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.
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Authors Guide and Word Templates
(v.3.0: updated 2024 February 2)
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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.
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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)..."
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From 2016 to 2017, images of minor planets were collected to investigate their rotational lightcurve periods. Those minor planets were 3361 Orpheus, 3749 Balam, (66391) 1999 KW4, (153415) 2001 QP153, (357027) 1999 YR14, (496018) 2008 NU, and 2014 YC15.
Lightcurves and Rotational Periods of Five Main-belt Asteroids
Lightcurves measurements are reported for five asteroids: 727 Nipponia, 857 Glasenappia, 1551 Argelander, 1676 Kariba, and 2556 Louise. Respectively their rotational periods are found to be 5.070 \± 0.001 h, 8.188 ± 0.006 h, 2.314 ± 0.012 h, 3.168 ± 0.002 h, 3.809 ± 0.001 h.
Fourier analysis of CCD-based photometric data has led to the determination of synodic periods for the asteroids 216 Kleopatra (5.386 h), 218 Bianca (6.339 h), 276 Adelheid (6.320 h), 694 Ekard (5.922 h), 1224 Fantasia (4.995 h), and 1627 Ivar (4.796 h)
Pattern of Minor Planet Numbers Versus Cumulative Number Observed
The author finds that as the cumulative number of minor planets that are visually observed increases, several effects are noticed. The author examines the pattern of assigned minor planet numbers observed versus the total number of distinct objects seen.
Lightcurve Analysis of Asteroids from BMO and DRO in 2016. II.
Photometric observations of selected asteroids were done from Blue Mountains Observatory (BMO), Perth Observatory (PO), and Darling Range Observatory (DRO) in 2016. The observations were made during a favorable apparition for each asteroid. Most of these objects were selected from a list of targets that matches the criteria for binary asteroids.
The inner main-belt asteroid (3677) Magnusson has been observed over several nights in the late 2018 summer in order to determine its synodic rotation period and amplitude. Lightcurve analysis shows a synodic period P = 7.90 ± 0.01 h with an amplitude A = 0.89 mag.
Lightcurve Analysis of Minor Planets Observed at the Oakley Southern Sky Observatory: 2018 January-March
Beginning 16 January 2018 and continuing through 17 March 2018 a total of seventeen minor planets were target for observation from the Oakley Southern Sky Observatory. Images were taken of 936 Kunigunde, 1281 Jeanne, 1644 Rafita, 1905 Ambartsumian, 2079 Jacchia, 2279 Barto, 2396 Kochi, 2463 Sterpin, 2677 Joan, 2764 Moeller, 3470 Yaronika, 3706 Sinnott, 4181 Kivi, 4628 Laplace, 5079 Brubeck, 7186 Tomioka, and (29934) 1999 JL46.
New Lightcurves of 153 Hilda, 293 Brasillia, and 318 Magdalena
Photometric observations of four main-belt asteroids were obtained on the nights of 2018 November 1 and 3 using the SARA-North telescope at Kitt Peak National Observatory. We derived the following rotational periods: 755 Quintilla 4.552 ± 0.002 h; 1830 Pogson 2.570 ± 0.001 h; 5076 Lebedev-Kulmach 3.215 ± 0.003 h; and (29153) 1988 SY2 3.492 ± 0.002 h.
A New Lightcurve and Spin-Shape Model for 46 Hestia
At its opposition in late 2018, minor planet 46 Hestia has a synodic rotation period of 21.039 ± 0.001 h and amplitude 0.11 ± 0.01 mag. A lightcurve inversion model based on four dense data sets in the years 1978- 2018 plus sparse observations provides a sidereal period of 21.04010 ± 0.000035 h with two mirrored pole solutions at longitude 291 deg, latitude +13 deg; or longitude 110 deg, latitude 7 deg; all ± 5 degrees, respectively. A shape model is also provided.
Photometric observations of 3951 Zichichi were made in order to acquire a lightcurve for shape/spin axis modeling. The synodic rotation period is 3.39 ± 0.01 h and the amplitude is 0.27 mag. Results are consistent with previously reported values.
Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2018 September-December
Lightcurves for 32 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2018 September-December were analyzed for rotation period and signs of satellites or tumbling.
Lightcurve analysis of the near-Earth asteroids (442742) 2012 WP3, (523604) 2004 QB17, and 2018 RL indicate that they are potential members of a relatively rare class of “very wide binary asteroids.” These objects feature a primary rotational period of tens to hundreds of hours and a secondary rotational period less than 24 hours, usually less than 10 hours. These three bring to 30 the number of suspected members of the class.
