Balonek, T. J. 8 (1) 1991-1995 Brown, J. A. 1 (1) 1990 Bancilhon, O. 1 1934 Brown, M. E. 21 (21) 2001-2008 Banh, S. 1 1998 Broˇzek, L. 23 1979-1982 Bannister, N. P. 1 (1) 1998 Bruton, J. 2 1997 Banno, Y. 1 (1) 1983 Bruton, W. D. 5 (5) 1999-2000 Barbieri, C. 4 2000-2003 Bruwer, J. A. 4 1953-1970 Barentine, J. C. 1 (1) 2004 Buchar, E. 1 1925 Barkume, K. M. 1 (1) 2004 Buie, M. W. 555 (7) 1997-2007 Barr, E. 5 1983 Buil, C. 5 1997 Barros, S. 5 (4) 1975-1977 Burks, G. 1 (1) 1998 Bartolini, S. 1 (1) 1999 Burleigh, M. R. 1 (1) 1998 Barucci, M. A. 3 (2) 1984-1985 Burnasheva, B. A. 13 1969-1971 Bauersima, I. 1 (1) 1972 Burnham, R. 1 (1) 1964 Baur, J. M. 14 (6) 1987-1990 Bus, E. S. 1 1977 Beatty, D. 1 (1) 1980 Bus, S. J. 1675 (331) 1975-1989 Becker, A. C. 243 (10) 2004-2006 Busch, M. 3 (3) 2009 Bedient, J. 3 (2) 2004-2005 Buttani, P. 1 (1) 1997 Beeson, E. S. 1 2005 Buzzi, L. 6 (3) 2001-2007 Behrend, R. 6 (5) 2003-2006 Behymer, B. E. 1 (1) 1983 Calanca, R. 2 (1) 1995 Bell, G. 54 (47) 1998-2000 Cameron, R. C. 1 1950 Bellini, F. 2 (2) 2001-2003 Candy, M. P. 5 (3) 1980-1984 Belyaev, Yu. A. 6 (6) 1968 Candy, V. M. 2 (2) 1984 Belyavskij, S. I. 36 (3) 1912-1927 Carnera, L. 16 (3) 1901-1902 Bergeron, D. 2 1999-2000 Carona, D. W. 1 (1) 1999 Bernardi, F. 3 (2) 2002-2004 Caronia, A. 4 (4) 1998-2000 Bernasconi, L. 8 1999 Carrasco, R. 1 1935 Berney, K. 1 (1) 1997 Carsenty, U. 1 (1) 1996 L.D. Schmadel, Dictionary of Minor Planet Names, DOI 10.1007/978-3-642-29718-2, © Springer-Verlag Berlin Heidelberg 2012 1312 Appendix 1 Casacci, C. 2 (2) 1995-1996 Cunningham, L. E. 4 1951-1952 Casady, L. 3 (3) 2001-2003 Curtis, H. D. 1 1913 Casarramona, F. 2 (2) 1998 Cwach, K. F. J. 1 1989 Casas, R. 2 (1) 1998-1999 Castellani, F. 6 (6) 1996-1998 D’Abramo, G. 3 (3) 1999 Casulli, V. S. 164 1993-2010 d’Arrest, H. 1 1862 Cattani, G. 18 (18) 1994-1997 Dal Prete, I. 1 (1) 1998 Cavadore, C. 1 (1) 2000 Danzl, N. 6 (1) 1995-1998 Cavagna, M. 19 (18) 1994-1998 Davis, D. 1 (1) 1999 Cavalletti, G. 1 (1) 1999 Davis, R. G. 4 1996-1998 Cecce, A. J. 17 2000-2001 Dawson, M. 5 2005-2006 Cecchini, V. 2 (2) 1998-2000 de Ball, L. 1 1882 Cernis,ˇ E. 1 (1) 2008 De Cat, P. 9 (3) 2004-2005 Cernis,ˇ K. 49 (43) 2001-2010 de Gasparis, A. 9 1849-1865 Cerulli, V. 1 1910 de Pascual, M. 1 1982 Cesco, C. U. 20 (14) 1965-1971 De Queiroz, J. 3 2009 Cesco, M. R. 6 1974-1976 de Saint-Aignan, C. P. 12 1991-1994 Chaboyer, B. 1 2000 De Sanctis, G. 42 (38) 1978-1986 Chacornac, J. 6 1853-1860 Debehogne, H. 735 (118) 1965-2003 Chamberlin, M. T. 2 1997 DeGraff, D. R. 2 (2) 1997 Chang, C.