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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. -
Occultation Newsletter Volume 8, Number 4
Volume 12, Number 1 January 2005 $5.00 North Am./$6.25 Other International Occultation Timing Association, Inc. (IOTA) In this Issue Article Page The Largest Members Of Our Solar System – 2005 . 4 Resources Page What to Send to Whom . 3 Membership and Subscription Information . 3 IOTA Publications. 3 The Offices and Officers of IOTA . .11 IOTA European Section (IOTA/ES) . .11 IOTA on the World Wide Web. Back Cover ON THE COVER: Steve Preston posted a prediction for the occultation of a 10.8-magnitude star in Orion, about 3° from Betelgeuse, by the asteroid (238) Hypatia, which had an expected diameter of 148 km. The predicted path passed over the San Francisco Bay area, and that turned out to be quite accurate, with only a small shift towards the north, enough to leave Richard Nolthenius, observing visually from the coast northwest of Santa Cruz, to have a miss. But farther north, three other observers video recorded the occultation from their homes, and they were fortuitously located to define three well- spaced chords across the asteroid to accurately measure its shape and location relative to the star, as shown in the figure. The dashed lines show the axes of the fitted ellipse, produced by Dave Herald’s WinOccult program. This demonstrates the good results that can be obtained by a few dedicated observers with a relatively faint star; a bright star and/or many observers are not always necessary to obtain solid useful observations. – David Dunham Publication Date for this issue: July 2005 Please note: The date shown on the cover is for subscription purposes only and does not reflect the actual publication date. -
Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1
Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals. -
Observing Water in Our Solar System
Observing water in our Solar System Colin Snodgrass Ice in our Solar System www.nightsky.ie www.nightsky.ie 250 K 150 K 50 K Equilibrium temperature drops with distance ( d-½ ) Present day snow line is at ~2.7 AU from Sun, in asteroid belt. Ice exists on surfaces in Kuiper Belt. In inner solar system, sublimation drives cometary activity. Kuiper Belt Objects – Haumea Spectroscopy of KBOs, particularly in the NIR, reveals differences in their surface ices. Haumea ‘family’ have spectra that match almost pure water ice. Remains from a collision. We used the VLT+Hawk-I to identify ices on potential family members using photometry. Snodgrass et al 2010, Carry et al (submitted) Further Family Members Ragozzine & Brown (2007, AJ 134, p2160) published a list of further family member candidates selected on dynamical grounds. The orbits in the TN region (and interactions with resonances) make this difficult to do. Need to confirm that they share the same water ice surface to be true family members. However, most are too faint for the NIR spectroscopy that can unambiguously detect water ice. Water Ice Detection We use HAWK-I at the VLT to perform J and CH4 band photometry, using the CH4 band as a narrower H band. We confirm that our measurements of (J-Hs) are sensitive to water ice. We measured this colour for 18 objects. 6 are objects previously claimed as family members - they have strongly negative (J-Hs). 2 other objects are confirmed as family members, 2003 SQ317 and 2005 CB79. The remaining 10 (including non-candidate Eris, observed for comparison) have positive values and we rule out water ice surfaces. -
The Minor Planet Bulletin Is Open to Papers on All Aspects of 6500 Kodaira (F) 9 25.5 14.8 + 5 0 Minor Planet Study
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 32, NUMBER 3, A.D. 2005 JULY-SEPTEMBER 45. 120 LACHESIS – A VERY SLOW ROTATOR were light-time corrected. Aspect data are listed in Table I, which also shows the (small) percentage of the lightcurve observed each Colin Bembrick night, due to the long period. Period analysis was carried out Mt Tarana Observatory using the “AVE” software (Barbera, 2004). Initial results indicated PO Box 1537, Bathurst, NSW, Australia a period close to 1.95 days and many trial phase stacks further [email protected] refined this to 1.910 days. The composite light curve is shown in Figure 1, where the assumption has been made that the two Bill Allen maxima are of approximately equal brightness. The arbitrary zero Vintage Lane Observatory phase maximum is at JD 2453077.240. 83 Vintage Lane, RD3, Blenheim, New Zealand Due to the long period, even nine nights of observations over two (Received: 17 January Revised: 12 May) weeks (less than 8 rotations) have not enabled us to cover the full phase curve. The period of 45.84 hours is the best fit to the current Minor planet 120 Lachesis appears to belong to the data. Further refinement of the period will require (probably) a group of slow rotators, with a synodic period of 45.84 ± combined effort by multiple observers – preferably at several 0.07 hours. The amplitude of the lightcurve at this longitudes. Asteroids of this size commonly have rotation rates of opposition was just over 0.2 magnitudes. -
