Non-Principal Axis Rotation (Tumbling) Asteroids
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Non-Principal Axis Rotation (Tumbling) Asteroids
NON-PRINCIPAL AXIS ROTATION (TUMBLING) ASTEROIDS Asteroid PAR Per1 Amp1 Per2 Amp2 Reference 244 Sita T0 129.51 0.82 0 129.51 0.82 Brinsfield, 09 253 Mathilde T 417.7 0.50 –3 417.7 0.45 250. Mottola, 95 –3 418. 0.5 250. Pravec, 05 288 Glauke T 1170. 0.9 –1 1200. 0.9 Harris, 99 0 Pravec, 14 –2 1170. 0.37 740. Pilcher, 15 299∗ Thora T– 272.9 0.50 0 274. 0.39 Pilcher, 14 +2 272.9 0.47 Pilcher, 17 319∗ Leona T 430. 0.5 –2 430. 0.5 1084. Pilcher, 17 341∗ California T 318. 0.92 –2 318. 0.9 250. Pilcher, 17 –2 317.0 0.54 Polakis, 17 –1 317.0 0.92 Polakis, 17 408 Fama T0 202.1 0.58 0 202.1 0.58 Stephens, 08 470 Kilia T0 290. 0.26 0 290. 0.26 Stephens, 09 0 Stephens, 09 496∗ Gryphia T 1072. 1.25 –2 1072. 1.25 Pilcher, 17 571 Dulcinea T 126.3 0.50 –2 126.3 0.50 Stephens, 11 630 Euphemia T0 350. 0.45 0 350. 0.45 Warner, 11 703∗ No¨emi T? 200. 0.78 –1 201.7 0.78 Noschese, 17 0 115.108 0.28 Sada, 17 –2 200. 0.62 Franco, 17 707 Ste¨ına T0 414. 1.00 0 Pravec, 14 763∗ Cupido T 151.5 0.45 –1 151.1 0.24 Polakis, 18 –2 151.5 0.45 101. Pilcher, 18 823 Sisigambis T0 146. -
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. -
The Minor Planet Bulletin 37 (2010) 45 Classification for 244 Sita
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 2, A.D. 2010 APRIL-JUNE 41. LIGHTCURVE AND PHASE CURVE OF 1130 SKULD Robinson (2009) from his data taken in 2002. There is no evidence of any change of (V-R) color with asteroid rotation. Robert K. Buchheim Altimira Observatory As a result of the relatively short period of this lightcurve, every 18 Altimira, Coto de Caza, CA 92679 (USA) night provided at least one minimum and maximum of the [email protected] lightcurve. The phase curve was determined by polling both the maximum and minimum points of each night’s lightcurve. Since (Received: 29 December) The lightcurve period of asteroid 1130 Skuld is confirmed to be P = 4.807 ± 0.002 h. Its phase curve is well-matched by a slope parameter G = 0.25 ±0.01 The 2009 October-November apparition of asteroid 1130 Skuld presented an excellent opportunity to measure its phase curve to very small solar phase angles. I devoted 13 nights over a two- month period to gathering photometric data on the object, over which time the solar phase angle ranged from α = 0.3 deg to α = 17.6 deg. All observations used Altimira Observatory’s 0.28-m Schmidt-Cassegrain telescope (SCT) working at f/6.3, SBIG ST- 8XE NABG CCD camera, and photometric V- and R-band filters. Exposure durations were 3 or 4 minutes with the SNR > 100 in all images, which were reduced with flat and dark frames. -
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. -
I N S I D E T H I S I S S
February / février 2008 Volume/volume 102 Number/numéro 1 [728] This Issue's Winning Astrophoto! FEATURING A FULL COLOUR SECTION! The Journal of the Royal Astronomical Society of Canada Cassiopeia Rising Over the Plaskett by Charles Banville, Victoria Centre. This is a montage of two pictures I took using a Canon 20Da and a Canon EF 17-40mm f/4L lens. The foreground image was acquired at the Dominion Astrophysical Observatory in Victoria on 2007 July 26. That evening the Plaskett Dome was illuminated by a bright 12-day-old Moon. The star trails were created using 87 light frames of 1 minute each taken from Cattle Point on 2007 August 8. Le Journal de la Société royale d’astronomie du Canada [Editor’s Note: The two-member team of Dietmar Kupke and Paul Mortfield of the Toronto Centre selected this late-entry image from among the 30 or so entries to the “Own the Back