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.
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Minor Planet Bulletin
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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.
For example,
*7.2,13.7.
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.
Pages 203 Klinglesmith III, Daniel A.; Risley, Ethan; Turk, Janek; Vargas, Angelica; Han Xiaming L.; Heffner, Orry R.; Kidd, Adam W.; Magnetta, Bradley J.; Rastede, Frederick W. 2012MPBu...39..203KDownload PDF
The main-belt asteroid 8077 Hoyle was observed on 13 nights over a span of 47 days in 2012 April-May. A bimodal synodic period of 2.7454 ± 0.0002 h and an amplitude of 0.20 ± 0.02 mag. were obtained.
Analysis of observations from North America and Australia of the nearly Earth-commensurate asteroid 247 Eukrate obtained over an interval of more than three months resulted in finding a unique rotation period of 12.093 ± 0.001h, amplitude 0.14 ± 0.02 mag.
Epoch Data in Sidereal Period Determination. I. Initial Constraint from Closest Epochs
Spin vector determination methods that use epoch information require establishing correct rotation counts over long time spans, which can involve ambiguities that are not necessarily correctly handled by purely statistical methods. I present an approach that can be used prior to spin vector analysis, to begin to check how well a given set of lightcurve epoch data can constrain the sidereal period. I also present two precepts to maximize the impact of observing efforts in cases where more epoch data are needed.
A Determination of the Rotational Period of 8882 Sakaetamura
CCD Observations of 8882 Sakaetamura were taken on nine nights between 2012 Jan 7 and 29. Analysis of the data found a synodic period of 4.874 ± 0.002 h with a lightcurve amplitude of 0.60 ± 0.1.
Light Curve for 8345 Ulmerspatz
Pages 207-209 Klinglesmith III, Daniel A.; Ferrero, Andrea; Odden, Caroline; Strabla, Luca; Quadri, Ulisse; Girelli, Roberto 2012MPBu...39..207KDownload PDF
The main-belt asteroid 8345 Ulmerspatz was observed by a collaboration of four observatories on 24 nights between 2011 Nov 24 and 2012 Jan 12, covering solar phase angles between –22.58° and +10.48°. The average synodic period for the entire observing period is estimated to be 17.1192 ± 0.0008 h with an amplitude of 0.70 ± 0.10 mag.
The synodic lightcurve period of 2423 Ibarruri is found to be 139.89 ± 0.03 h. The synodic lightcurve period of 8345 Ulmerspatz is found to be 17.14 ± 0.02 h. For 8345 Ulmerspatz, phase curve parameters are also determined: H = 13.75 ± 0.03, G = –0.14 ± 0.02.
Lightcurve and Rotation Period Determination for Minor Planet 3397 Leyla
Photometric observations of Mars-crossing minor planet 3397 Leyla (1964 XA) was undertaken in March 2012. The resulting synodic rotation period of 3.098 ± 0.002 h and amplitude, A = 0.29 ± 0.05 mag was measured and determined from five nights of observations.
Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory: 2012 January-April
We request that all authors of published lightcurve inversion papers, past and current, submit their results to the DAMIT lightcurve inversion website for permanent retention and ready availability to interested people.
Observations of (47035) 1998 WS between 2012 January and April showed a large change in lightcurve shape. By combining sparse data from the Catalina Asteroid Survey with our dense data set, we have been able to determine a preliminary spin axis and shape model. The synodic period is on the order of 3.995 h. The amplitude ranged from 0.10 to 0.20 mag.
Rotation Period Determinations for 47 Aglaja, 252 Clementina, 611 Valeria, 627 Charis, and 756 Lilliana
A consortium of observers from Australia, Europe, and North America have obtained lightcurves of the previously unobserved asteroid 801 Helwerthia. The period spectrum between 10 and 50 hours is presented, all minima on which have been carefully investigated. We strongly prefer a rotation period 23.93 ± 0.01 hours, amplitude 0.15 ± 0.03 magnitudes, with almost complete phase coverage, and consider all other alias periods to be highly unlikely.