CCD photometric observations at the Center for Solar System Studies (CS3) were made of the near-Earth asteroid (12538) 1998 OH in 2018 November. The goal was to find a secure period and so resolve ambiguous solutions from previous years. Final analysis of the 2018 data found that it is anything but ordinary. One possibility is that it is a low-amplitude, fast-rotating tumbler. The other, more exotic, possibility is that it may be an asteroid pair in the making, i.e., the two fast-rotating components have not yet broken their mutual bond. Future observations may show that one of these, or yet another solution, correctly describes the asteroid.
Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2018 September-December
Lightcurves for four Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2018 September-November: 3514 Hooke, 3557 Sokolsky, 4495 Dassanowksy, and 10331 Peterbluhm. 4495 Dassanowksy appears to be a binary asteroid with a primary period of either 2.6314 hr or 5.263 hr and an orbital period of 18.516 hr. The secondary-to-primary ratio of the effective diameters is 0.26 ± 0.02.
(20882) 2000 VH57: An Inner Main-belt Binary Asteroid
Pages 164-165 Warner, Brian D.; Aznar Macias, Amadeo; Serra-Ricart, M.; Licandro, J.; Pravec, Petr 2019MPBu...46..164WDownload PDF
CCD photometric observations of the inner main-belt asteroid (20882) 2000 VH57 were made from 2018 Sept. 15 through Oct. 20. Analysis of the data showed that the asteroid is binary with a primary rotational period of 2.5586 hr and a satellite orbital period of 32.81 hr. Mutual eclipse/occultation events indicate a lower limit on the secondary-to-primary mean diameter ratio (Ds/Dp) of 0.23. During the period of observations, the primary and secondary lightcurves evolved as the viewing aspect changed. In particular, the depth of the secondary event increased significantly towards the end of the observations.
Lightcurve Analysis of Asteroids Observed by KMTNET-SAAO
Observations from the South Africa node of the Korea Microlensing Telescope Network (KMTNe-SAAO) were analyzed using the open source Photometry Pipeline (PP). PP can identify serendipitously observed asteroids in the observation fields which led to the extraction of 53 asteroid lightcurves. Rotational periods for 49 of these targets could be determined and are presented here.
Observers who have made visual, photographic, or CCD measurements of positions of minor planets in calendar year 2018 are encouraged to report them to this author on or before 2019 April 1.
Main-belt Asteroids Observed from CS3: 2018 October - December
CCD photometric observations of 18 main-belt asteroids were obtained from the Center for Solar System Studies from 2018 October to December. A pole solution was found for 4910 Kawasato of (λ, β, PSID) = (355°, 35°, 4.66271 h). (31320) 1998 HX2 is a binary asteroid with a P1 of 2.8149 ± 0.0001 h and P2 of 47.06 ± 0.05 h.
Photometric observations of near-Earth asteroid 2018 RC were made in September 2018, few days after its discovery. Lightcurve analysis shows a tumbling nature with a principal rotational period of 0.16548 ± 0.00001 h with an amplitude 0.57 mag and a secondary rotational period 0.26201 ± 0.00001 h with an amplitude 0.20 mag. Multi-band photometric sessions shows color indexes VR = 0.48 ± 0.07 mag and R-I = 0.40 ± 0.04 mag.
CCD photometric observations of two Near-Earth asteroids (NEAs) were made from 2018 November 6 to 9. Fourier analysis of the data for 2018 UQ1 and 2018 UR2 yielded rotations periods of 3.73 ± 0.01 h and 6.88 ± 0.01 h, respectively.
CCD Photometric Observations of Asteroids 2678 Aavasaksa, 3769 Arthurmiller, 4807 Noboru, (7520) 1990 BV, and (14510) 1996 ES2
CCD photometric observations of asteroids 2678 Aavasaksa, 3769 Arthurmiller, 4807 Noboru, (7520) 1990 BV, and (14510) 1996 ES2, were conducted from the George West ISD Mobile Observatory. The rotational period of 2678 Aavasaksa is 124 ± 2 hours, with an amplitude of 1.3 magnitudes. The rotational period of 3769 Arthurmiller is 8.28 ± 0.01 hours, with an amplitude of 0.82 magnitudes. The rotational period of 4807 Noboru is 4.04 ± 0.02 hours with an amplitude of 0.23 magnitudes. The rotational period of (7520) 1990 BV is 3.83 ± 0.01 hours with an amplitude of 0.28 magnitudes. The rotational period of (14510) 1996 ES2 is 6.24 ± 0.01 hours, with an amplitude of 0.35 magnitudes.
