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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CCD photometric observations of main-belt asteroid 5237 Yoshikawa were obtained in order to measure its rotation period. These measures were performed during two different nights on 2022/04/05 and 2022/04/10, using the instrumentation available at the Osservatorio Astronomico Margherita Hack located on the hills near Florence (Italy).
Lightcurve Photometry of Asteroid 8693 Matsuki
Pages 242-243 Sani, Idris Abubakar; Nowinski, Matthew C.; Umahi, A. E.; Okike O.; Oyibo M, Umeh C. N.; Okolo O. E.; Bonaventure Okere 2022MPBu...49..242SDownload PDF
Lightcurve photometry of the main-belt asteroid 8693 Matsuki yielded an estimated period of 6.10550 ± 0.00225 h and an amplitude of 0.53 ± 0.01 mag.
Asteroid 471109 Vladobahyl (2010 CO12): Observations of the Lightcurve
We present CCD photometry results for the asteroid 471109 Vladobahyl (2010 CO12). From 507 images we have constructed the lightcurve of this asteroid and estimate its rotational period to be 4.9217 ± 0.1746 h.
Photometric measurements were conducted on asteroid 2999 Dante from the Phillips Academy Observatory (PAO), the Mittelman Observatory, and the iTelescope T18 Observatory from 2022 February 06 to March 04. The rotational period and amplitude were determined to be 49.714 ± 0.001 h and 0.55 ± 0.05 mag.
Lightcurve Analysis of Asteroid 5889 Mickiewicz
Pages 246-247 Odden, Caroline; Cahill, Claire; Darling, Victoria; Du, Anna; von Eckartsberg, Nicholas; Gerakaris, Ethan; He, Jessica; Jin, Yifei; Lin, Jeremy; McCormack, Mason; Reagan, Brooklyn; Shen Xinkai 2022MPBu...49..246ODownload PDF
Photometric observations of asteroid 5889 Mickiewicz were performed at the Phillips Academy Observatory (PAO) from 2022 April 30 to May 26. The rotational period and amplitude were determined to be: P = 6.141 ± 0.001h, A = 0.51 ± 0.05 mag.
Lightcurve Analysis and Rotation Period Determination of Asteroid 1466 Mundleria
Photometric observations of asteroid 1466 Mundleria (e = 0.15, i = 13.15°, H = 12.23) were conducted using telescopes located in New Mexico, Italy, and Malta between 2022 Mar 24 and Apr 25. An analysis of these data yielded a rotation period of 89.280 ± 0.065 h.
Rotation Period Determination and Lightcurve Analysis of Asteroid 3736 Rokoske
Observations of the main-belt asteroid 3736 Rokoske were conducted over 8 nights between 2022 March 25 and 2022 April 23. Images were collected using three telescopes in the USA, Malta, and Italy. 3736 Rokoske has a diameter of 19.5 km and an absolute magnitude of 11.15. MPO Canopus was used for calibration and lightcurve analysis. The phased lightcurve resulted in a rotation period of 17.411 ± 0.004 h and 0.10 ± 0.02 mag amplitude.
A Reexamination of the Rotation Period of 1541 Estonia
A previously published period ambiguity for 1541 Estonia of 6.444 or 12.890 hours has been reexamined. We prefer a 12.889 ± 0.001-hour period with amplitude 0.16 ± 0.01 magnitudes.
Rotation Period Determination for Asteroid 3616 Glazunov
Photometric observations of the main-belt asteroid 3616 Glazunov were conducted in order to determine its synodic rotation period. We found P = 18.932 ± 0.004 h, A = 0.14 ± 0.03 mag.
Lightcurve for Koronis Family Member (1363) Herberta
Pages 253 Wilkin, Francis P.; Bromberg, Jayson; AlMassri, Zuhair; Beauchaine, Louis; Nguyen, Minh 2022MPBu...49..253WDownload PDF
We present our composite lightcurve for Koronis family asteroid (1363) Herberta. Based upon six nights in 2022 we obtained an improved rotation period of 3.016 ± 0.002 h with amplitude 0.13 ± 0.02 mag.
The Rotation Period and Variability Amplitude of 1664 Felix
Photometric monitoring of 1664 Felix was carried out in 2022 February through a Johnson V filter. Based on 90 images collected over two nights, we find a best-fit rotation period of 3.345±0.001 hours, in good agreement with previous results, and a V-band variability amplitude of 0.45±0.02 mag that is slightly larger than previously reported from observations through a clear filter.