Analysis of CCD photometric observations of the Hungaria asteroid 2074 Shoemaker in 2012 showed a low amplitude lightcurve of 0.08 mag. No definitive period could be found, with those of 2.8, 2.5, and 2.4 hours having nearly equal probability. No evidence was found of a satellite, which was suspected based on data from a previous apparition.
Asteroids Observed from Santana, CS3 and GMARS Observatories: 2012 April - June
Lightcurves of seven asteroids were obtained from Santana Observatory, Goat Mountain Astronomical Research Station (GMARS), and the Center for Solar System Studies (CS3): 412 Elisabetha, 1055 Tynka, 1424, Sundmania, 3493 Stepanov, (6254) 1993 UM3, and (33736) 1999 NY36.
A consortium of observers from Australia, Europe, and North America have obtained full phase coverage of 482 Petrina, and from these observations find a rotation period of 11.794 ± 0.001 hours, amplitude 0.10 ± 0.02 mag, with a highly unsymmetrical but bimodal lightcurve.
CCD photometric observations of the known Hungaria binary 5477 Holmes were made in 2012. Analysis of the data confirmed the previously-determined rotation and orbital periods and size ratio of the secondary to primary. The data will useful for further modeling of the system.
Analysis of CCD photometric observations of the Phocaea asteroid 1090 Sumida in 2012 showed a low amplitude lightcurve of 0.11 mag. A period of 2.7181 h was determined by Fourier analysis. There were indications of a secondary period with several possible solutions. However, none of them were sufficiently convincing.
Lightcurve for 7758: A Possible Binary?
Pages 232-233 Warner, Brian D.; Harris, Alan W.; Pravec, Petr; Kusnirak, Peter; Hornoch, Kamil; Stephens, Robert D.; Pray, Donald P.; Husarik, Marek; Pollock, Joseph; Reichart, Daniel E.; Ivarsen, Kevin M.; Nysewander, Melissa C.; LaCluyze, Aaron P. 2012MPBu...39..232WDownload PDF
Analysis of CCD photometric observations of the Phocaea asteroid 7758 Poulanderson in 2012 found a period of 2.64753 ± 0.00007 h with A = 0.14 mag. Data from two nights showed a possible event due to a satellite. If true, the orbital period would appear to be long, with one solution falling between 59-60 hours and others ranging up to approximately 100 hours.
CCD photometric observations of the main-belt asteroid 205 Martha were obtained from Santana Observatory (MPC 646) in 2012 May - June. The period of 14.912 ± 0.001 h updates several previously reported results.
We present shape and spin axis model for main-belt asteroid 161 Athor. The model was obtained with lightcurve inversion process, using combined dense photometric data from apparition in 1979, 1980, 1982, 2008, 2009, 2010-11 and sparse data from USNO Flagstaff. Analysis of the resulting data found a sidereal period P = 7.280087 ± 0.000005 h and two mirrored pole solution at (350°, -6°) and (170°, 4°), with an error of ± 10 degrees.
Lightcurves for four asteroids were obtained at Phillips Academy Observatory (PAO) and HUT observatory from 2012 March to May: 2927 Alamosa, 4419 Allancook, 5374 Hokutosei, and (28704) 2000 GU91.
CCD photometric observations were made of the near- Earth asteroid, 2012 KP24 during a close flyby in 2012 May. Analysis of more than 700 data points found a period of 0.041667 ± 0.000002 h, or 150.00 ± 0.01 seconds. The maximum amplitude of the asymmetric lightcurve was 0.86 ± 0.03 mag.