Appendix 1 897 Discoverers in Alphabetical Order
Appendix 1 897 Discoverers in Alphabetical Order Abe, H. 22 (7) 1993-1999 Bohrmann, A. 9 1936-1938 Abraham, M. 3 (3) 1999 Bonomi, R. 1 (1) 1995 Aikman, G. C. L. 3 1994-1997 B¨orngen, F. 437 (161) 1961-1995 Akiyama, M. 14 (10) 1989-1999 Borrelly, A. 19 1866-1894 Albitskij, V. A. 10 1923-1925 Bourgeois, P. 1 1929 Aldering, G. 3 1982 Bowell, E. 563 (6) 1977-1994 Alikoski, H. 13 1938-1953 Boyer, L. 40 1930-1952 Alu, J. 20 (11) 1987-1993 Brady, J. L. 1 1952 Amburgey, L. L. 1 1997 Brady, N. 1 2000 Andrews, A. D. 1 1965 Brady, S. 1 1999 Antal, M. 17 1971-1988 Brandeker, A. 1 2000 Antonini, P. 25 (1) 1996-1999 Brcic, V. 2 (2) 1995 Aoki, M. 1 1996 Broughton, J. 179 1997-2002 Arai, M. 43 (43) 1988-1991 Brown, J. A. 1 (1) 1990 Arend, S. 51 1929-1961 Brown, M. E. 1 (1) 2002 Armstrong, C. 1 (1) 1997 Broˇzek, L. 23 1979-1982 Armstrong, M. 2 (1) 1997-1998 Bruton, J. 1 1997 Asami, A. 5 1997-1999 Bruton, W. D. 2 (2) 1999-2000 Asher, D. J. 9 1994-1995 Bruwer, J. A. 4 1953-1970 Augustesen, K. 26 (26) 1982-1987 Buchar, E. 1 1925 Buie, M. W. 13 (1) 1997-2001 Baade, W. 10 1920-1949 Buil, C. 4 1997 Babiakov´a, U. 4 (4) 1998-2000 Burleigh, M. R. 1 (1) 1998 Bailey, S. I. 1 1902 Burnasheva, B. A. 13 1969-1971 Balam, D. -
Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2013 Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites Driss Takir [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Part of the The Sun and the Solar System Commons Recommended Citation Takir, Driss, "Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites. " PhD diss., University of Tennessee, 2013. https://trace.tennessee.edu/utk_graddiss/1783 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Driss Takir entitled "Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Harry Y. McSween Jr., Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffery E. Moersch, Michael W. Guidry Accepted for the Council: Carolyn R. Hodges Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Nature and Degree of Aqueous Alteration of Outer Main Belt Asteroids and CM and CI Carbonaceous Chondrites A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Driss Takir May 2013 Copyright © 2013 by Driss Takir All rights reserved. -
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) .................. -
The Minor Planet Bulletin Are Indexed in the Astrophysical Data System (ADS) and So Can Be Referenced by Others in Subsequent Papers
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 4, A.D. 2017 OCTOBER-DECEMBER 287. PHOTOMETRIC OBSERVATIONS OF MAIN-BELT were operated at sensor temperature of –15°C and images were ASTEROIDS 1990 PILCHER AND 8443 SVECICA calibrated with dark and flat-field frames. Stephen M. Brincat Both telescopes and cameras were controlled remotely from a Flarestar Observatory (MPC 171) nearby location via Sequence Generator Pro (Binary Star Fl.5/B, George Tayar Street Software). Photometric reduction, lightcurve construction, and San Gwann SGN 3160, MALTA period analyses were done using MPO Canopus software (Warner, [email protected] 2017). Differential aperture photometry was used and photometric measurements were based on the use of comparison stars of near- Winston Grech solar colour that were selected by the Comparison Star Selector Antares Observatory (CSS) utility available through MPO Canopus. Asteroid 76/3, Kent Street magnitudes were based on MPOSC3 catalog supplied with MPO Fgura FGR 1555, MALTA Canopus. (Received: 2017 June 8) 1990 Pilcher is an inner main-belt asteroid that was discovered on 1956 March 9 by K. Reinmuth at Heidelberg. Also known as 1956 We report on photometric observations of two main-belt EE, this asteroid was named in honor of Frederick Pilcher, asteroids, 1990 Pilcher and 8443 Svecica, that were associate professor of physics at Illinois College, Jacksonville acquired from 2017 March to May. We found the (Illinois), who has promoted extensively, the interest in minor synodic rotation period of 1990 Pilcher as 2.842 ± planets among amateur astronomers (Schmadel & Schmadel, 0.001 h and amplitude of 0.08 ± 0.03 mag and of 8443 1992). -
The Minor Planet Bulletin (Warner Et Al., 2009A)