-H. 1 1957 Delahodde, C. E. 1 (1) 2000 Chang, M.-T. 5 (5) 2006 Dellinger, J. 52 (33) 2000-2009 Chang, Y. C. 2 1928-1957 Delporte, E. 66 1925-1942 Charlois, A. 99 1887-1904 Delsanti, A. C. 2 (2) 1999-2000 Chassagne, R. 1 (1) 2000 Demeautis, C. 7 (6) 1997-2004 Chemin, R. 1 1985 Derekas, A. 3 (3) 2001 Chen, J. 10 (10) 1994-1997 Deutsch, A. N. 1 1929 Chen, T. 1 (1) 2009 Devore, H. 1 (1) 2008 Chernykh, L. I. 266 (18) 1966-1992 DeYoung, J. 1 1993 Chernykh, N. S. 539 (19) 1966-1986 di Cicco, D. 59 1994-1997 Chesney, D. K. 38 1998-2000 Di Clemente, A. 1 (1) 1996 Chestnov, D. N. 8 (8) 2009 Di Paola, A. 11 (11) 1996-1997 Chiang, E. 1 (1) 2002 Di Sora, M. 2 (2) 1998-1999 Chiavenna, P. 15 (15) 1995-2000 Dieckvoss, W. 2 1938 Child, J. B. 13 (10) 1992-1999 Dillon, E. R. 1 (1) 1998 Choo, K.-J. 1 (1) 2001 Dillon, W. G. 37 (25) 1996-2009 Christensen, P. R. 1 (1) 1985 Dimai, A. 1 2000 Christophe, B. 54 2003-2010 Dixon, D. S. 16 (1) 1998-2009 Churms, J. 2 1953 Djurkovic, P. 2 1936-1940 Ciffreo, J. 1 1984 Dobrzycki, J. 1 (1) 1949 Clem, J. L. 1 2002 Donati, S. 22 (1) 1998-2000 Clingan, R. 43 2001-2007 Doressoundiram, A. 1 (1) 2002 Coddington, E. F. 3 1898-1899 Dossin, F. 5 1981-1984 Cofre, S. 6 (6) 1968 Duczmal, L. 2 (2) 1999 Coggia, J. 5 1868-1899 Dugan, R. S. 16 1902-1904 Cohen, S. 1 (1) 1991 Dunbar, R. S. 10 (7) 1981-1987 Coker, R. 4 (4) 1988 Dunn, A. 1 1992 Colas, F. 1 (1) 2000 Dupouy, P. 2 (2) 1997-1998 Collander-Brown, S. 1 (1) 2002 Durig, D. T. 34 (3) 2000-2009 Collier, M. 2 (2) 1998 Durman, C. F. 1 (1) 1996 Collins, M. 40 (40) 1999-2002 Dusi´c, M. 2 (2) 1998 Colombini, E. 3 1981-1998 Dyvig, R. 16 2001-2002 Colzani, E. 1 (1) 1993 Comas Sol´a, J. 11 1915-1930 Eastman, M. 5 (5) 2004-2009 Comba, P. G. 634 1995-2003 Edmonds, J. 1 2002 Cooney Jr, W. R. 43 (24) 1998-2004 Eglitis, I. 2 (2) 2008-2010 Cottenot, P. 1 1878 Ehring, N. 5 1997-1999 Courty, F. 2 1894 Elenin, L. 7 2008-2009 Cowell, P. H. 1 1909 Elliot, J. L. 1 (1) 2002 Crawford, G. 3 2001-2002 Elst, E. W. 3812 (102) 1986-2009 Crespo da