Asteroid Lightcurve Analysis at Riverland Dingo Observatory: 1394 Algoa, 1660 Wood, 8882 Sakaetamura, and (15269) 1990 XF
Lightcurves for four asteroids were obtained at Riverland Dingo Observatory (RDO) from 2012 January-June: 1394 Algoa, 1660 Wood, 8882 Sakaetamura, and (15269) 1990 XF.
Analysis of CCD photometric observations of the Hungaria asteroid 7958 Leakey made in 2012 reveals that the object is mostly likely a binary with a primary rotation period of 2.34843 ± 0.00006 h, A = 0.22 mag. The orbital period of the tidally-locked satellite is likely 50.29 ± 0.08 h, although it’s possible that the period is 25.26 ± 0.04 h. The secondary lightcurve shows a bowing (amplitude) of about 0.05 mag, indicating that satellite has a projected a/b ratio of 2/1. Two possible mutual events (occultations/eclipses) were observed. From these, the estimated size ratio of the two bodies is Ds/Dp = 0.30 ± 0.03. Additional observations are needed to confirm these results.
Lightcurves for Shape Modeling: 852 Wladilena, 1089 Tama, and 1180 Rita
The folded lightcurves and synodic periods of 852 Wladilena, 1089 Tama, and 1180 Rita are reported. The data are used by Hanus et al. (2012) to derive the rotation axis and to construct a shape model by applying the inversion lightcurve technique.
Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2012 March - June
Lightcurves for 34 asteroids, including a new Hungaria binary, were obtained at the Palmer Divide Observatory (PDO) from 2012 March to July: 1656 Suomi, 3169 Ostro, 3266 Bernardus, 4116 Elachi, 4483 Petofi, 4490 Bambery, 5968 Trauger, 6107 Osterbrock, 6354 Vangelis, 6517 Buzzi, 6670 Wallach, 7087 Lewotsky, (11304) 1993 DJ, (17129) 1999 JM78, (17590) 1995 CG, (20996) 1986 PB, (23482) 1991 LV, (24702) 1991 OR, (31182) 1997 YZ3, (31881) 2000 FL15, (42811) 1999 JN81, (47143) 1999 LL31, (48307) 2002 LP53, (49674) 1999 SB5, (51302) 2000 KY54, (51381) 2001 BG51, (51386) 2001 CN35, (74081) 1998 OU1, (79472) 1998 AX4, (88259) 2001 HJ7, (326732) 2003 HB6, 2011 WV134, 2012 AA11, and 2012 DO. The Hungaria asteroid (79472) 1998 AX2 showed what appeared to be mutual events (occultations/eclipses) in its lightcurve, likely indicating a satellite. Analysis of the data gives an orbital period of 25.95 ± 0.02 h and size ratio of Ds/Dp ~ 0.32 ± 0.03.
Lightcurve for NEA 2012 LZ1
Pages 252-253 Warner, Brian D.; Harris, Alan W.; Sherrod, P. Clay; Bacci, Paolo; Franco, Lorenzo; Pollock, Joseph; Reichart; Daniel E.; Ivarsen, Kevin M.; Nysewander, Melissa C.; LaCluyze, Aaron P. 2012MPBu...39..252WDownload PDF
Analysis of CCD photometric observations of the near- Earth asteroid 2012 LZ1 during a flyby in 2012 June found a synodic rotation period of 12.87 ± 0.01 h and amplitude A = 0.28 ± 0.03 mag. The data are being used to supplement analysis of radar and other optical observations obtained at the time.
Pages 254-259 Warner, Brian D.; Harris, Alan W.; Pravec, Petr; Durech, Josef; Benner, Lance A.M. 2012MPBu...39..254WDownload PDF
We present lists of asteroid photometry opportunities for objects reaching a favorable apparition and have no or poorly-defined lightcurve parameters. Additional data on these objects will help with shape and spin axis modeling via lightcurve inversion. We also include lists of objects that will be the target of radar observations. Lightcurves for these objects can help constrain pole solutions and/or remove rotation period ambiguities that might not come from using radar data alone.
