The Minor Planet Bulletin BULLETIN OF THE MINOR PLANETS SECTION OF THE ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS
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The Minor Planet Bulletin is the journal for almost all amateurs and even some professionals for publishing
asteroid photometry results, including lightcurves, H-G parameters, color indexes, and shape/spin axis models.
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Authors Guide and Word Templates
(v.2.9: updated 2019 November 14)
The ZIP file contains the Authors Guide PDF as well as a "starter" paper in Word 97 (DOT) and Word 2007+ (DOTX). Please read this updated guide since there are a number of changes from previous guides.
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Smith, J.J.; Jones, A.A. (2019).
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Lightcurves of 165 Loreley obtained on three nights in early 2006 can be satisfied by several different rotation periods, one of which, 7.224 hours, is consistent with the tabulated value, with an amplitude of 0.17 mag.
CCD photometry of asteroids 276 Adelheid, 1490 Limpopo, and 2221 Chilton from the Universidad de Monterrey Observatory
CCD photometry of asteroids 276 Adelheid, 1490 Limpopo, and 2221 Chilton obtained at the Universidad de Monterrey Observatory during August and September 2005 is reported. A synodic rotation period of 6.315±0.005 hours and an amplitude of 0.17±0.03 magnitudes is confirmed for Adelheid from five nights of observations. The resulting synodic rotation period and amplitude for Limpopo is 6.426±0.003 hours and 0.16±0.03 magnitudes from three nights of observations. Chilton was observed on four nights and exhibits a synodic rotation period of 7.445±0.015 hours and an amplitude of 0.20±0.05 magnitudes, though the period is uncertain due to the faintness of the asteroid in the images. Another possible solution for the rotation period of Chilton is 8.63±0.02 hours.
Brightness variation of the asteroid (35690) 1999 CT21
The asteroid (35690) 1999 CT21 was incidentally recorded on 29 and 30 July 2000 UT during the observations of the globular cluster M22. These data have allowed determination of the synodic rotation period to be 9.06 ± 0.02 hours. On 29 July 2000 the reduced V magnitude, the amplitude of the light variation and color index B-V were 14.82 ± 0.01, 0.60 ± 0.02 and 0.7 ± 0.1 mag, respectively. Dimensions and the biaxial ellipsoid models of this asteroid have been obtained for two assumed taxonomic classes (C and S).
Asteroid lightcurve analysis at the Palmer Divide Observatory - February - March 2006
Lightcurves for the following asteroids were obtained at Hunters Hill Observatory and one or more collaborating stations: 2195 Tengstrom, 2501 Lohja, 4580 Child, 9423 Abt, (9992) 1997 TG19, (10909) 1997 XB10, (12271) 1998 RC2, (12290) 1991 LZ, 12317 MadiCampbell, (31383) 1998 XJ94, (33116) 1998 BO12, (34442) 2000 SS64.
A Practical Guide to Lightcurve Photometry and Analysis (Second Edition) by Brian D. Warner. Springer Science + Business Media, 2006. 298 pages, 110 illustrations. ISBN: 0-387-29365-5. (Price $39.95, available at www.springer.com)
Lightcurve analysis of asteroids 53, 698, 1016, 1523, 1950, 4608, 5080 6170, 7760, 8213, 11271, 14257, 15350 and 17509
Pages 92-95 Pray, Donald P.; Galad, Adrian; Gajdos, Stefan; Vilagi, Jozef; Cooney, Walt; Gross, John; Terrel, Dirk; Higgins, David; Husarik, Marek; Kusnirak, Peter 2006MPBu...33...92PDownload PDF
Lightcurve period and amplitude results are reported for fourteen asteroids observed at Carbuncle Hill Observatory and other sites during October 2005 - May 2006. The following synodic periods and amplitudes were determined: 53 Kalypso, 18.075±0.005hr, 0.14mag; 698 Ernestina, 5.0363±0.0005hr, 0.30mag; 1016 Anitra, 5.928±0.001hr, 0.30mag; 1523 Pieksamaki, 5.3202±0.0005hr, 0.50mag; 1950 Wempe, 16.788±0.001hr, 0.98mag; 4608 Wodehouse, 13.95±0.01hr, 0.10mag; 5080 Oja, 7.2220±0.0004hr, 0.37mag; 6170 Levasseur, 2.6529±0.0003hr, 0.14mag; (7760) 1990 RW3, 25.940±0.005hr, 0.32mag; (8213) 1995 FE, 2.911±0.001hr, 0.38mag; (11271) 1988 KB, 6.326±0.001hr, 0.36mag; (14257) 2000 AR97, 13.584±0.002hr, 0.67mag; 15350 Naganuma, 2.5835±0.0001hr, 0.20mag; 17509 Ikumadan, 5.788±0.001hr, 0.40mag.
