The Minor Planet Bulletin BULLETIN OF THE MINOR PLANETS SECTION OF THE ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS
Click on image to zoom
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
UMD Astronomy Department
1113 PSC Bldg 415
College Park, MD 20742
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.
Important: If the ADS bibcode and "Download PDF" links are missing for the latest issue, it is because the ADS has
not processed the files. The links will be made available after the ADS processes the files.
If the "Download PDF" link is visible and there is no PDF available, clicking the link will download an arbitrary
page. We are working with ADS to make sure all papers are available and, if not, being able to diasable the link.
The "Download Full Issue" link does retrieve the correct file.
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 235-237 Garceràn, Alfonso Carreño; Macias, Amadeo Aznar; Mansego, Enrique Arce; Rodriguez, Pedro Brines; de Harro, Juan Lozano 2015MPBu...42..235GDownload PDF
Photometric observations of six asteroids were made from 2015 March to May. We report the results of our lightcurve analysis for 425 Cornelia, 625 Xenia, 664 Judith, 785 Bredichina, 910 Anneliese, and 1831 Nicholson.
Finding the Lightcurve and Rotation Period of Minor Planet 13003 Dickbeasley
The lightcurve of 13003 Dickbeasley was determined using five nights of data from 2015 April and May, from which we found its rotation period to be 3.502 ± 0.0005 hrs. Images were taken at the Phillips Academy Observatory.
These are the first photometric observations ever reported for 2020 Ukko. We find a rotational amplitude of 0.24 ± 0.02 magnitudes and prefer a period of 25.478 ± 0.002 hours with a symmetric bimodal lightcurve. However, periods of 12.733 ± 0.001 hours with a monomodal lightcurve and 38.154 ± 0.002 hours with a trimodal lightcurve fit the data almost as well.
Rotation Period Determination for 318 Magdalena and 335 Roberta
Lightcurve analysis using MPO Canopus from two nights of observation of 1238 Predappia found a possible rotation period of 6.13 ± 0.04 h and lightcurve amplitude of 0.05 mag. Low lightcurve amplitude and period spectrum analysis did not provide enough evidence to confirm this rotation period. There are three possible conclusions to gather from these data: Predappia may have a nearly spherical shape, long rotation period, or pole-on orientation during the observation period.
Target Asteroids! Observing Campaigns for 2015 October through December
Asteroid campaigns to be conducted by the Target Asteroids! program during the 2015 October-December quarter are described. In addition to asteroids on the original Target Asteroids! list of easily accessible spacecraft targets, an effort has been made to identify other asteroids that are 1) brighter and easier to observe for small telescope users and 2) analogous to 101955 Bennu and (162173) 1999 JU3, targets of the OSIRISREx and Hayabusa-2 sample return missions.
Rotation Period Determination for Asteroid (16813) 1997 UT6
Photometric observations of main-belt asteroid (16813) 1997 UT6 were made over two nights during 2015 March and April. Observations were obtained remotely at iTelescope Observatory H06 in Mayhill, New Mexico. Analysis of the CCD data found several possible periods. The most likely period is 8.2934 ± 0.0035 h with an alternate period of 7.88 ± 0.003 h.
A lightcurve was determined for the main-belt asteroid 5181 SURF. The asteroid was observed for seven nights over the course of two months during 2015 March-April. The rotation period was found to be 6.111 ± 0.001 h.
Photometric observations of the main-belt asteroid 107 Camilla were made from 2015 May to June. Our analysis found a synodic period of 4.845 ± 0.005 h and lightcurve amplitude of 0.33 mag.
3841 Dicicco: A Binary Asteroid
Pages 249-250 Klinglesmith, Daniel A. III; Franco, Lorenzo; Odden, Carolyn E.; Pravec, Petr; Scardella, Maurizio; Tomassini, Angelo 2015MPBu...42..249KDownload PDF
Initial observations of 3841 Dicicco indicated a period of 3.6 hours with three nights being anomalously low over part of the period. Further analysis showed that 3841 is a binary asteroid with a primary period of 3.5950 ± 0.0001 h with an amplitude of 0.19 mag and a secondary period of 21.641 ± 0.002 h with an amplitude of 0.19 mag. Both the primary eclipse and secondary eclipses were visible. We also estimate the H and G parameters to be H = 13.63 ± 0.04, G = 0.15 ± 0.05.
