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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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
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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.
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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
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Photometric observations of the main-belt asteroid 665 Sabine were conducted from the NOAK Observatory, in Greece in order to determine its synodic rotation period. The results are: P = 4.299 ± 0.004 h, A = 0.33 mag.
Fast Rotator Minor Planet 2020 UA From Cluj and Berthelot Observatory
We have observed minor planet 2020 UA during an exceptional close approach and determined that it is a fast rotator. For two data sets, taken 2 hours apart, our measurements suggest two different rotational periods: 0.0440 ± 0.0006 h and 0.0293 ± 0.0002 h.
I present high quality lightcurve data on the large Hilda 1269 Rollandia. The data were obtained using a 0.9m telescope at Cerro Tololo Interamerican Observatory in Chile in May 2013 and cover over 17 hours split over two consecutive nights. This data is not sufficient to find a reliable rotation period for Rollandia. However, the data it is sufficient to rule out most of the published periods for this object.
Photometric Analysis and Rotation Period Determination of the Potentially Hazardous Asteroid 2020 WU5
Pages 104-105 Marchini, Alessandro; Papini, Riccardo; Baj, Giorgio; Galli, Gianni; Bacci, Paolo; Franco, Lorenzo 2021MPBu...48..104MDownload PDF
Photometric observations of 2020 WU5 were conducted in 2021 January in order to determine its synodic rotation period and revealed a bimodal solution with P = 5.574 ± 0.002 h and an amplitude A = 0.84 ± 0.08 mag.
Rotational Period and Lightcurve Determination of 2020 UQ6: A Super Fast Rotator
The lightcurve and rotation period determination for 2020 UQ6 are reported based on observations made in late October 2020. 2020 UQ6 is a super-fast rotator with a period of 0.04521 +/- 0.000001 h.
Photometric observations of two main-belt asteroids, (11894) 1991 GW, 19120 Doronina (1983 PM1), were made at the Filzi School Observatory (School in country Laives - Italy) MPC code D12.
Photometric observations of three main-belt asteroids, (18640) 1998 EF9, (41331) 1999 XB232, (50713) 2000 EZ135, were made at the Filzi School Observatory (School in country Laives - Italy) MPC code D12.
The main-belt asteroid 1526 Mikkeli was observed over seven nights throughout 2020 October-November in order to determine its synodic rotational period. Lightcurve analysis was done using differential photometry technique using MPO Canopus (Warner, 2012). The observations were carried out from “F. Fuligni” Observatory using a 0.35-m f/10 ACF telescope and SBIG ST8-XE CCD camera unfiltered. All images were dark and flat-field calibrated with Maxim DL.
Photometric Analysis and Rotation Period Determination for Asteroids 5445 Williwaw, (8823) 1987 WS3 and (26568) 2000 ET49
Photometric observations of three main-belt asteroids were conducted in order to determine their synodic rotation periods. For 5445 Williwaw we found P = 10.65 ± 0.02 h, A = 0.29 ± 0.05 mag; for (8823) 1987 WS3, a slow rotator, we found a rough period of P = 86.0 ± 1.0 h, A = 0.24 ± 0.02 mag; for (26568) 2000 ET49 we found P = 7.171 ± 0.003 h, A = 0.71 ± 0.04 mag
We report rotation lightcurves of 1840 Hus observed during its apparition in 2020. The constraints from our data, combined with a reanalysis of published lightcurves recorded in 2009, yield a secure rotation period of 4.7483 ± 0.0008 h.
In the following paper we present the result of a photometric survey on six asteroids: 2262 Mitidika, P = 28.257 ± 0.004 h, A = 0.26 mag; 3955 Bruckner, P = 7.549 ± 0.002 h, A = 0.25 mag; (16559) 1991 VA3, P = 473.34 ± 0.27 h, A = 1.17 mag; (21182) 1994 EC2, P = 12.981 ± 0.002 h, A = 0.10 mag; (22393) 1994 QV, P = 3.419 ± 0.001 h, A = 0.23 mag; (43028) 1999 VE23, P = 3.940 ± 0.002 h, A = 0.36 mag.
Photometry of 12 Asteroids from Sopot Astronomical Observatory: 2020 October- December
A brief overview of the lightcurve and synodic rotation period determination for 12 asteroids from CCD photometric observations conducted at Sopot Astronomical Observatory (SAO) in the time span 2020 October - December is presented in this paper.
Collaborative Asteroid Photometry from UAI: 2020 October-December
Photometric observations of five asteroids were made in order to acquire lightcurves for shape/spin axis modeling. The synodic period and lightcurve amplitude were found for 102 Miriam: 23.63 ± 0.01 h, 0.14 mag; 635 Vundtia: 11.784 ± 0.004 h, 0.20 mag; 1342 Brabantia: 4.175 ± 0.001 h, 0.13 mag; 2346 Lilio: 3.0290 ± 0.0005 h, 0.18 mag; (153201) 2000 WO107: 5.026 ± 0.001 h, 1.14 mag.