Silva, L. 1 1999 Emerson, G. 1 1995 Cross, K. 2 1994-1996 Emmerich, M. 1 (1) 2009 Cruz, A. 2 (2) 2001 Endate, K. 606 (570) 1987-2008 Appendix 1 1313 Ernst, E. 1 1910 Goldstein, D. B. 1 1985 Esquerdo, G. A. 1 (1) 2004 G´omez, J. J. 1 2000 Evans, W. 1 (1) 2000 Gonnessiat, F. 2 1918-1920 Ewen-Smith, B. M. 1 (1) 1996 Gonzalez, L. E. 2 1981-1982 Goretti, V. 31 (5) 1993-1999 Fagioli, G. 4 (4) 2003-2008 G¨otz, P. 20 (2) 1903-1905 Falla, N. 5 2009 Graham, A. 1 1848 Farnham, T. L. 2 2000 Grav, T. 2 (2) 2000 Faul, K. L. 1 1977 Graziani, M. 2 (2) 2007-2009 Fedon, G. 3 (3) 1999 Greimel, R. 1 2001 Ferguson, J. 3 1854-1860 Grennan, D. 1 2008 Ferrando, M. 4 (4) 2005 Griesser, M. 7 2001-2007 Ferrando, R. 112 (4) 2001-2010 Griffin, I. P. 25 (3) 1998-2001 Ferreri, W. 18 (4) 1984-1988 Grigsby, A. 2 (1) 2003 Ferrero, M. 2 (2) 1930 Groeneveld, I. ∗ 2 (1) 1955-1956 Ferr´ın, I. R. 9 (7) 2000-2006 Gross, J. 4 (4) 2004 Fiedler, M. 3 2005 Grossman, A. 1 1984 Fisch, G. 1 (1) 1992 Gualdoni, C. 1 (1) 1994 Fitzsimmons, A. 8 (8) 1993-2002 Guarro, J. 5 1999-2001 Foerster, W. 1 (1) 1860 Guidetti, D. 2 (2) 1998-2000 Fogh Olsen, H. J. 9 (9) 1984-1987 Guido, E. 3 2005 Foglia, S. 2 2005 Gulbis, A. 2 2005 Forti, G. 48 (48) 1977-2001 Gustava, C.
Load more

Recommended publications
  • Asteroid Shape and Spin Statistics from Convex Models J
    Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen To cite this version: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen. Asteroid shape and spin statistics from convex models. Icarus, Elsevier, 2008, 198 (1), pp.91. 10.1016/j.icarus.2008.07.014. hal-00499092 HAL Id: hal-00499092 https://hal.archives-ouvertes.fr/hal-00499092 Submitted on 9 Jul 2010 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Accepted Manuscript Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen PII: S0019-1035(08)00283-2 DOI: 10.1016/j.icarus.2008.07.014 Reference: YICAR 8734 To appear in: Icarus Received date: 18 September 2007 Revised date: 3 July 2008 Accepted date: 7 July 2008 Please cite this article as: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen, Asteroid shape and spin statistics from convex models, Icarus (2008), doi: 10.1016/j.icarus.2008.07.014 This is a PDF file of an unedited manuscript that has been accepted for publication.