Cover” con- test. Thanks to all the submitters. We welcome further entries, so don’t delay – send in yours now! INSIDE THIS ISSUE Watch the back cover of the April issue for the next winner.] One Hundred Editions of the Observer's Handbook · Seriously Seeking Ceres! Mont-Mégantic Dark-Sky Reserve Conference, 2007 September 19-21 Duplicity of ZC1042: My First Double-Star Discovery In Memory of Gertrude Jean Southam Building for the International Year of Astronomy (IYA2009) THE ROYAL ASTRONOMICAL SOCIETY OF CANADA February / février 2008 NATIONAL OFFICERS AND COUNCIL FOR 2007-2008/CONSEIL ET ADMINISTRATEURS NATIONAUX Honorary President Robert Garrison, Ph.D., Toronto President Scott Young, B.Sc., Winnipeg Vol. -
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. -
Handbook for Limiting Orbital Debris
NASA-HANDBOOK NASA HANDBOOK 8719.14 National Aeronautics and Space Administration Approved: 2008-07-30 Washington, DC 20546 HANDBOOK FOR LIMITING ORBITAL DEBRIS Measurement System Identification: Metric APPROVED FOR PUBLIC RELEASE – DISTRIBUTION IS UNLIMITED NASA-Handbook 8719.14 This page intentionally left blank. Page 2 of 174 NASA-Handbook 8719.14 DOCUMENT HISTORY LOG Status Document Approval Date Description Revision Baseline 2008-07-30 Initial Release Change 1 2018-04-10 Removed expiration date from the cover page. Page 3 of 174 NASA-Handbook 8719.14 This page intentionally left blank. Page 4 of 174 NASA-Handbook 8719.14 FOREWORD This NASA-Handbook (NASA-HDBK) is published by the National Aeronautics and Space Administration (NASA) to provide the scientific background to NASA’s Orbital Debris Program as defined in NASA Procedural Requirements (NPR) 8715.6, Procedural Requirements for Limiting Orbital Debris, and NASA Standard (NASA-STD) 8719.14, Process for Limiting Orbital Debris. This NASA-HDBK serves as a companion to NPR 8715.6 and NASA-STD 8719.14 and provides each NASA program and project with supporting material to assist in implementing the NPR and the NASA-STD. The uniform engineering, processes, procedures, practices, and methods that have been endorsed in NPR 8715.6 and NASA-STD 8719.14 are further explained in this NASA-HDBK during the selection, application, and design criteria of an item. This NASA-HDBK is consistent with the objectives of the U.S. National Space Policy (August 2006), the U.S. Government Orbital Debris Mitigation Standard Practices (February 2001), the Inter-Agency Space Debris Coordination Committee (IADC) Space Debris Mitigation Guidelines (October 2002), the Space and Missile Center Orbital Debris Handbook, Technical Report on Space Debris (July 2002), and the space debris mitigation guidelines of the Scientific and Technical Subcommittee of the United Nations Committee on the Peaceful Uses of Outer Space, (A/AC.105/720, 1999 and A/AC.105/890, Feb 2007). -
Insidethisissue
February / février 2008 Volume/volume 102 Number/numéro 1 [728] This Issue's Winning Astrophoto! FEATURING A FULL COLOUR SECTION! The Journal of the Royal Astronomical Society of Canada Cassiopeia Rising Over the Plaskett by Charles Banville, Victoria Centre. This is a montage of two pictures I took using a Canon 20Da and a Canon EF 17-40mm f/4L lens. The foreground image was acquired at the Dominion Astrophysical Observatory in Victoria on 2007 July 26. That evening the Plaskett Dome was illuminated by a bright 12-day-old Moon. The star trails were created using 87 light frames of 1 minute each taken from Cattle Point on 2007 August 8. Le Journal de la Société royale d’astronomie du Canada [Editor’s Note: The two-member team of Dietmar Kupke and Paul Mortfield of the Toronto Centre selected this late-entry image from among the 30 or so entries