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 36, NUMBER 4, A.D. 2009 OCTOBER-DECEMBER 133. NEW LIGHTCURVES OF 8 FLORA, 13 EGERIA, consistent with a period near 12.9 h. Hollis et. al. (1987) derived a 14 IRENE, 25 PHOCAEA, 40 HARMONIA, 74 GALATEA, period of 12.790 h. Di Martino (1989) and Harris and Young AND 122 GERDA (1989) also found periods of approximately 12.87 h, as did Piiornen et al. (1998). Torppa et al. (2003) found a sidereal period Frederick Pilcher of 12.79900 h using lightcurve inversion techniques. Several 4438 Organ Mesa Loop attempts have also been made to determine the spin axis Las Cruces, NM 88011 USA orientation for Flora. Hollis et al. (1987) reported a pole longitude [email protected] near 148° while Di Martino et al. (1989) found two possible solutions at longitude 140° or 320°. Torppa et al. (2003) found a (Received: 2009 Jun 30 Revised: 2009 Aug 2) pole solution of (160°, +16°) and sidereal period of 12.79900 h, similar to (155°, +5°) found by Durech (2009a), both using lightcurve inversion methods. Durech’s sidereal period, however, New lightcurves yield synodic rotation periods and was 12.86667 h. amplitudes for: 8 Flora, 12.861 ± 0.001 h, 0.08 ± 0.01 mag; 13 Egeria, 7.0473 ± 0.0001 h, 0.15 ± 0.02 mag in New observations of the asteroid obtained by the author on 8 2007, 0.37 ± 0.02 mag in 2009; 14 Irene, 15.089 ± nights from 2009 Feb. -
The Planetary and Lunar Ephemerides DE430 and DE431
IPN Progress Report 42-196 • February 15, 2014 The Planetary and Lunar Ephemerides DE430 and DE431 William M. Folkner,* James G. Williams,† Dale H. Boggs,† Ryan S. Park,* and Petr Kuchynka* ABSTRACT. — The planetary and lunar ephemerides DE430 and DE431 are generated by fitting numerically integrated orbits of the Moon and planets to observations. The present-day lunar orbit is known to submeter accuracy through fitting lunar laser ranging data with an updated lunar gravity field from the Gravity Recovery and Interior Laboratory (GRAIL) mission. The orbits of the inner planets are known to subkilometer accuracy through fitting radio tracking measurements of spacecraft in orbit about them. Very long baseline interfer- ometry measurements of spacecraft at Mars allow the orientation of the ephemeris to be tied to the International Celestial Reference Frame with an accuracy of 0′′.0002. This orien- tation is the limiting error source for the orbits of the terrestrial planets, and corresponds to orbit uncertainties of a few hundred meters. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of fitting spacecraft tracking data. The orbits of Uranus, Neptune, and Pluto are determined primarily from astrometric observations, for which measurement uncertainties due to the Earth’s atmosphere, combined with star catalog uncertainties, limit position accuracies to several thousand kilometers. DE430 and DE431 differ in their integrated time span and lunar dynamical modeling. The dynamical model for DE430 included a damping term between the Moon’s liquid core and solid man- tle that gives the best fit to lunar laser ranging data but that is not suitable for backward integration of more than a few centuries. -
Close Encounters of Asteroids Before and During the ESA GAIA Mission
A&A 406, 751–758 (2003) Astronomy DOI: 10.1051/0004-6361:20030641 & c ESO 2003 Astrophysics Close encounters of asteroids before and during the ESA GAIA mission A. Fienga, J.-F. Bange, A. Bec-Borsenberger, and W. Thuillot Institut de m´ecanique c´eleste et de calcul deseph´ ´ em´erides (IMCCE) – Observatoire de Paris, UMR 8028 du CNRS, 77 avenue Denfert-Rochereau, 75014 Paris, France Received 15 October 2002 / Accepted 15 April 2003 Abstract. Observation of close encounters of asteroids is a powerful method to determine their masses. A systematic search of such close encounters of asteroids with diameters larger than 40 km has been made thanks to a procedure to select the most efficient phenomena by means of the observable gravitational deflection. This study allows us to give lists of such single (one encounter) and multiple (several encounters between two pairs of asteroids) phenomena that will be observable from ground based astrometric telescopes from 2003 to 2022. We also give lists of single and multiple phenomena spanning 2010-2022 and implying less sensitive deflections only accessible by space astrometry. These last encounters may be observed during the ESA GAIA space mission. Key words. minor planets, asteroids – astrometry – celestial mechanics – methods: observational 1. Introduction mass of Ceres (Schubart 1971; Landgraf 1988; Goffin 1991; Williams 1983; Viateau & Rapaport 1998; Michałak 2001). The determination of the masses of asteroids remains a primor- With similar methods, several papers recently led also to the dial problem to be solved in order to improve our knowledge determination of the mass of smaller asteroids from ground- of the dynamics of the asteroid families.