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.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
OpenOffice and convert their files to
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.
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.
Composite Lightcurves of Three Main-Belt Asteroids
Pages 97-99 Castro, Eduardo; Wilkin, Francis P.
We present composite lightcurves of Koronis family asteroids (2092) Sumiana and (2953) Vysheslavia, and serendipitous observations of main-belt asteroid (2705) Wu. The lightcurve of Sumiana was assembled from seven nights of observations and its period and amplitude are 30.523 ± 0.014 h and 0.38 ± 0.04 mag respectively. Our observations of Vysheslavia and Wu are consistent with previously reported periods.
Lightcurve Analysis and Rotation Period for NEA 2006 WB
Pages 100 Nobre, Geovandro
Analysis of lightcurve observations of NEA 2006 WB during its closest approach to Earth in 2024 yields a synodic rotation period solution of 8.53 ± 0.29 h. Even though this period is compatible with the value found by the Arecibo telescope in 2006, the data set allowed for many other periods with similar RMS values in the Fourier analysis. Thus the 8.53 h period solution must be considered ambiguous and inconclusive.
Lightcurve Analysis and Rotation Period for PHA 2020 XR
Pages 101 Nobre, Geovandro
Lightcurve observations of the potentially hazardous asteroid (PHA) 2020 XR during its closest approach to Earth in 2024 yielded a synodic rotation period of 10.70 ± 0.04 h. This result should not be considered secure given a large number of other periods of similar RMS fit found by the Fourier analysis.
Lightcurve and Rotation Period of 2266 Tchaikovsky
Pages 102 Wang, Luyi
Twelve sets of photometric observations of the main-belt asteroid 2266 Tchaikovsky were obtained from 2024 December 10th to 2025 January 12th. Using Tycho Tracker software, we plotted the lightcurve of 2266 Tchaikovsky and measured its rotation period to be 37.8330 ± 0.0126 h with a lightcurve amplitude of 0.252 mag., in agreement with its tabulated value.
Lightcurve and Rotation Period of the Slow Rotator 6176 Horrigan
Pages 103 Noschese, Alfonso; Vecchione, Antonio; D’Avino, Luca; Di Dato, Andrea
Based on preliminary lightcurve measurements of 6176 Horrigan in September 2024, a long period seemed evident. Consequently, an additional two months of observations were devoted to this object. Analysis of the additional collected data has produced a lightcurve with a period of 670.36 ± 1.12 hours and an amplitude of 0.874 magnitudes.
The Ambiguous Rotation Period of 1269 Rollandia Is Solved By a Global Collaboration Of Observers
A global collaboration of photometric observers has found for 1269 rotational parameters: synodic period 59.70 ± 0.01 hours with an unsymmetric bimodal lightcurve and amplitude 0.09 ± 0.01 hours.
A collaboration of observers from Europe and North America have found for 1237 Genevieve a synodic rotation period of 24.711 ± 0.002 hours and amplitude 0.14 ± 0.01 magnitudes.
Lightcurves and Rotation Periods of 691 Lehigh, 795 Fini, and 1302 Werra
Pages 106-107 Pilcher, Frederick
Synodic rotation periods and amplitudes are found for 691 Lehigh 12.899 ± 0.001 hours, 0.13 ± 0.02 magnitudes with an irregular trimodal lightcurve; 795 Fini 51.71 ± 0.01 hours, 0.06 ± 0.01 magnitudes.; and 1302 Werra 13.957 ± 0.002 hours, 0.15 ± 0.02 magnitudes with an irregular trimodal lightcurve.
Photometric Observations and Analysis of Six Main-Belt Asteroids
Pages 108-111 Bucek, Marek; Galdies, Charles; Brincat, Stephen M.; Mifsud, Martin
We report the results of our photometric observations and lightcurve analysis of six main-belt asteroids: 3423 Slouka, 4367 Meech, (7878) 1992 DZ, 9628 Sendaiotsuna, (14127) 1998 QA91, and 17851 Kaler. The asteroids were observed by a network of four observatories located in Malta and Slovakia.