to the “Own the Back Cover” con- test. Thanks to all the submitters. We welcome further entries, so don’t delay – send in yours now! INSIDE THIS ISSUE Watch the back cover of the April issue for the next winner.] One Hundred Editions of the Observer's Handbook · Seriously Seeking Ceres! Mont-Mégantic Dark-Sky Reserve Conference, 2007 September 19-21 Duplicity of ZC1042: My First Double-Star Discovery In Memory of Gertrude Jean Southam Building for the International Year of Astronomy (IYA2009) THE ROYAL ASTRONOMICAL SOCIETY OF CANADA February / février 2008 NATIONAL OFFICERS AND COUNCIL FOR 2007-2008/CONSEIL ET ADMINISTRATEURS NATIONAUX Honorary President Robert Garrison, Ph.D., Toronto President Scott Young, B.Sc., Winnipeg Vol. -
The Minor Planet Bulletin
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 3, A.D. 2007 JULY-SEPTEMBER 53. CCD PHOTOMETRY OF ASTEROID 22 KALLIOPE Kwee, K.K. and von Woerden, H. (1956). Bull. Astron. Inst. Neth. 12, 327 Can Gungor Department of Astronomy, Ege University Trigo-Rodriguez, J.M. and Caso, A.S. (2003). “CCD Photometry 35100 Bornova Izmir TURKEY of asteroid 22 Kalliope and 125 Liberatrix” Minor Planet Bulletin [email protected] 30, 26-27. (Received: 13 March) CCD photometry of asteroid 22 Kalliope taken at Tubitak National Observatory during November 2006 is reported. A rotational period of 4.149 ± 0.0003 hours and amplitude of 0.386 mag at Johnson B filter, 0.342 mag at Johnson V are determined. The observation of 22 Kalliope was made at Tubitak National Observatory located at an elevation of 2500m. For this study, the 410mm f/10 Schmidt-Cassegrain telescope was used with a SBIG ST-8E CCD electronic imager. Data were collected on 2006 November 27. 305 images were obtained for each Johnson B and V filters. Exposure times were chosen as 30s for filter B and 15s for filter V. All images were calibrated using dark and bias frames Figure 1. Lightcurve of 22 Kalliope for Johnson B filter. X axis is and sky flats. JD-2454067.00. Ordinate is relative magnitude. During this observation, Kalliope was 99.26% illuminated and the phase angle was 9º.87 (Guide 8.0). Times of observation were light-time corrected. -
The Minor Planet Bulletin (Warner Et 2010 JL33
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 38, NUMBER 3, A.D. 2011 JULY-SEPTEMBER 127. ROTATION PERIOD DETERMINATION FOR 280 PHILIA – the lightcurve more readable these have been reduced to 1828 A TRIUMPH OF GLOBAL COLLABORATION points with binning in sets of 5 with time interval no greater than 10 minutes. Frederick Pilcher 4438 Organ Mesa Loop MPO Canopus software was used for lightcurve analysis and Las Cruces, NM 88011 USA expedited the sharing of data among the collaborators, who [email protected] independently obtained several slightly different rotation periods. A synodic period of 70.26 hours, amplitude 0.15 ± 0.02 Vladimir Benishek magnitudes, represents all of these fairly well, but we suggest a Belgrade Astronomical Observatory realistic error is ± 0.03 hours rather than the formal error of ± 0.01 Volgina 7, 11060 Belgrade 38, SERBIA hours. Andrea Ferrero The double period 140.55 hours was also examined. With about Bigmuskie Observatory (B88) 95% phase coverage the two halves of the lightcurve looked the via Italo Aresca 12, 14047 Mombercelli, Asti, ITALY same as each other and as in the 70.26 hour lightcurve. Furthermore for order through 14 the coefficients of the odd Hiromi Hamanowa, Hiroko Hamanowa harmonics were systematically much smaller than for the even Hamanowa Astronomical Observatory harmonics. A 140.55 hour period can be safely rejected. 4-34 Hikarigaoka Nukazawa Motomiya Fukushima JAPAN Observers and equipment: Observer code: VB = Vladimir Robert D. Stephens Benishek; AF = Andrea Ferrero; HH = Hiromi and Hiroko Goat Mountain Astronomical Research Station (GMARS) Hamanowa; FP = Frederick Pilcher; RS = Robert Stephens. -
