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.
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 311-312 Bentz, Misty C.; Abbot, Caleb; Agudelo, Steven; Dassing, Steven; Flynn, Wyatt; Gibbs, Austin; Gonzalez, Louis; Kim, Bokyoung; Paredes, Leonardo; Toben, Christopher; Vrijmoet, Eliot Halley; Yep, Alexandra 2018MPBu...45..311BDownload PDF
Broad-band BVR photometry of asteroid 1591 Baize was obtained over four nights in 2017 February and March. We determined a rotation period of 7.788 ± 0.003 hours and typical colors of B-V = 0.9 and V-R = 0.5. The amplitude of color variations is small, ~0.02 mag. These characteristics support the classification of 1591 Baize as an S-type asteroid.
Photometric observations of the Amor class asteroid (138847) 2000 VE62 were performed by the author over five nights from 2018 April 22 to May 10. The rotation period was found to be 7.601 ± 0.001 h with an amplitude of 0.30 ± 0.03 mag.
Photometric Observations of Near-Earth Asteroid 2018 GE3
On 2018 April 14, we observed as a target of opportunity the near-Earth asteroid (NEA) 2018 GE3 from the Astronomical Institute of the Romanian Academy (IAU code 073). Analysis of our data found a synodic period of 0.304 ± 0.001 h based on data obtained over one hour prior to the asteroid’s closest approach to Earth.
Fourier analysis of data taken of asteroid 418 Alemannia determined a rotational period of 4.670 ± 0.006 h with an amplitude of 0.16 ± 0.02 mag. 4911 Rosenzweig’s analysis shows a period of 9.75 ± 0.01 h with an amplitude of 0.08 ± 0.02 mag.
Lightcurve Analysis of Main-belt Asteroid (9899) 1996 EH
We obtained multiple sessions of observations of the main belt asteroid (9899) 1996 EH, using the iTelescope Observatory in Siding Spring, Australia. After analysis, we were unable to determine a conclusive period.
Two Possible Rotation Periods for (86401) 2000 AF143
The minor planet (86401) 2000 AF143 was observed remotely using the T27 telescope located in Siding Spring, Australia. Two aliasing periods are potential rotation periods: 15.0 ± 0.3 h and 30 ± 2 h.
The Rotation Period of 3394 Banno and the Raw Lightcurve of (48697) 1996 HX14
Pages 323 Hayes-Gehrke, Melissa N.; Hannon, Cory; Lockwood, Isaac; Lee, Justin; Moyer, Richard III; Hidayat, Adrian; Moore, Steve; Newman, Michael; Toujas-Bernate, Oliver 2018MPBu...45..323HDownload PDF
Over the course of five nights of observations, we observed asteroid 3394 Banno using iTelescope facilities in New Mexico and Australia. Using the software MPO Canopus, we analyzed and plotted our data to find a rotation period of 7.321 ± 0.025 hours. Additionally, we present raw data for the asteroid (48697) 1996 HX14 found in one night of our observations.
CCD photometric observations of the main-belt asteroid 4221 Picasso ware made at the Studios Observatory over five nights from 2018. The rotation period was found to be 3.111 ± 0.001 h with a lightcurve amplitude of 0.31 ± 0.05 mag.
Lightcurve Analysis of Minor Planets Observed at the Oakley Southern Sky Observatory: 2017 June-July
From 2017 June 20 to July 25, images of nine minor planets were collected to investigate their rotational lightcurve periods. The minor planets observed were 1049 Gotho, 1184 Gaea, 1737 Severny, 1887 Virton, 2672 Pisek, 3995 Sakaino, 6358 Chertok, (13538) 1991 ST, and 14339 Knorre.
Lightcurve Analysis and Rotation Period for (3394) Bano
Photometric data for asteroid 3394 Banno were collected from 2018 April 19-25. The analysis obtained led to a good multiple coverage lightcurve that fit to a period of 7.324 ± 0.002 hours and amplitude of 0.24 mag.
Five Lightcurves from the Shed of Science: 2017 November - 2018 April
CCD observations of five asteroids were made between 2017 November and 2018 April. Analysis of the data found the period and lightcurve amplitudes for 965 Angelica (P = 26.63 ± 0.03 h, A = 0.12 mag), 1266 Tone (P = 15.55 ± 0.03 h, A = 0.19 ± 0.05 mag), 3210 Lupishko (P = 14.255 ± 0.03 h, A = 0.74 ± 0.05 mag), 4435 Holt (P = 2.867 ± 0.002 h, A = 0.18 ± 0.05 mag), and 5133 Phillipadams (P = 6.665 ± 0.005 h, A = 0.43 mag).
A photometric observing campaign conducted in 2018 April and May by Aznar et al. revealed the near-Earth asteroid 15745 Yuliya as a binary system with an orbital period of 15.63 h. Later analysis by Pravec using the dense photometric data obtained in 2018 June by Benishek yielded a different orbital period of 11.735 h, or nearly commensurate with an Earth day.
Lightcurve Analysis of Minor Planets Observed at the Oakley Southern Sky Observatory: 2017 August-September
From 2017 July 26 to September 28, images of 19 minor planets were collected: 820 Adriana, 1326 Losaka, 1594 Danjon, 2021 Poincare, 2164 Lyalya, 2353 Alva, 2558 Viv, 2623 Zech, 3341 Hartmann, 4522 Britastra, (10113) 1992 PX2, 11434 Lohnert, (11889) 1991 AH2, (14892) 1991 VE5, (15549) 2000 FN, (21893) 1999 VL4, (23621) 1996 PA, (30769) 1984 ST2, and (42284) 2001 TV8.