Photometric Observations and Lightcurve Analysis of (25450) 1999 XQ7
Pages 111-112 Bucek, Marek; Brincat, Stephen M.; Rivard, Normand
In this paper we report the results of our photometric observation campaign and lightcurve analysis of an asteroid (25450) 1999 XQ7 during its favorable opposition in 2024.
Photometric observations of three main-belt asteroids were conducted to determine their synodic rotation periods. We found: for 1626 Sadeya, P = 3.421 ± 0.002 h with A = 0.11 ± 0.01 mag; for 5552 Studnicka, P = 5.912 ± 0.001 h with A = 0.12 ± 0.02 mag; for 5565 Ukyounodaibu, P = 5.752 ± 0.001 h with A = 0.20 ± 0.03 mag.
Lightcurves of 40 Asteroids
Pages 115-125 Stone, Geoffrey
We present lightcurves and synodic rotation periods for 40 asteroids based on observations obtained at the Dimension Point Observatory (V42) from September 2024 through January 2025.
Lightcurves of Eighteen Asteroids
Pages 125-133 Dose, Eric V.
We present lightcurves and synodic rotation periods for eighteen asteroids including the family parent asteroid (2732) Witt.
Lightcurve and Rotation Period Analysis for Twenty-Five Minor Planets
Pages 134-140 Wiles, Mike
Photometric measurements of CCD observations on twenty-five minor planets were made from 2024 April through 2025 January. Phased lightcurves were created for each one. All data has been submitted to the ALCDEF database.
A Lightcurve Analysis for Nine Main-Belt and One Mars-Crossing Asteroids
Pages 141-145 Huet, Fernando; Fornas, Gonzalo; Fornas, Alvaro
Photometric observations of nine main-belt and one Mars-crossing asteroids were obtained from 2024 February 4 to October 10. We derived synodic rotational periods for 728 Leonisis, 1698 Christophe, 1802 Zhang Heng, 2741 Valdivia, 3583 Burdett, 3895 Earhart, (12543) 1998 QM5, (20490) 1999 OW2, (31545) 1999 DN6, and (32575) 2001 QY78. Sidereal rotation periods were found 728 Leonisis, 1802 Zhang Heng, 2741 Valdivia, and 3895 Earhart.
Collaborative Asteroid Photometry from UAI: 2024 October-December
Photometric observations of four asteroids were made in order to acquire lightcurves for shape/spin axis modeling. Lightcurves were acquired for 1808 Bellerophon, 3672 Stevedberg, (36183) 1999 TX16, and (154589) 2003 MX2.
Photometry of NEAs (187026) 2005 EK70 and (152787) 1999 TB10
Pages 148-150 Hutton, Lucas J.; Fieber-Beyer, Sherry; Linder, Tyler R.; Reichart, Daniel E.; Haislip, Joshua B.; Kouprianov, Vladimir V.; Moore, Justin P.
Near-Earth asteroids (187026) 2005 EK70 and (152787) 1999 TB10 were observed over five nights in February 2024 and four nights in March 2024, respectively, using the Prompt 3 telescope at the Cerro Tololo Inter- American Observatory. The rotational period for (187026) 2005 EK70 is 6.966 ± 0.001 hours and the lightcurve amplitude is 0.20 ± 0.02 magnitude. The rotational period for (152787) 1999 is 2.876 ± 0.001 hours and the amplitude is 0.29 ± 0.05 magnitude. A search of the Asteroid Lightcurve Database provided no previously published results for either NEA.
Lightcurves of Near-Earth Asteroids 2024 ON, 2024 MK and 1998 ST27 As Observed From Trappist
We report photometric observations of three near-Earth asteroids: 2024 ON, 2024 MK, and 1998 ST27. The observations were performed between June and October 2024 during their close approaches to Earth using the TRAPPIST network. Applying lightcurve analysis, we determined that the rotation period and amplitude of 2024 ON are P = 6.0116 ± 0.0003 h and A = 0.94 ± 0.05 mag. For 2024 MK we found two possible rotation periods. In the first case P1 = 0.5028 ± 0.0001 h with A1= 0.67 mag ± 0.02, and P2 = 0.3663 ± 0.0001 h with A2 = 0.45 mag ± 0.02. In the second case P1 = 0.7301 ± 0.0011 h with A1 = 0.503 mag, and P2 = 0.5031 ± 0.0005 h with A2 = 0.643 mag. For 1998 ST27 we obtain P = 3.56 ± 0.02 h and A= 0.07 ± 0.01 mag. All measurements have been submitted to the ALCDEF database.