December 1996 the Official Publication of the Hamilton Centre of the Royal Astronomical Society of Canada
PRINTED MATTER RBIT December 1996 Vol. 29, Issue 11 Light Pollution - Toronto, Hamilton, and Buffalo The Official Publication of the Hamilton Centre of The Royal Astronomical Society of Canada Cover Image - Digitally Processed from International Dark Sky Association Image EDITORIAL MEMBERSHIP APPLICATION BY COLIN A. HAIG Application for Membership in the Hamilton Centre of the RASC. Annual membership officially commences October 1. We welcome people of all oliday time and still cloudy skies! Yikes! We have had a record of ages, skills, and interests in things Astronomical. Please make your cheque rotten weather for observing, but that has just meant its time to focus payable to: “RASC Hamilton Centre” and mail to the Treasurer c/o the energies elsewhere, into the Hamilton Centre, instead of into the address on the back. Associate membership is for those in other Astronomy skies. Please welcome a number of new members that have arrived, and let Clubs. Please state the club. Full members receive: The Observer’s them know when you will be out observing, so they can experience our Handbook ($20 value), Journal of RASC ($70 value), SkyNews ($22 value), facilities. I’d also like to extend a hearty welcome to our Trial Members, and and many other great privileges, including discounts on popular magazines, hope that they are finding what they are looking for. As always, if there is supplies and cool stuff. There is a Free 3 month Trial available - send no something of particular interest to you, you are most welcome to mention it to money! Info: Leave a message at: (905) 689-0266. -
Spectral Reflectance Properties of Carbonaceous Chondrites
Icarus 216 (2011) 309–346 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Spectral reflectance properties of carbonaceous chondrites: 2. CM chondrites ⇑ E.A. Cloutis a, , P. Hudon b,1, T. Hiroi c, M.J. Gaffey d, P. Mann a a Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba, Canada R3B 2E9 b Astromaterials Research and Exploration Science Office, NASA Johnson Space Center, Mail Code KR, 2101 NASA Road 1, Houston, TX 77058-3696, USA c Department of Geological Science, Brown University, Box 1846, Providence, RI 02912-1846, USA d Department of Space Studies, University of North Dakota, PO Box 9008, Grand Forks, ND 58202-9008, USA article info abstract Article history: We have examined the spectral reflectance properties and available modal mineralogies of 39 CM carbo- Received 3 May 2011 naceous chondrites to determine their range of spectral variability and to diagnose their spectral features. Revised 6 September 2011 We have also reviewed the published literature on CM mineralogy and subclassification, surveyed the Accepted 7 September 2011 published spectral literature and added new measurements of CM chondrites and relevant end members Available online 16 September 2011 and mineral mixtures, and measured 11 parameters and searched pair-wise for correlations between all quantities. CM spectra are characterized by overall slopes that can range from modestly blue-sloped to Keywords: red-sloped, with brighter spectra being generally more red-sloped. Spectral slopes, as measured by the Asteroids, Surfaces 2.4:0.56 m and 2.4 m:visible region peak reflectance ratios, range from 0.90 to 2.32, and 0.81 to Meteorites l l Spectroscopy 2.24, respectively, with values <1 indicating blue-sloped spectra.