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.
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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
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Authors Guide and Word Templates
(v.3.0: updated 2024 February 2)
The ZIP file contains the Authors Guide PDF as well as a "starter" paper in Word 2007+ (DOTX).
Those using Word 97 (DOC/DOT) are encouraged to download
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the most recent Word format (DOCX). Please read this updated guide since there are a number of changes from previous guides.
A new, optional, table is available for those wanting to include physical and
discovery information
in a more accessible way.
See the announcement in Minor Planet Bulletin51-2.
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.
Asteroid 5331 Erimomisaki was observed between 2007 Nov. 30 and 2008 Jan. 9. A synodic period of 24.26 ± 0.02 h with a mean amplitude of 0.27 ± 0.02 mag was derived.
A Collection of Lightcurves from Modra: 2007 December- 2008 June
Lightcurve analysis led to rotation periods of main-belt asteroids 651 Antikleia, 653 Berenike, 2363 Cebriones, 12482 Pajka, 23327 Luchernandez, (28292) 1999 CX54, and (74424) 1999 BN. Only tentative results were obtained for rotation periods of 17102 Begzhigitova, 27270 Guidotti, and (74056) 1998 KM9.
New observations at Organ Mesa and Hunters Hill Observatories 2008 March and April show that 161 Athor has a synodic period of 7.281 ± 0.001 h and, during that time, a monomodal lightcurve with amplitude of 0.08 ± 0.02 magnitudes. An approximate pole position is also reported.
A collaborative effort from two widely-separated geographical longitudes resulted in three nights of long, continuous observations of 788 Hohensteina. The 14-hour, non-overlapping lightcurve allowed us to constrain the synodic period of the asteroid to 37.176 ± 0.004 h with an amplitude of 0.18 ± 0.03 mag.
Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory: 2008 March
Photometric data for 17 asteroids were collected over ten nights of observing during 2008 February and March at the Oakley Southern Sky Observatory. The asteroids were: 170 Maria, 266 Aline, 426 Hippo, 441 Bathilde, 619 Triberga, 701 Oriola, 840 Zenobia, 1175 Margo, 1232 Cortusa, 1297 Quadea, 1309 Hyperborea, 1355 Magoeba, 1505 Koranna, 2120 Tyumenia, 2606 Odessa, 3428 Roberts, and 4254 Kamel.
Lightcurve Analysis of 102 Miriam, 1433 Geramtina, and 2648 Owa
Pages 151-152 Johnson, Thomas; Pech, Katherin; van Schilfgaarde, Ryan; Chase, Matt; Burns, M. Shane 2008MPBu...35..151JDownload PDF
Asteroids 102 Miriam, 1433 Geramtina,and 2648 Owa were observed from NURO facilities in Flagstaff, AZ. Synodic rotation periods were estimated for each asteroid. Miriam’s period was estimated to be 15.789 h. We were able to estimate a lower limit the period of Geramtina to be 14 h. Owa’s period is 3.563 h
The lightcurves for the following asteroids are reported: 305 Gordonia, 316 Goberta, 608 Adolfine, 707 Steina, 710 Gertrud, 1187 Afra, 1216 Askania, 1325 Inanda, 1462 Zamenhoff, 1559 Kustaanheimo, 1671 Chaika, 1999 Hirayama, 2075 Martinez, 2094 Magnitka, 2444 Lederle, 3156 Ellington, 4264 Karljosephine, and 7895 Kaseda. Three of these (707, 1325, and 4264) are slow rotators.
Lightcurve Analysis of Asteroids 3036 Krat, 3285 Ruth Wolfe and 5448 Siebold
Pages 160-161 Hummel, Jacob; Postma, Angela; Sumter, George C.; Moore, Harold; Sweet, Samantha; Beaky, Matthew M. 2008MPBu...35..160HDownload PDF
Main-belt asteroids 3036 Krat, 3285 Ruth Wolfe, and 5448 Siebold were observed by the authors. 3036 Krat, observed at Lowell Observatory in 2007 December, was found to have a period of 9.61 ± 0.01 h. For the other two asteroids, both observed at the Truman Observatory in 2007, we found 3285 Ruth Wolfe to have a period of 3.919 ± 0.001 h and 5448 Siebold was determined to have a period of 2.929 ± 0.001 h.
CCD Photometry of Three Short-period Asteroids from the Universidad de Monterry Observatory
CCD photometry of three asteroids was obtained at the Universidad de Monterrey Observatory during 2007 April and 2008 March. These asteroids were observed on only one or two nights, but complete lightcurves were obtained due to relatively short rotation periods. The resulting synodic rotation periods and amplitudes are as follows: 811 Nauheima, 4.011 ± 0.006 h, 0.11 ± 0.03 mag; 3787 Aivazovskij, 2.97 ± 0.01 h, 0.18 ± 0.02 mag; and 5474 Gingasen, 3.628 ± 0.005 h, 0.16 ± 0.03 mag.