2207 Antenor: A Suspected Jovian Trojan Binary
Pages 341-342 Stephens, Robert D.; Praved, Petr; Kučáková, Hana; Kusnirak; Hornoch, Kamil; Benishek, Vladimire; Aznar Macias, Amadeo; Warner, Brian D. 2018MPBu...45..341SDownload PDF
We report that asteroid 2207 Antenor is a very likely binary asteroid candidate. If confirmed, it would be the fifth known binary Jovian Trojan asteroid. The primary lightcurve has a period of 7.96436 ± 0.00006 h and an amplitude 0.22 to 0.23 mag. A secondary orbital period could not be determined.
Lightcurve Analysis of L5 Trojan Asteroids at the Center for Solar System Studies: 2018 April to May
Lightcurves of four Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2018 April to May. One of the Trojans observed was 617 Patroclus to time the start of mutual events in support of NASA’s Lucy mission.
Lightcurve Analysis for Fourteen Main-belt Minor Planets
Synodic rotation periods and amplitudes are found for 33 Polyhymnia 18.610 ± 0.001 hours, 0.12 ± 0.01 magnitudes; 49 Pales 20.709 ± 0.001 hours, 0.19 ± 0.01 magnitudes with 4 maxima and minima per cycle; 289 Nenetta 6.916 ± 0.001 hours, 0.20 ± 0.02 magnitudes; 504 Cora 7.587 ± 0.001 hours, 0.18 ± 0.01 magnitudes; 821 Fanny, 235 ± 1 hour, amplitude increasing from 0.22 to 0.28 magnitudes. For 821 Fanny the color index V-R = 0.37, H = 11.763 ± 0.018, G = 0.079 ± 0.018.
(139345) 2001 KA67: A Potential NEA Very-wide Binary Asteroid
Analysis of CCD photometric observations of the near- Earth asteroid (139345) 2001 KA67 show that it may be a very wide asynchronous binary, which features a long primary and short secondary period. The two periods that were found for 2001 KA67, P1 = 44.25 ± 0.05 h and P2 = 6.011 ± 0.003 h, are in-line with other potential members of this class.
Lightcurve Analysis of Main-belt Asteroids from BMO and DRO in 2016: I
Photometric observations of selected asteroids were done from Blue Mountains Observatory (BMO) and Darling Range Observatory (DRO) in 2016. The observations were made during a favorable apparition for each asteroid as part of the Photometric Survey of Asynchronous Binary Asteroids (PSABA) program.
Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2018 April-June
Lightcurves for 39 Near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2018 April-June were analyzed for rotation period and signs of satellites or tumbling. In addition, re-examination of data for 2014 UR taken in 2014 shows that the rotation period is 0.2300 h and not the 2.37 h that was originally reported.
Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2018 April-June
CCD photometric observations of seven asteroids were conducted from 2018 January through June. A review of the results obtained for synodic rotation periods as well as the lightcurves established is presented here.
Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2018 April-June
Lightcurves for seven Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2018 April-June: 1180 Rita, 1748 Mauderli, 1877 Marsden, (13035) 1989 UA6, (42237) 2001 EG21, and (60381) 2000 AX180. The previously reported period (Warner and Stephens, 2017) for 1180 Rita was revised following analysis of the 2018 data.
CCD photometric observations were made of the Hungaria asteroid 2491 Tvashtri from 2018 Mar 29. April 27. Analysis of the data determined that the asteroid is binary with periods of P1 = 4.0852 h and Porb = 26.712 h. The estimated ratio of effective diameters is DS/DP >= 0.24.
Three Asteroids from Etscorn: 461 Saskia, 3800 Karayusuf and (42701) 1998 MD13
In the second quarter of 2018 we obtained lightcurves for three asteroids. 461 Saskia, 3800 Karayusuf and (42701) 1998 MD13. 461 Saskia and 3800 Karayusuf are spin-shape candidates and (42701) 1998 MD13 is a first time observation for a lightcurve determination.
Lightcurves for 91 Aegina, 235 Carolina, 1117 Reginita, and (505657) 2014 SR339
Photometric observations of three main-belt and one near-Earth asteroids were made in order to acquire lightcurves for shape/spin axis models. For 91 Aegina, the synodic rotation period is 6.029 ± 0.001 h, amplitude 0.19 mag. For 235 Carolina, the synodic rotation period is 17.61 ± 0.01 h, amplitude 0.31 mag. For 1117 Reginita, the synodic rotation period is 2.9467 ± 0.0001 h, amplitude 0.19 mag. For (505657) 2014 SR339, the synodic rotation period is 8.71 ± 0.01 h, amplitude 0.75 mag.
Lightcurve Analysis of Asteroids 2040 Chalonge, 4575 Broman and 5852 Nanette
Photometric observations of asteroids 2040 Chalonge 4575 Broman, and 5852 Nanette were made at the Philips Academy Observatory from 2018 March through 2018 June. 2040 Chalonge was found to have rotational period of 10.367 ± 0.001 h with amplitude 0.12 mag, consistent with the previously reported period; 4575 Broman was found to have a rotational period of 10.774 ± 0.001 h with an amplitude of 0.59 mag; 5852 Nanette was found to have a rotational period of 5.606 ± 0.001 h with an amplitude of 0.49 mag.
Lightcurve for 3800 Karayusuf
Pages 403 Franco, Lorenzo; Bacci, Paolo; Maestripieri, Martina; Carotta, Giulio; Carotta, Marco; Nesti, Linda; Fragai, Martina 2018MPBu...45..403FDownload PDF
Photometric observations of Mars-crosser 3800 Karayusuf were made in May 2018. Lightcurve analysis shows a synodic rotation period P = 2.2318 ± 0.0002 hours with an amplitude 0.17 magnitudes.
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 or might be radar targets. 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.