    [Show full text]
  • 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]
  • Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations*
    Multiple Asteroid Systems: Dimensions and Thermal Properties from Spitzer Space Telescope and Ground-Based Observations* F. Marchisa,g, J.E. Enriqueza, J. P. Emeryb, M. Muellerc, M. Baeka, J. Pollockd, M. Assafine, R. Vieira Martinsf, J. Berthierg, F. Vachierg, D. P. Cruikshankh, L. Limi, D. Reichartj, K. Ivarsenj, J. Haislipj, A. LaCluyzej a. Carl Sagan Center, SETI Institute, 189 Bernardo Ave., Mountain View, CA 94043, USA. b. Earth and Planetary Sciences, University of Tennessee 306 Earth and Planetary Sciences Building Knoxville, TN 37996-1410 c. SRON, Netherlands Institute for Space Research, Low Energy Astrophysics, Postbus 800, 9700 AV Groningen, Netherlands d. Appalachian State University, Department of Physics and Astronomy, 231 CAP Building, Boone, NC 28608, USA e. Observatorio do Valongo/UFRJ, Ladeira Pedro Antonio 43, Rio de Janeiro, Brazil f. Observatório Nacional/MCT, R. General José Cristino 77, CEP 20921-400 Rio de Janeiro - RJ, Brazil. g. Institut de mécanique céleste et de calcul des éphémérides, Observatoire de Paris, Avenue Denfert-Rochereau, 75014 Paris, France h. NASA Ames Research Center, Mail Stop 245-6, Moffett Field, CA 94035-1000, USA i. NASA/Goddard Space Flight Center, Greenbelt, MD 20771, United States j. Physics and Astronomy Department, University of North Carolina, Chapel Hill, NC 27514, U.S.A * Based in part on observations collected at the European Southern Observatory, Chile Programs Numbers 70.C-0543 and ID 72.C-0753 Corresponding author: Franck Marchis Carl Sagan Center SETI Institute 189 Bernardo Ave. Mountain View CA 94043 USA [email protected] Abstract: We collected mid-IR spectra from 5.2 to 38 µm using the Spitzer Space Telescope Infrared Spectrograph of 28 asteroids representative of all established types of binary groups.
    [Show full text]
  • 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.
    [Show full text]
  • 1620 Geographos and 433 Eros: Shaped by Planetary Tides?
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server 1620 Geographos and 433 Eros: Shaped by Planetary Tides? W. F. Bottke, Jr. Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853-6801 D. C. Richardson Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195 P. Michel Osservatorio Astronomico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy and S. G. Love Jet Propulsion Laboratory, California Institute of Technology, M/S 306-438, 4800 Oak Grove Drive, Pasadena, CA 91109-8099 Received 23 September 1998; accepted 10 December 1998 –2– ABSTRACT Until recently, most asteroids were thought to be solid bodies whose shapes were determined largely by collisions with other asteroids (Davis et al., 1989). It now seems that many asteroids are little more than rubble piles, held together by self-gravity (Burns 1998); this means that their shapes may be strongly distorted by tides during close encounters with planets. Here we report on numerical simulations of encounters between a ellipsoid-shaped rubble-pile asteroid and the Earth. After an encounter, many of the simulated asteroids develop the same rotation rate and distinctive shape (i.e., highly elongated with a single convex side, tapered ends, and small protuberances swept back against the rotation direction) as 1620 Geographos. Since our numerical studies show that these events occur with some frequency, we suggest that Geographos may be a tidally distorted object. In addition, our work shows that 433 Eros, which will be visited by the NEAR spacecraft in 1999, is much like Geographos, which suggests that it too may have been molded by tides in the past.