CCD Photometric Observations of Asteroids 4493 Naitomitsu, (21242) 1995 WZ41, (68130) 2001 AO17, And (183230) 2002 TC58
Using a previously described workflow built on applying to each image dozens of comparison stars from the ATLAS refcat2 catalog, we have obtained and present here lightcurves and synodic rotation periods for eighteen asteroids.125-132
Lightcurves and Rotation Periods of 67 Asia, 74 Galatea, 356 Liguria, 570 Kythera, 581 Tauntonia, 589 Croatia, and 605 Juvisia
Asteroids 4092 Tyr (Follow Up, Analysis, Preliminary Results) and 699 Hela (Spin-Shape Model)
Pages 136-139 Alonso, E. Díez; García, F.; Farfán, R.G.; Pravec, P.; Gutiérrez, P.J.; Ruíz, J.; Limón, F.; Delgado, J.; Naves, R.; Bosch, J.M.; Reina, E.; Temprano, J.; Gómez, Sergio Luis Suárez; Gutiérrez, C. González; García, F. Riesgo; Fernández, S.; de Cos Juez, J. 2021MPBu...48..136ADownload PDF
In this work we present the results of the photometric follow up of the asteroid 4092 Tyr carried out by the Grupo de Observadores de Asteroides throughout the months of 2020 August and September. The rotation period derived from the observations is P = 16.091 ± 0.003 h. Furthermore, 4092 Tyr has been revealed to be a synchronous binary asteroid with two main bodies of similar size. We also present a confirmation of the rotation period of the asteroid 699 Hela (0.1415100 ± 0.0000024 d), and a study of its shape and spin. We analyze dense lightcurves acquired in 2020 by the Grupo de Observadores de Asteroides, as well as those available in public databases. We have also used sparse lightcurves from USNO (Flagstaff) and the TESS mission. We find two possible solutions for the spin axis (λ1, ß1) = (37°, +51°), (λ2, ß2) = (189°, +14°), in agreement with previously published models.
Asteroid Photometry and Lightcurve Analysis at Gora’S Observatories, Part IV.
Synodic rotation periods and amplitudes are reported for: 424 Gratia, 579 Sidonia, 589 Croatia, 693 Zerbinetta, 791 Ani, 824 Anastasia, 858 El Djezair, 1024 Hale, 1271 Isergina, 1663 van den Bos.
Photometric Observations of Eight Minor Planets for Shape Modeling
Phased lightcurves and synodic rotation periods for eight main-belt asteroids are presented, based on CCD observations made in 2020 October. The purpose of obtaining these particular lightcurves is to augment shape modeling efforts. All the data have been submitted to the ALCDEF database.
Rotational Period and Lightcurve Determination of 4625 Shchedrin, (8823) 1987 WS3, (15010) 1998 QL92, (19755) 2000 EH34, and 21082 Araimasaru
Pages 147-149 Noschese, Alfonso; Ruocco, Nello; Catapano, Antonio; Mollica, Maurizio; Vecchione, Antonio 2021MPBu...48..147NDownload PDF
Photometric observations of five asteroids were performed in order to acquire lightcurves and to determine the rotational periods. The synodic period and lightcurve amplitude were found for 4625 Shchedrin, (8823) 1987 WS3, (15010) 1998 QL92, (19755) 2000 EH34, and 21082 Araimasaru.
Main-belt Asteroids Observed from CS3: 2020 October to December
Phased lightcurves and synodic rotation periods for 17 main-belt asteroids are presented, based on CCD observations made from 2020 October through 2020 December. All the data have been submitted to the ALCDEF database.
Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2020 October-December
New CCD photometric observations of two Hilda asteroid members were made from 2020 October through December: 748 Simeisa and 1754 Cunningham. The latest data for Simeisa conclusively reject earlier reports of a period near 11.9 h.
Lightcurve Based Determination of 10 Hygiea’S Rotational Period With Trappist-North and -South
A densely-sampled lightcurve of the large main-belt asteroid 10 Hygiea was obtained with the TRAPPISTSouth (TS) and TRAPPIST-North (TN) telescopes in 2018 September and October. We found its synodic rotation period and amplitude to be 13.8224 ± 0.0005 h and 0.27 mag. The data have been submitted to the ALCDEF database.
Lightcurve Analysis of L4 Trojan Asteroids at the Center for Solar System Studies: 2020 October to December
Observers who have made visual, photographic, or CCD measurements of positions of minor planets in calendar year 2020 are encouraged to report them to this author on or before 2021 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 2020,” to be published in MPB Vol. 48, No. 3.
Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2020 September to 2021 January
Lightcurves of 22 Near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2020 October to early 2021 January were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling.
Lightcurves and amplitudes for ten near-Earth asteroids observed from Great Shefford Observatory during close approaches in 2018 and 2020 are reported: 2018 KF1, 2020 GF2, 2020 OH3, 2020 RA6, 2020 RZ6, 2020 TP1, 2020 TD8, 2020 UQ6, 2020 VZ6 and 2020 XX3. 2020 UQ6 is the largest, with H = 22.6, all others are small objects, H > 24.5. Seven have superfast rotation periods, P < 10 min, including 2020 RZ6 and 2020 TD8 with P < 1 min.
On Confirmed and Suspected Binary Asteroids Observed at the Center for Solar System Studies
The analysis of observations made at the Center for Solar System Studies from 2020 September to 2021 January led to the discovery that the Vestoid asteroid 3865 Lindbloom is a fully synchronous binary. The orbital period is 26.016 h and the ratio of the effective diameters is 0.65 < Ds/Dp < 1.0. Assuming a bulk density of 2 g/cm, Dp <= 7.2 km, Ds >= 4.6 km, and the center-to-center separation is 20 km. Other objects presented here were found to have secondary periods: 4503 Cleobulus, (22056) 2000 AU31, 25465 Rajagopalan, (46818) 1998 MZ24, (48205) 2012 TQ78, 2013 PY6, and 2020 PD1. Of those, only 1998 MZ24 and 2013 PY6 might be said to show mutual events due to a satellite.
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.
