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The Minor Planet Bulletin, Alan W
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 42, NUMBER 2, A.D. 2015 APRIL-JUNE 89. ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2014 SEPTEMBER Lucas Bohn, Brianna Hibbler, Gregory Stein, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected] (Received: 24 November) Photometric data were collected over the course of seven nights in 2014 September for eight asteroids: 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 2699 Kalinin, 3197 Weissman, 7837 Mutsumi, 14927 Satoshi, and (29769) 1999 CE28. Eight asteroids were remotely observed from the Oakley Southern Sky Observatory in New South Wales, Australia. The observations were made on 2014 September 12-14, 16-19 using a 0.50-m f/8.3 Ritchey-Chretien optical tube assembly on a Paramount ME mount and SBIG STX-16803 CCD camera, binned 3x3, with a luminance filter. Exposure times ranged from 90 to 180 sec depending on the magnitude of the target. The resulting image scale was 1.34 arcseconds per pixel. Raw images were processed in MaxIm DL 6 using twilight flats, bias, and dark frames. MPO Canopus was used to measure the processed images and produce lightcurves. In order to maximize the potential for data collection, target asteroids were selected based upon their position in the sky approximately one hour after sunset. Only asteroids with no previously published results were targeted. Lightcurves were produced for 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 3197 Weissman, and (29769) 1999 CE28. -
The Handbook of the British Astronomical Association
THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2012 Saturn’s great white spot of 2011 2011 October ISSN 0068-130-X CONTENTS CALENDAR 2012 . 2 PREFACE. 3 HIGHLIGHTS FOR 2012. 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS. 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S. 7-8 ECLIPSES . 9-15 TIME. 16-17 EARTH AND SUN. 18-20 MOON . 21 SUN’S SELENOGRAPHIC COLONGITUDE. 22 MOONRISE AND MOONSET . 23-27 LUNAR OCCULTATIONS . 28-34 GRAZING LUNAR OCCULTATIONS. 35-36 PLANETS – EXPLANATION OF TABLES. 37 APPEARANCE OF PLANETS. 38 MERCURY. 39-40 VENUS. 41 MARS. 42-43 ASTEROIDS AND DWARF PLANETS. 44-60 JUPITER . 61-64 SATELLITES OF JUPITER . 65-79 SATURN. 80-83 SATELLITES OF SATURN . 84-87 URANUS. 88 NEPTUNE. 89 COMETS. 90-96 METEOR DIARY . 97-99 VARIABLE STARS . 100-105 Algol; λ Tauri; RZ Cassiopeiae; Mira Stars; eta Geminorum EPHEMERIDES OF DOUBLE STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 INTERNET RESOURCES. 110-111 GREEK ALPHABET. 111 ERRATA . 112 Front Cover: Saturn’s great white spot of 2011: Image taken on 2011 March 21 00:10 UT by Damian Peach using a 356mm reflector and PGR Flea3 camera from Selsey, UK. Processed with Registax and Photoshop. British Astronomical Association HANDBOOK FOR 2012 NINETY-FIRST YEAR OF PUBLICATION BURLINGTON HOUSE, PICCADILLY, LONDON, W1J 0DU Telephone 020 7734 4145 2 CALENDAR 2012 January February March April May June July August September October November December Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day Day of of of of of of of of of of of of of of of of of of of of of of of of of Month Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year Week Year 1 Sun. -
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. -
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) .................. -
I N S I D E T H I S I S S
t April / avril 2009 Volume/volume 103 Number/numéro 2 [735] Great Images Share a Galileo Moment The Journal of The Royal Astronomical Society of Canada Mike Wirths writes: My Wife and I are setting up an astronomy B&B in the mountains of northern Baja, Mexico, which is where I took the image on 2008 October 18, 6:00-6:30 p.m. PDT. Le Journal de la Société royale d’astronomie du Canada I used an 18-inch Starmaster + 2.5 Tele Vue Barlow + Infinity 2-2 camera + R/IR True Tech filter. The image was processed in Registax 4 and PhotoShop Creative Suite (PS CS). INSIDE THIS ISSUE Observations Taken of the 1769 Transit • A Major New Observatory in Canada Exploring the Pingualuit Impact Crater • Aboriginal Sky Lore The Art of Gentle Persuasion • Edmonton Centre Observers Measure