    [Show full text]
  • PACS Sky Fields and Double Sources for Photometer Spatial Calibration
    Document: PACS-ME-TN-035 PACS Date: 27th July 2009 Herschel Version: 2.7 Fields and Double Sources for Spatial Calibration Page 1 PACS Sky Fields and Double Sources for Photometer Spatial Calibration M. Nielbock1, D. Lutz2, B. Ali3, T. M¨uller2, U. Klaas1 1Max{Planck{Institut f¨urAstronomie, K¨onigstuhl17, D-69117 Heidelberg, Germany 2Max{Planck{Institut f¨urExtraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany 3NHSC, IPAC, California Institute of Technology, Pasadena, CA 91125, USA Document: PACS-ME-TN-035 PACS Date: 27th July 2009 Herschel Version: 2.7 Fields and Double Sources for Spatial Calibration Page 2 Contents 1 Scope and Assumptions 4 2 Applicable and Reference Documents 4 3 Stars 4 3.1 Optical Star Clusters . .4 3.2 Bright Binaries (V -band search) . .5 3.3 Bright Binaries (K-band search) . .5 3.4 Retrieval from PACS Pointing Calibration Target List . .5 3.5 Other stellar sources . 13 3.5.1 Herbig Ae/Be stars observed with ISOPHOT . 13 4 Galactic ISOCAM fields 13 5 Galaxies 13 5.1 Quasars and AGN from the Veron catalogue . 13 5.2 Galaxy pairs . 14 5.2.1 Galaxy pairs from the IRAS Bright Galaxy Sample with VLA radio observations 14 6 Solar system objects 18 6.1 Asteroid conjunctions . 18 6.2 Conjunctions of asteroids with pointing stars . 22 6.3 Planetary satellites . 24 Appendices 26 A 2MASS images of fields with suitable double stars from the K-band 26 B HIRES/2MASS overlays for double stars from the K-band search 32 C FIR/NIR overlays for double galaxies 38 C.1 HIRES/2MASS overlays for double galaxies .
    [Show full text]
  • Ty996i the Astronomical Journal Volume 71, Number
    coPC THE ASTRONOMICAL JOURNAL VOLUME 71, NUMBER 6 AUGUST 1966 TY996I Observations of Comets, Minor Planets, and Satellites Elizabeth Roemer* and Richard E. Lloyd U. S. Naval Observatory, Flagstaff Station, Arizona (Received 10 May 1966) Accurate positions and descriptive notes are presented for 38 comets, 33 minor planets, 5 faint natural satellites, and Pluto, for which astrometric reduction of the series of Flagstaff observations has been completed. THE 1022 positions and descriptive notes presented reference star positions; therefore, she bears responsi- here supplement those given by Roemer (1965), bility for the accuracy of the results given here. who also described the program, the equipment used, Coma diameters and tail dimensions given in the and the procedures of observation and of reduction. Notes to Table I refer to the exposures taken for In this paper as in the earlier one, the participation astrometric purposes unless otherwise stated. In of those who shared in critical phases of the work is general, longer exposures show more extensive head and indicated in the Obs/Meas column of Table I according tail structure. to the following letters: For brighter comets the minimum exposure is determined by the necessity of recording measurable R=Elizabeth Roemer. images of 12th-13th magnitude reference stars. On Part-time assistants under contract Nonr-3342(00) such exposures the position of the nuclear condensation with Lowell Observatory: may be more or less obscured by the overexposed coma and be correspondingly difficult and uncertain to L = Richard E. Lloyd, measure. T = Maryanna Thomas, A colon has been used to indicate greater than normal S = Marjorie K.
