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.
It is considered to be a refereed journal by the SAO/NASA ADS.
All MPB papers are indexed in the ADS.
Print subscriptions are no longer available to individuals. Institutions (e.g., college libraries) can still
obtain print copies via a special subscription. See details in MPB 37-4 or contact the editor, Richard Binzel.
Annual voluntary contributions of $5.00 or more in support of the publication are welcome.
Please send a check, drawn on a U.S. bank and payable in U.S. funds, to "Minor Planet Bulletin" and send it to:
Minor Planet Bulletin
c/o Melissa Hayes-Gehrke
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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.
The Pts column is no longer required and has been removed from the template for the standard table
to allow more room for the other columns.
The phase column should have only two values: for the first and last date in the range.
If the phase reaches an extrema between those dates, put an asterisk before the first value.
Use semicolons to separate names in the references section. For example:
Smith, J.J.; Jones, A.A. (2019).
This also applies if using several references to the same author in the text. For example:
"This asteroid was observed at three previous apparitions (Jones, 2015; 2017; 2018)..."
Issues for the upcoming quarter-year are released on about the 21st of March, June, September, and December.
Full issues and individual papers from vol 1 (1973) to present are available via links on this page.
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Vol 1-7 run Jul-Jun. Vol 8-present run Jan-Dec. Only papers indexed in the ADS are included.
Earlier volumes often contain more papers than listed here. It's recommended to download the
full issue in vol 1-9.
We report results obtained by the “Magnitude Alert Project” (MAP) during the first ten years of activity, from 1996 to 2006. As of December 31, 2006 the MAP Database contained 430 asteroids and 4927 measures. 16 minor planets, for which visual and CCD measures indicate an average difference of H magnitude from the current predicted values, have been observed at least during three oppositions. These confirmed discrepancies are from 0.3 to 2.6 magnitudes. We suggest a revision of their catalogued H magnitude to permit better predicted magnitudes in ephemerides of these objects, notably by the Minor Planet Center.
Observations of asteroid 335 Roberta show the synodic period to be 12.054 ± 0.003 hr. The amplitude of the somewhat unusually shaped lightcurve is 0.13 ± 0.02 mag.
Lightcurve Analysis of 235 Carolina
Pages 100 Warner, Brian D.; Stephens, Robert D.; Behrend, Raoul; Poncy, Raymond; Klotz, Alain; Dyvig, Ron; Reddy, Vishnu; Antonini, Pierre; Crippa, Roberto; Leroy, Arnaud; Goncalves, Rui; Kryszczynka, Agnieszka; Barbotin, Eric 2007MPBu...34..100WDownload PDF
The lightcurve of main-belt asteroid 235 Carolina was obtained by an international group of observers in January-February 2007. The synodic period was found to be 17.1600 ± 0.0004 hr with the lightcurve having an amplitude of 0.30 ± 0.02 mag.
6615 Plutarchos was observed from Leura and Carbuncle Hill Observatories in April and May 2007. The synodic period is reported to be 2.3247 ± 0.0001 h. This asteroid also has a partial solution as a binary with asynchronous orbital period of 40.02 ± 0.1 h
Photometry from GMARS and Santana Observatories - April to June 2007
Lightcurves for 12 asteroids were obtained at the Palmer Divide Observatory from March through May 2007: 28 Bellona, 56 Melete, 148 Gallia, 223 Rosa, 273 Atropos, 747 Winchester, 3940 Larion, (5384) 1957 VA, 5390 Huichiming, 6029 Edithrand, (15822) 1994 TV15, and (29515) 1997 YL7. In addition, a revised period is given for 10261 Nikdollezhal’.
Lightcurves of Minor Planets 559 Nanon and 1602 Indiana
Lightcurves of 559 Nanon reveal a rotation period of 10.059 ± 0.001 hr and amplitude of 0.26 ± 0.03 mag. Lightcurves of 1602 Indiana reveal a rotation period of 2.601 ± 0.001 hr and an amplitude of 0.17 ± 0.03 mag.
The Rotation Periods of 873 Holda, 3028 Zhangguoxi 3497 Innanen, 5484 Inoda, 5654 Terni, and 7304 Namiki
Lightcurves for 872 Holda, 3028 Zhangguoxi, 3497 Innanen, 5484 Inoda, 5654 Terni, and 7304 Namiki were obtained at the Via Capote Observatory in April and May 2007. The derived synodic periods were: 872 Holda, 5.943 ± 0.002 hr; 3028 Zhangguoxi, 4.827 ± 0.001 hr; 3497 Innanen, 7.181 ± 0.001 hr; 5484 Inoda, 14.144 ± 0.009 hr; 5654 Terni, 9.99 ± 0.01 hr; 7304 Namiki, 8.90 ± 0.02 hr.
One of the main obstacles to studies of the asteroid population, NEAs in particular, is the lack of good H (absolute magnitude) and G (phase slope) values. Starting in early 2007, the Palmer Divide Observatory began a dedicated program for determining the H-G values for as many asteroids as possible. The initial efforts involved MBA asteroids as a control group where the results were compared to values given in the MPCORB file (MPC 2007). Subsequent observations will concentrate on brighter targets within the NEA and inner main-belt populations. A consequence of these observations is also the determination of the V-R color index for almost all targeted asteroids. This paper discusses the details of the project, from strategy to implementation, as well as reporting some initial findings.
Asteroid Lightcurve Analysis at the Oakley Observatory - March/April 2007
Lightcurves for 24 asteroids were collected over six nights of observing during March and April of 2007 at the Oakley Observatory. The asteroids were: 234 Barbara, 279 Thule, 303 Josephina, 348 May, 621 Werdandi, 715 Transvaalia, 791 Ani, 1132 Hollandia, 1164 Kobolda, 1184 Gaea, 1385 Gelria, 1534 Nasi, 2341 Aoluta, 2582 Harimaya-Bashi, 2887 Krinov, 3166 Klondike, 3310 Patsy, 3451 Mentor, 3497 Innanen, 3575 Anyuta, 5484 Inoda, (7792) 1995 WZ3, (9873) 1992 GH, and (41577) 2000 SV2.
Observing Program "T3": Finding Comets in the Asteroid Population
An observing program to search for cometary features among the asteroidal population is presented. No additional instruments other than those normally used for minor planet observations are necessary. The involved observers periodically receive an observing planner by email and the observing results are shared over the internal mailing list. Once confirmed, results are communicated to the professional community.
High-speed Photometric Analysis for Minor Planets 1586 Thiele, 4246 Telemann, (10662) 32-1 T-2, and (49880) 1999 XP 135
Synodic rotation periods and amplitudes for five mainbelt asteroids observed at the Calvin-Rehoboth Observatory are reported: 1335 Demoulina, 2658 Gingerich, 3091 van den Heuvel, 8887 Scheeres, and (12168) 5141 T-2. The asteroid 2658 Gingerich is a binary candidate, having exhibited a possible eclipse. The asteroid (12168) 5141 T-2 has an amplitude of 1.44 mag, matching the largest value established for main belt objects.
Minor planet 3406 Omsk was observed over six nights in May 2007. The synodic period was determined as 7.275 ± 0.006 hr. The peak to peak amplitude was approximately 0.28 magnitudes, implying an axial ratio (a/b) of 1.3.
Asteroid Lightcurve Analysis from Volunteer Observatory During April and May 2007
We present here four lists of “targets of opportunity” for the period 2007 October-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.