Asteroids Observed at Etscorn Observatory: 2015 April - June
We observed four main-belt asteroids and obtained periods and amplitudes: 3366 Godel, P = 4.684 ± 0.002 h, A = 0.20 mag; 5438 Saurez, P = 2.941 ± 0.001 h, A = 0.20 mag; 8474 Rettig, P = 11.514 ± 0.024 h, A = 0.91 mag; and 15224 Penttila, P = 4.377 ± 0.001 h, A = 0.51 mag.
Rotation Period and H-G Parameters Determination for 910 Anneliese
Lightcurve analysis for 910 Anneliese was performed using observations during its 2015 opposition. The synodic rotation period was found to be 11.2863 ± 0.0002 h and the lightcurve amplitude was 0.16 ± 0.02 mag; the absolute magnitude was HR = 9.974 ± 0.028 mag and the slope parameter was G = 0.107 ± 0.030. These lead to an estimated diameter of 46.3 ± 3.5 km.
Lightcurve Analysis of the Near-Earth Asteroid (6053) 1993 BW3
CCD photometric observations of the near-Earth asteroid (6053) 1993 BW3 were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2015 January and March. Analysis of the individual and combined data sets produced a period on the order of 2.8 hours. This differs significantly from the results of Pravec et al. (1997; P = 2.573 h) and from shape models by Durech (2002) and Kaasalainen (2002). While this discordance is not resolved, the 2.573 h value has the greatest amount of data supporting it, and for now, remains the favored period solution.
Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2015 March-June
Lightcurves for 29 main-belt asteroids were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2015 March-June. All but three were members of the Hungaria orbital group or collisional family and observed as part of an ongoing program to obtain data for spin axis and shape modeling. One Hungaria, (79472) 1998 AX4 showed signs of having a satellite. Analysis indicates it is a possible binary.
Two near-Earth asteroids (NEAs) were observed from Cerro Tololo Inter-American Observatory in May and June 2015. 2014 YB35 was found to have a synodic rotation period of 3.277 h with an amplitude of 0.16 mag. (68216) 2001 CV26 has a well-established rotational period of 2.429 h and displayed some weak evidence of mutual events.
Photometric observations of the main-belt asteroid 2641 Lipschutz performed by the authors from Italy in 2015 April revealed a bimodal lightcurve phased to 21.62 ± 0.03 hours as the most likely solution resulting from the synodic rotation rate for the asteroid.
Asteroids Observed from CS3: Results for 1754 Cunningham and 7023 Heiankyo
CCD photometric observations of 1754 Cunningham, and 7023 Heiankyo were obtained from the Center for Solar System Studies from 2015 June to July. For 1754, the period of 7.7416 ± 0.0005 hours appears to be about twice the previously reported value. For 7023, our solution of 10.807 ± 0.002 hours matches one previously noted possible solution.
Rotation Period Determination for 134 Sophrosyne, 521 Brixia, and 873 Mechthild
Analysis of photometric observations of two main-belt asteroids were performed by the authors in Italy from 2015 April to June. Assuming bimodal lightcurves, the synodic periods were: 4149 Harrison, P = 3.956 ± 0.001 h and (5633) 1978 UL7 P = 7.212 ± 0.001 h.
Lightcurve and Rotation Period Determination for 1492 Oppolzer and (9773) 1993 MG1
Photometric observations of the main-belt asteroids 1492 Oppolzer and (9773) 1993 MG1 were performed by the authors in 2015 April-July. Analysis of the data revealed bimodal lightcurves for each object. For 1492 Oppolzer, we found a synodic period of P = 3.770 ± 0.001 h; for (9773) 1993 MG1, we found P = 2.746 ± 0.001 h.
The minor planet 2296 Kugultinov was observed on 13 nights between 2015 March 13 and April 21. The analysis yielded a synodic period of rotation of P = 16.850 ± 0.004 h and amplitude of A = 0.23 mag. This result is in disagreement with a previously reported period of P = 10.41 h.
We present lists of asteroid photometry opportunities for objects reaching a favorable apparition and having either none 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.
Photometric data were collected over the course of three nights in 2015 March and April for asteroid 6518 Vernon. A rotation period of 4.911 ± 0.001 hours was determined with an amplitude of 0.52 magnitudes.