    [Show full text]
  • On the Accuracy of Restricted Three-Body Models for the Trojan Motion
    DISCRETE AND CONTINUOUS Website: http://AIMsciences.org DYNAMICAL SYSTEMS Volume 11, Number 4, December 2004 pp. 843{854 ON THE ACCURACY OF RESTRICTED THREE-BODY MODELS FOR THE TROJAN MOTION Frederic Gabern1, Angel` Jorba1 and Philippe Robutel2 Departament de Matem`aticaAplicada i An`alisi Universitat de Barcelona Gran Via 585, 08007 Barcelona, Spain1 Astronomie et Syst`emesDynamiques IMCCE-Observatoire de Paris 77 Av. Denfert-Rochereau, 75014 Paris, France2 Abstract. In this note we compare the frequencies of the motion of the Trojan asteroids in the Restricted Three-Body Problem (RTBP), the Elliptic Restricted Three-Body Problem (ERTBP) and the Outer Solar System (OSS) model. The RTBP and ERTBP are well-known academic models for the motion of these asteroids, and the OSS is the standard model used for realistic simulations. Our results are based on a systematic frequency analysis of the motion of these asteroids. The main conclusion is that both the RTBP and ERTBP are not very accurate models for the long-term dynamics, although the level of accuracy strongly depends on the selected asteroid. 1. Introduction. The Restricted Three-Body Problem models the motion of a particle under the gravitational attraction of two point masses following a (Keple- rian) solution of the two-body problem (a general reference is [17]). The goal of this note is to discuss the degree of accuracy of such a model to study the real motion of an asteroid moving near the Lagrangian points of the Sun-Jupiter system. To this end, we have considered two restricted three-body problems, namely: i) the Circular RTBP, in which Sun and Jupiter describe a circular orbit around their centre of mass, and ii) the Elliptic RTBP, in which Sun and Jupiter move on an elliptic orbit.
    [Show full text]
  • Planetary Science : a Lunar Perspective
    APPENDICES APPENDIX I Reference Abbreviations AJS: American Journal of Science Ancient Sun: The Ancient Sun: Fossil Record in the Earth, Moon and Meteorites (Eds. R. 0.Pepin, et al.), Pergamon Press (1980) Geochim. Cosmochim. Acta Suppl. 13 Ap. J.: Astrophysical Journal Apollo 15: The Apollo 1.5 Lunar Samples, Lunar Science Insti- tute, Houston, Texas (1972) Apollo 16 Workshop: Workshop on Apollo 16, LPI Technical Report 81- 01, Lunar and Planetary Institute, Houston (1981) Basaltic Volcanism: Basaltic Volcanism on the Terrestrial Planets, Per- gamon Press (1981) Bull. GSA: Bulletin of the Geological Society of America EOS: EOS, Transactions of the American Geophysical Union EPSL: Earth and Planetary Science Letters GCA: Geochimica et Cosmochimica Acta GRL: Geophysical Research Letters Impact Cratering: Impact and Explosion Cratering (Eds. D. J. Roddy, et al.), 1301 pp., Pergamon Press (1977) JGR: Journal of Geophysical Research LS 111: Lunar Science III (Lunar Science Institute) see extended abstract of Lunar Science Conferences Appendix I1 LS IV: Lunar Science IV (Lunar Science Institute) LS V: Lunar Science V (Lunar Science Institute) LS VI: Lunar Science VI (Lunar Science Institute) LS VII: Lunar Science VII (Lunar Science Institute) LS VIII: Lunar Science VIII (Lunar Science Institute LPS IX: Lunar and Planetary Science IX (Lunar and Plane- tary Institute LPS X: Lunar and Planetary Science X (Lunar and Plane- tary Institute) LPS XI: Lunar and Planetary Science XI (Lunar and Plane- tary Institute) LPS XII: Lunar and Planetary Science XII (Lunar and Planetary Institute) 444 Appendix I Lunar Highlands Crust: Proceedings of the Conference in the Lunar High- lands Crust, 505 pp., Pergamon Press (1980) Geo- chim.