Asteroid Lightcurve Analysis at the Palmer Divide Observatory: February-May 2008
The authors present shape and spin axis models for four asteroids: 54 Alexandra, 167 Urda, 409 Aspasia, and 1022 Olympiada. The models were constructed using a combination of dense lightcurves and sparse data sets from USNO observations for lightcurve inversion. The use of combined dense and sparse data sets in order to find asteroid models will become more common as next-generation large surveys come on line.
A Preliminary Shape and Spin Axis Model for 595 Polyxena
Photometric observations made at the Palmer Divide Observatory during the 2006 and 2008 apparitions of the main-belt asteroid 595 Polyxena were combined with dense lightcurves from 1993 included in the Uppsala Asteroid Photometric Catalog and a sparse lightcurve based on data from the USNO to determine a preliminary shape and spin axis model. Two solutions dominated the result set, one prograde (? = 42°, ß = 8°) and one retrograde (l = 222°, l = -4°). The uncertainty in each coordinate is ± 5°. The sidereal period was found to be 11.794162 ± 0.000023 h.
7233 Majella was observed over eight nights in May 2008. The synodic period was determined as 3.812 ± 0.004 h. The peak-to-peak amplitude was ~0.5 mag.
Asteroid Lightcurve Analysis of Suspected Binary Asteroids
Pages 173-175 Higgins, David; Pravec, Petr; Kusnirak, Peter; Hornoch, Kamil; Pray, Donald P.; Vilagi, Jozef; Kornos, Leonard; Gajdos, Sefan; Husarik, Marek; Pikler, Michal; Cervak, Gabriel 2008MPBu...35..173HDownload PDF
Photometric observations undertaken by collaborating observatories in the BINAST group have uncovered strong evidence of asynchronous binary nature of minor planet 5474 Gingasen and the synchronous binary nature of minor planet 7369 Gavrilin.
Do What You Can Do Photometry: Unfiltered Photometry of NEOs 2005 PJ2, 2005 WC1, and 2006 GY2
The authors made observations of three Near-Earth Objects (NEOs), 2005 PJ2, 2005 WC1 and 2006 GY2, using clear filter photometry and instrumental magnitude relationships to determine preliminary rotation periods. This study demonstrates the potential utility of what is referred to as “do what you can do” photometry.
Asteroids Observed from GMARS and Santana Observatories: Eary 2008
Lightcurve period and amplitude results from Santana and GMARS Observatories are reported for 2008 January to March: 411 Xanthe (11.344 ± 0.002 h and 0.10 mag), 655 Briseis (160.66 ± 0.12 h and 0.40 mag), and (5851) 1991 DM1 (367.52 ± 0.5 h and 0.90 mag).
Asteroid Lightcurve Analysis at the Via Capote Observatory: 2nd Quarter 2008
Lightcurve 2005 NB7 revealed binary characteristics with an orbital period of 15.267 ± 0.094 h with amplitude 0.26 ± 0.05 mag and a primary rotation period of 3.472 ± 0.003 h with amplitude 0.15 ± 0.05 mag. No secondary period was detected indicating tidal lock.
A Study of the Trinary NEA 2001 SN263
Pages 182-184 Betzler, Alberto Silva; Novaes, Alberto Brum; Celedon, Julian Hermogenes Quesada 2008MPBu...35..182BDownload PDF
The trinary NEA, 2001 SN263, was observed by the authors in 2008 February in Salvador, Bahia, Brazil. Based on the data obtained, the synodic period of the primary body was estimated to be 3.20 ± 0.01h with a lightcurve amplitude of 0.27 ± 0.07 mag. The orbital period of the smaller satellite (0.4 Km) was estimated to be 46.1 ± 0.3 h. The NIR spectrum suggests the object is of type C according to DeMeo classification. Lance, a CO3 type meteorite, is the best analogous meteorite.
The synodic rotation period of minor planet 1231 Auricula was found to be 3.9816 ± 0.0006 h. Assuming a near equatorial aspect, the overall amplitude of 0.75 mag implies an axial ratio a/b = 1.99.
Pages 186-189 Warner, Brian D.; Harris, Alan W.; Pravec, Petr; Durech, Josef; Benner, Lance A. M. 2008MPBu...35..186WDownload PDF
We present here four lists of “targets of opportunity” for the period 2008 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 and, in many cases, may not be so for many years. The goal for these asteroids is to find a welldetermined rotation rate. Don’t hesitate to solicit help from other observers at widely spread longitudes should the initial findings show that a single station may not be able to finish the job.