Asteroid 111 Ate Celebrating the International Year of Astronomy (IYA2009) THE ROYAL ASTRONOMICAL SOCIETY OF CANADA April / avril 2009 NATIONAL OFFICERS AND COUNCIL FOR 2009/CONSEIL ET ADMINISTRATEURS NATIONAUX Honorary President Robert Garrison, Ph.D., Toronto President Dave Lane, Halifax Vol. 103, No. 2 Whole Number 735 1st Vice-President Mary Lou Whitehorne, Halifax 2nd Vice-President Glenn Hawley, B.Sc., B.Ed., Calgary Secretary/Recorder James Edgar, Regina Treasurer Mayer Tchelebon, Toronto, MBA, CMA Past Presidents Scott Young, B.Sc., Winnipeg and Peter Jedicke, M.A. London contents Editor of Journal Jay Anderson, B.Sc., MNRM, Winnipeg Editor of Observer’s Handbook Patrick Kelly, M.Sc., Halifax table des matières Editor of The Beginner’s Observing Guide Leo Enright, -
The Minor Planet Bulletin (Warner Et Al
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 39, NUMBER 3, A.D. 2012 JULY-SEPTEMBER 99. ROTATION PERIOD DETERMINATION FOR 203 others, were also allowed. The only way to fill the large gap in POMPEJA – ANOTHER TRIUMPH OF GLOBAL phase coverage at a single observatory for an Earth commensurate COLLABORATION object is to obtain data from other observatories widely spaced in longitude. Andrea Ferrero in Italy and Hiromi and Hiroko Frederick Pilcher Hamanowa in Japan obtained at the first author's request the 4438 Organ Mesa Loop additional observations required to enable full phase coverage. A Las Cruces, NM 88011 USA total of 14 sessions 2011 Nov. 10 - 2012 Jan. 25 showed a 24.052 [email protected] ± 0.001 hour period, amplitude 0.10 ± 0.01 magnitude and unsymmetric bimodal lightcurve. A lightcurve phased to twice this Andrea Ferrero period showed two halves which were within observational error Bigmuskie Observatory (B88) the same as each other and as the 24.052 hour lightcurve. An via Italo Aresca 12, 14047 Mombercelli, Asti, ITALY irregularly shaped asteroid which was invariant over a 180 degree rotation would be required to produce the 48.1 hour lightcurve. Hiromi Hamanowa, Hiroko Hamanowa The probability of such a symmetric shape for an otherwise Hamanowa Astronomical Observatory irregular real asteroid is so small that it may be safely rejected. 4-34 Hikarigaoka Nukazawa Motomiya Fukushima JAPAN Hence we claim that the 24.052 hour period is the correct one. To make the lightcurve more legible the large number of data points (Received: 30 January) have been binned in sets of three points with a maximum of five Early observations by the first author yielded a rotation minutes between points. -
54 Minor Planet Bulletin 40 (2013) LIGHTCURVE
54 LIGHTCURVE PHOTOMETRY OPPORTUNITIES: create custom lists for objects reaching V d 18.0 during any month 2013 JANUARY-MARCH in the current year, e.g., limiting the results by magnitude and declination. Brian D. Warner Palmer Divide Observatory/MoreData! http://www.minorplanet.info/PHP/call_OppLCDBQuery.php 17995 Bakers Farm Rd. Colorado Springs, CO 80908 USA In a general note, small objects with periods up to 4 hours or even [email protected] longer are possible binaries. For longer periods (4-6 hours or so), the odds of a binary may be less, but the bonus is that the size of Alan W. Harris the secondary, if it exists, is likely larger (see Pravec et al. (2010), MoreData! Nature 466, 1085-1088), thus eclipses, if they occur, will be deeper La Cañada, CA 91011-3364 USA and easier to detect. Petr Pravec The Low Phase Angle list includes asteroids that reach very low Astronomical Institute phase angles. The “D” column is the minimum solar phase angle CZ-25165 Ondejov, CZECH REPUBLIC for the asteroid. Getting accurate, calibrated measurements (usually V band) at or very near the day of opposition can provide Josef urech important information for those studying the “opposition effect.” Astronomical Institute You will have the best chance of success working objects with low Charles University in Prague amplitude and periods that allow covering, e.g., a maximum, every 18000 Prague, CZECH REPUBLIC night. Objects with large amplitudes and/or long periods are much [email protected] more difficult for phase angle studies since, for proper analysis, the data have to be reduced to the average magnitude of the asteroid Lance A.M.