Rotational Periods and Lightcurves of 1475 Yalta and 7230 Lutz
Photometric observations were made from 2018 October 12 to December 18 of the main-belt asteroids 1475 Yalta and 7230 Lutz at the Elianto Observatory located at Pontecagnano, Italy.
Lightcurve and Spin-Shape Model for 16847 Sanpoloamosciano
The minor planet 16847 Sanpoloamosciano at the 2018 opposition had a synodic rotation period 8.183 ± 0.001 h and amplitude 0.15 ± 0.02 mag. A lightcurve inversion spin-shape model based on dense and sparse data provides a sidereal period 8.184371 ± 0.000046 h with two mirrored pole solutions at (λ = 90°, β = –39°) and (λ = 286°, β = –20°) with an error of ± 10 deg.
We report on the photometric analysis results for eleven main-belt asteroids (MBA) and one near-Earth asteroid by Asteroides Observers (OBAS). This work is part of the Minor Planet Photometric Database effort that was initiated by a group of Spanish amateur astronomers. We have managed to obtain a number of accurate and complete lightcurves as well as some additional incomplete lightcurves to help analysis at future oppositions.
Lightcurve Analysis of Three Potentially Hazardous Asteroids
CCD photometric observations of three near-Earth asteroids (NEAs) also listed as potentially hazardous (PHAs) were made during 2016 September and 2018 April. Fourier analysis of the data for the three targets found rotation periods for 1999 YR14, 4.40 ± 0.05 h; 2016 LX48, 2.23 ± 0.06 h; and 2018 BY2, 9.17 ± 0.01 h.
Lightcurve Analysis and Rotation Period for 5321 Jagras
Data for asteroid 5321 Jagras were collected from 2018 October 12th to 2018 November 14th. The lightcurve analysis obtained has led to a trimodal curve with a period of 2.6375 ± 0.0001 hours, with an amplitude equal to 0.06 mag, with a full coverage.
Asteroid Lightcurve and Synodic Period Determinations: 2018 October-December
Results of lightcurve and synodic rotation period determinations from photometric data obtained at Sopot Astronomical Observatory for eight asteroids in the time span 2018 October - December are presented.
Rotation Period Determination for 3157 Novikov and 7485 Changchun
Pages 211-212 Marchini, Alessandro; Papini, Riccardo; Banfi, Massimo; Salvaggio, Fabio; Bachini, Mauro; Galdies, Charles; Brincat, Stephen M. 2019MPBu...46..211MDownload PDF
Collaborative photometric observations of two main-belt asteroids were conducted from five observatories in order to determine their synodic rotation periods. For 3157 Novikov we found a period of 9.952 ± 0.001 h with an amplitude of 0.31 ± 0.04 mag, for 7485 Changchun we found a period of 10.234 ± 0.001 h with an amplitude of 0.39 ± 0.02 mag.
Rotation Period Determination of Three Main-belt Asteroids: 3769 Arthurmiller, 3995 Sakaino and (7520) 1990 BV
Photometric observations of three main-belt asteroids were conducted from the Astronomical Observatory of the University of Siena (Italy) in order to determine their synodic rotation periods. For 3769 Arthurmiller we found a period of 8.297 ± 0.001 h with an amplitude of 0.78 ± 0.01 mag, for 3995 Sakaino we found a period of 4.552 ± 0.001 h with an amplitude of 0.97 ± 0.02 mag and for (7520) 1990 BV we found a period of 3.828 ± 0.001 h with an amplitude of 0.26 ± 0.04 mag.
Lightcurve photometry observations of the main-belt asteroid (32209) 2000 OW9 were made at Xingming Observatories on 2019 Jan 6. We find that the asteroid has a synodic rotation period of 4.85 ± 0.11 h and amplitude of 0.32 ± 0.04 mag.
We present 4.6 and 3.4 micron lightcurves of the Amor class near-Earth asteroid (523806) 2002 WW17 constructed from NEOWISE measurements in 2018 October and December. The lightcurve from the December measurements exhibit a 10.51 ± 0.08 hour period with a maximum amplitude of variation of nearly two magnitudes. The October lightcurve has a period consistent with that measured in December, but with an amplitude of approximately 0.8 mag.
Rotation Period Determination of the Asteroid 5321 Jagras (1985 VN)
Pages 218-219 Papini, Riccardo; Banfi, Massimo; Salvaggio, Fabio; Marchini, Alessandro; Franco, Lorenzo 2019MPBu...46..218PDownload PDF
Photometric observations were made in 2018 of the main-belt asteroid 5321 Jagras (1985 VN). Analysis of the collected data suggests a period of 2.638 ± 0.001 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.
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.