Observations spanning more than two months reveal the synodic period of the main-belt asteroid 774 Armor to be 25.162±0.002hr with an amplitude of 0.37±0.02mag. This study affirmed the importance of both collaboration and having data from widely separated locations.
Lightcurves analysis of 10 asteroids from Leura Observatory
Hungaria asteroid 6384 Kervin is found to have a synodic lightcurve period of 3.6203±0.0003hr and amplitude 0.10±0.02mag. The period and size are such that the asteroid was a binary candidate. No signs of mutual events were seen; however, initial runs showed slight, but eventually unsubstantiated, indications of a secondary period. Observations at other viewing aspects are encouraged to rule out a binary nature completely.
Asteroid lightcurve photometry from Santana and GMARS observatories - winter and spring 2006
Lightcurve period and amplitude results from Santana and GMARS Observatories are reported for 2006 January - June. 58 Concordia (9.895±0.002hr and 0.10mag.), 268 Adorea (7.800±0.002hr and 0.16mag.), 293 Brasilia (8.17±0.01hr and 0.20mag.), (6185) 1997 YD (21.05±0.01hr and 0.34mag.), (19204) 1992 ME (3.17±0.01hr and 0.04mag.)
The main-belt asteroid, 71 Niobe, was the target of radar observations in early 2006 by Shepard. Supporting optical observations (lightcurve) were requested. Initial optical observations by Warner indicated the previously reported period of 14.38h (Harris 1989a) may have been incorrect. Follow up observations, optical and radar, showed that a synodic period of 35.6±0.1h is more likely correct. The observed amplitude is 0.22±0.02mag.
The main-belt asteroid 1304 Arosa was observed in late 2005 and early 2006 in a collaborative effort by observers in France, Italy and the United States. A period of 7.7478±0.0001hr with an amplitude 0.375±0.011 mag was derived.
Observations of 1043 Beate in April 2006 found the synodic period to be 22.05±0.10hr or, possibly, 44.10±0.10hr. The lightcurve amplitude was 0.32±0.02mag. The synodic period for 1186 Turnera was determined to be 12.066±0.004hr based on observations also obtained in April 2006; its lightcurve amplitude was 0.34±0.02mag. With both having adopted periods nearly commensurate with 24hr, the importance of collaboration among observers at different longitudes was again demonstrated. This was particularly true in the case of 1043 Beate, where combined runs allowed forming a single long run on more than one occasion, and so provided additional clues in finding a solution.
Lightcurve analysis of asteroids 453 Tea and 454 Mathesis
For members of the ALPO Minor Planets Section and readers of the Minor Planet Bulletin, it is useful to review the outcome and implications of the resolutions passed at the XXVIth General Assembly of the International Astronomical Union (IAU) held August 14-25 in Prague.
Lightcurve photometry opportunities October - December 2006
We present here four lists of “targets of opportunity” for the period 2006 October through December. The first list is those asteroids reaching a favorable apparition during this period, are <15m at brightest, and have either no or poorly constrained lightcurve parameters. By “favorable” we mean the asteroid is unusually brighter than at other times. In many cases, a favorable apparition may not come again for many years. The goal for these asteroids is to find a well-determined rotation rate, if at all possible. Don’t hesitate to solicit help from other observers at widely spread longitudes should the initial finding for the period indicated that it will be difficult for a single station to find the period.