Lightcurve Analysis for Six Near-Earth Asteroids Observed in 2009 and October - December 2024
Pages 153-158 Birtwhistle, Peter
Lightcurves and amplitudes for six near-Earth asteroids observed from Great Shefford Observatory during close approaches in June 2009 and October to December 2024 are reported. All are small objects with rotation periods 1 hour or shorter and four are identified as having tumbling rotation.
Ligthcurves and Colors of Five Small Near-Earth Asteroids: 2024 SY6, 2024 TU, 2024 TK1, 2024 TX13, 2024 UF9
Pages 158-163 Kikwaya Eluo, Jean-Baptiste; Hergenrother, Carl W.
September 2024 and October 2024 observation campaigns resulted in photometric observations of five small near-Earth asteroids. Lightcurves of three asteroids (2024 SY6, 2024 TU, and 2024 TK1) clearly indicated rapid rotation, and those of two others (2024 TX13, and 2024 UF9) remained inconclusive. Color indices of all five asteroids were computed and were used to produce two-color plots to determine the taxonomy class of each of them, and in addition to compute their relative reflectance, which was compared to asteroid spectra (from SMASS and SMASSII) to refine the primary taxonomy classification.
A Lightcurve Analysis for Nine Main-Belt and One Mars-Crossing Asteroids
Two mutual events were observed for 617 Patroclus- Menoetius synchronous binary system in 2024 October in order to contribute to refine the physical parameters of the system, in view of the NASA’s Lucy fly-by mission, expected in year 2033.
Lightcurves from Three Mutual Events of Trojan Binary 617 Patroclus in October 2024
We present three raw lightcurves of Trojan binary 617 Patroclus on 2024 October 2, 6, and 21 during mutual events of the binary system.
Follow-Up Observations of 617 Patroclus-Menoetius Mutual Events: 2024 November to 2025 January
Pages 178-183 Warner, Brian D.; Durkee, Russ; Fauerbach, Michael; Gebauer, John; Cloutier, William; Nastasi, Alessandro; Oey, Julian; Sioulas, Nick; Stephens, Robert D.; Tedesco, Daniel Guimaraes; de Oliveira Barreto, Carlos Henrique
We report on additional observations made and analysis following (Warner et al., 2025), continuing the effort to provide data prior to for NASA’s Lucy fly-by mission in 2033 March. The additional data led to the same period, 102.873 h, but the formal precision was reduced by half to 0.003 h. Data for 2024 October 10-11 received after submission of our previous work filled in the missing part of the event, and we were able to refine the date and time for the start and minimum of the event. Other observations in late 2024 October through 2025 January 11 were either outside an event or covered only part of one. As before, we offer no interpretation regarding the parameters of the system beyond the rotation/orbital period. We also report H-G values of HPR = 8.032 ± 0.042, GPR = 0.075 ± 0.066. The value for HPR was converted to H = 0.82 ± 0.06. The MPC reports H = 8.25 using G = 0.15.
Pages 184-187 Warner, Brian D.; Harris, Alan W.; Durech, Josef; Benner, Lance A.M.
We present lists of asteroid photometry opportunities for 2025 April-July. The extended four-month listing continues the changes announced in MPB 51-4 (Warner et al., 2024). Extending to the month beyond the usual quarter-year allows better observation planning, especially for those working in wide-spread collaborations. With the massive input of survey photometry, even if mostly sparse data, the small telescope researcher’s role is moving away generic studies to those concentrating on specific needs and targets and so, we hope, leading to even more fulfilling and fruitful efforts.
In This Issue
Pages 188 Warner, Brian D.
This list gives those asteroids in this issue for which physical observations (excluding astrometric only) were made. This includes lightcurves, color index, and H-G determinations, etc. In some cases, no specific results are reported due to a lack of or poor quality data. The page number is for the first page of the paper mentioning the asteroid. EP is the "go to page" value in the electronic version.