    [Show full text]
  • (704) Interamnia from Its Occultations and Lightcurves
    International Journal of Astronomy and Astrophysics, 2014, 4, 91-118 Published Online March 2014 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2014.41010 A 3-D Shape Model of (704) Interamnia from Its Occultations and Lightcurves Isao Satō1*, Marc Buie2, Paul D. Maley3, Hiromi Hamanowa4, Akira Tsuchikawa5, David W. Dunham6 1Astronomical Society of Japan, Yamagata, Japan 2Southwest Research Institute, Boulder, USA 3International Occultation Timing Association, Houston, USA 4Hamanowa Astronomical Observatory, Fukushima, Japan 5Yanagida Astronomical Observatory, Ishikawa, Japan 6International Occultation Timing Association, Greenbelt, USA Email: *[email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Received 9 November 2013; revised 9 December 2013; accepted 17 December 2013 Copyright © 2014 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract A 3-D shape model of the sixth largest of the main belt asteroids, (704) Interamnia, is presented. The model is reproduced from its two stellar occultation observations and six lightcurves between 1969 and 2011. The first stellar occultation was the occultation of TYC 234500183 on 1996 De- cember 17 observed from 13 sites in the USA. An elliptical cross section of (344.6 ± 9.6 km) × (306.2 ± 9.1 km), for position angle P = 73.4 ± 12.5˚ was fitted. The lightcurve around the occulta- tion shows that the peak-to-peak amplitude was 0.04 mag. and the occultation phase was just be- fore the minimum.
    [Show full text]
  • HUBBLE ULTRAVIOLET SPECTROSCOPY of JUPITER TROJANS Ian Wong1†, Michael E
    Draft version March 11, 2019 Preprint typeset using LATEX style emulateapj v. 12/16/11 HUBBLE ULTRAVIOLET SPECTROSCOPY OF JUPITER TROJANS Ian Wong1y, Michael E. Brown2, Jordana Blacksberg3, Bethany L. Ehlmann2,3, and Ahmed Mahjoub3 1Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA; [email protected] 2Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 3Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA y51 Pegasi b Postdoctoral Fellow Draft version March 11, 2019 ABSTRACT We present the first ultraviolet spectra of Jupiter Trojans. These observations were carried out using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope and cover the wavelength range 200{550 nm at low resolution. The targets include objects from both of the Trojan color sub- populations (less-red and red). We do not observe any discernible absorption features in these spectra. Comparisons of the averaged UV spectra of less-red and red targets show that the subpopulations are spectrally distinct in the UV. Less-red objects display a steep UV slope and a rollover at around 450 nm to a shallower visible slope, whereas red objects show the opposite trend. Laboratory spectra of irradiated ices with and without H2S exhibit distinct UV absorption features; consequently, the featureless spectra observed here suggest H2S alone is not responsible for the observed color bimodal- ity of Trojans, as has been previously hypothesized. We propose some possible explanations for the observed UV-visible spectra, including complex organics, space weathering of iron-bearing silicates, and masked features due to previous cometary activity.
    [Show full text]
  • Astrocladistics of the Jovian Trojan Swarms
    MNRAS 000,1–26 (2020) Preprint 23 March 2021 Compiled using MNRAS LATEX style file v3.0 Astrocladistics of the Jovian Trojan Swarms Timothy R. Holt,1,2¢ Jonathan Horner,1 David Nesvorný,2 Rachel King,1 Marcel Popescu,3 Brad D. Carter,1 and Christopher C. E. Tylor,1 1Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD, Australia 2Department of Space Studies, Southwest Research Institute, Boulder, CO. USA. 3Astronomical Institute of the Romanian Academy, Bucharest, Romania. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Jovian Trojans are two swarms of small objects that share Jupiter’s orbit, clustered around the leading and trailing Lagrange points, L4 and L5. In this work, we investigate the Jovian Trojan population using the technique of astrocladistics, an adaptation of the ‘tree of life’ approach used in biology. We combine colour data from WISE, SDSS, Gaia DR2 and MOVIS surveys with knowledge of the physical and orbital characteristics of the Trojans, to generate a classification tree composed of clans with distinctive characteristics. We identify 48 clans, indicating groups of objects that possibly share a common origin. Amongst these are several that contain members of the known collisional families, though our work identifies subtleties in that classification that bear future investigation. Our clans are often broken into subclans, and most can be grouped into 10 superclans, reflecting the hierarchical nature of the population. Outcomes from this project include the identification of several high priority objects for additional observations and as well as providing context for the objects to be visited by the forthcoming Lucy mission.
    [Show full text]