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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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.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 photometric analysis of two asteroids observed at the Carl Sagan Observatory (OCS in Spanish) of the Universidad de Sonora in Hermosillo, Sonora, México. For 2070 Humason, our derived intrinsic rotation period is P = 3.18851 ± 0.00032 h and A = 0.14 mag. For 3122 Florence, our derived intrinsic rotation period is P = 2.3589 ± 0.0005 h and A = 0.24 mag. In both cases, we found good agreement with previously reported values.
Lightcurve-Based Period Determination for Apollo PHA (162082) 1998 HL1
Asteroid (162082) 1998 HL1 was observed during October 2019 at the Observatorio Estelar Carl Sagan from the Universidad de Sonora. Photometric data were collected during two nights that showed a period P = 7.587 ± 0.006 h and amplitude of A= 0.11 ± 0.03 mags.
Rotation Period and Amplitude Determination of (18172) 2000 Ql7: A Fast Rotator
Photometric observations of (18172) 2000 QL7, a fast rotator Amor/Mars-crosser asteroid, were made over three consecutive nights: 2019 October 29 through November 1. A synodic rotation period of 2.3767 ± 0.0005 h and lightcurve amplitude of 0.11 ± 0.01 mag were determined. The result significantly differs from the one published by Warner and Stephens (2020). Additional observations were made in January 2020. Initial results have been examined and confirmed.
Photometric Observations of Twenty-Three Minor Planets
Phased lightcurves and synodic rotation periods for 23 main-belt asteroids are presented, based on CCD observations made from 2019 September through 2019 November. All the data have been submitted to the ALCDEF database.
Lightcurve Analysis of Long-period Minor Planet 2580 Smilevskia
2580 Smilevskia is a main-belt asteroid with no prior rotational period determinations. Data were acquired from two observatories spanning five weeks near a perihelic opposition. A synodic rotation period of 658.4 ± 1.2 h was computed. Data have been submitted to the ALCDEF database.
The authors report on the results of photometric observations of near-Earth asteroid (NEA) 2019 GT3. The most probable synodic rotation period is 0.73 ± 0.03 h with an amplitude of 1.3 ± 0.2 mag. The body appears to be rather elongated with a lower limit a/b . 1.4 ± 0.3 (if S-type) and strength-bound.
Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2019 September - 2020 January
Lightcurves for 33 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2019 September to early 2020 January were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling. Some objects are good candidates for being members of the class of very wide binary asteroids. Others show signs of being “ordinary” binary asteroids, while others proved to be difficult to categorize as one or the other or if their behavior was due to tumbling. There were few easy answers.
We present a shape and spin axis model for main-belt asteroid 33 Polyhymnia. The model was achieved with the lightcurve inversion process, using combined dense photometric data acquired from five apparitions, between 2008-2019 and sparse data from USNO Flagstaff. Analysis of the resulting data found a sidereal period P = 18.60888 ± 0.00029 hours and two mirrored pole solutions at (λ = 19°, β = -65°) and (λ = 185°, β = -61°) with an uncertainty of ± 15 degrees.
Observers who have made visual, photographic, or CCD measurements of positions of minor planets in calendar year 2019 are encouraged to report them to this author on or before 2020 April 1. This will be the deadline for receipt of reports, for which results can be included in the "General Report of Position Observations for 2019," to be published in MPB Vol. 47, No. 3.
Lightcurve Analysis Of Hilda Asteroids At The Center for Solar System Studies: 2019 November
Photometric observations of a selection of Near-Earth Asteroids were done from Blue Mountains Observatory (BMO), JBL Observatory (JBL). The observations were made during the favorable apparition for each asteroid. Most of these objects were selected from The Asteroid Lightcurve Database and the data was collected using multiple instruments across Australia.
Rotation Period Determination for Asteroid 8323 Krimigis
Minor planet 2000 Herschel is tumbling with a principal period of 133.6 h. A secondary period of 344 h is suggested, although other secondary periods are possible. The maximum amplitude is 1.1 magnitudes.
Collaborative Asteroid Photometry from UAI: 2019 October-December
CCD photometric observations of seven main-belt asteroids were made from 2019 CCD photometric observations of seven main-belt asteroids were made from 2019 October-December. We report on the results of lightcurve analysis for 2634 James Bradley, 3171 Wangshoguang, 3662 Dezhnev, 3819 Robinson, 4686 Maisica, (7397) 1986 QS, and (51149) 2000 HF52.
The Rotation Rates of Three Near-Earth Asteroids and a Mars-Crossing Asteroid
Photometric observations of three near-Earth asteroids (NEAs) and a Mars-crossing asteroid (MCA) were performed during 2017 October 18 to October 22. Fourier analysis of the four targets yielded rotation periods of: 3.494 ± 0.034 h for 3361 Orpheus, 6.653 ± 0.008 h for 1990 UQ, 5.491 ± 0.003 h for 1999 RT198 and 5.319 ± 0.002 h for 1998 ST4.
Photometry of 2729 Urumqi at the Xingming Observatory in Urumqi City
Lightcurve photometry observations of the main-belt asteroid 2729 Urumqi were made at Xingming Observatory in 2019 December. We find that the asteroid has a synodic rotation period of 3.127 ± 0.001 h and amplitude of 0.22 ± 0.01 mag. Multi-band photometric sessions shows the mean color indices of gr = 0.67 ± 0.02, and r-i = 0.20 ± 0.02 mag. According to these color indices, 2729 Urumqi can be classified as a type S asteroid.
The Rotation Periods of the Asteroids 587 Hypsipyle, 1152 Pawona, and 2937 Gibbs
We present photometric synodic rotation periods for the asteroids 2937 Gibbs (P=2.983 ± 0.001 h and a possible P2=5.626 ± 0.001 h), 1152 Pawona (P=3.4151 ± 0.0003 h), and 587 Hypsipyle (P=2.8881 ± 0.0005 h).
Rotational Periods and Lightcurves of 2051 Chang, 3171 Wangshouguan, 8141 Nikolaev, and 10426 Charlierouse
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.
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.