Broad-band Photometric Monitoring of 1226 Golia and 6349 Acapulco
Broad-band photometric monitoring of 1226 Golia and 6349 Acapulco was carried out in 2021 February-March. For 1226 Golia, we report a rotation period of 4.46 ± 0.05 h and a V-band variability amplitude of 0.41 ± 0.02 mag, which are in agreement with the range of previously reported measurements. For 6349 Acapulco, we find typical colors for a C-type asteroid of B-V = 0.7 ± 0.1 mag and V-R = 0.3 ± 0.1 mag and little evidence for color changes as a function of time. We report a rotation period of 4.48 ± 0.05 h that is in good agreement with a previous measurement, and a variability amplitude of 0.55 ± 0.02 mag that is three times larger than previously reported.
Photometric monitoring of 782 Montefiore was carried out in 2020 February through a Johnson V filter. Based on 247 images collected over three nights, we find a best fit rotation period of 4.073±0.001 h and a V-band variability amplitude of 0.50±0.02 mag, in good agreement with previous results.
We have observed minor planet 2022 KK5 during a close approach on 30th of May 2022 and determined that it is a fast rotator, having a rotational period of 0.0830±0.0002 h, with uneven minima and maxima.
(29606) 1998 QN94: A Binary Asteroid in a Self-synchronous Orbit
We report that asteroid (29606) 1998 QN94 is a binary asteroid. The primary lightcurve has a period of 2.8965 ± 0.0001 h and an amplitude 0.17 mag. The orbital period of the secondary matches what we deduce as its own rotation period: 19.666 ± 0.004 h.
On Confirmed and Suspected Binary Asteroids Observed at the Center for Solar System Studies: 2022 March-June
Analysis of CCD photometric observations of seven asteroids from 2022 March to June at the Center for Solar System Studies indicate that, by virtue of a suspected or distinct second period, they are either suspected or confirmed binary asteroids.
Lightcurves for Three Koronis Family Asteroids from the Union College Observatory
We present lightcurves for Koronis family asteroids (243) Ida, (321) Florentina, and (2713) Luxembourg. All had periods consistent with previously reported values and showed classic doubly-periodic lightcurves.
Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2022 March-May
CCD photometric observations of four Hilda asteroids were made at the Center for Solar System Studies between 2022 March and May. Of those, 3561 Devine and 8551 Daitarabochi had distinct secondary periods.
Photometry and Lightcurve Analysis of Four Mars-crossing Asteroids
Rotational periods of four Mars-crossing asteroids (MCs) were determined from lightcurves acquired at the Observatório Astronômico do Sertão de Itaparica (MPC Y28, OASI) between 2020 July to 2021 October.
Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2022 March-June
CCD photometry of 11 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) in 2022 March to June were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling. While there were no signs of any of the asteroids being binary, seven of them are suspected tumblers: (10302) 1989 ML, (100756) 1998 FM5, (163692) 2003 CY18, (388945) 2008 TZ3, (464798) 2004 JX20, and 2018 XV5.
Lightcurves and amplitudes for seven near-Earth asteroids observed from Great Shefford Observatory during close approaches between 2022 April and June are reported. Four are superfast rotators with periods P < 1 minute. The effects of lightcurve smoothing due to an inappropriately chosen exposure length are modelled for 2022 JL.
Lightcurve Analysis of L5 Trojan Asteroids at the Center for Solar System Studies: 2022 June
Lightcurves for three Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) in 2022 June.
Rotation Periods for Asteroids from Carl Sagan Observatory: 2021 November - 2022 May
Pages 289-290 Loera-González, P. A.; Olguín, P. A.; Saucedo, J. C.; Contreras, M. E.; Nuñez-López, R.; Domínguez-González, Rafael; Angulo, O. E.; Chapetti, S. D.; Córdova, D. E.; Cortez, R. A.; Ramírez, M. A.; Vázquez, P. S. 2022MPBu...49..289LDownload PDF
We present photometric visible wavelength lightcurves and derive rotation periods for a sample of four asteroids:190 Ismene (6.5195 ± 0.0002 h), 5009 Sethos (2.688 ± 0.001 h), (7335) 1989 JA (2.590 ± 0.002 h) and (11512) 1991 AB2 (2.93275 ± 0.00025 h). Observations were carried out at the Observatorio Astronómico Carl Sagan (OACS) of the Universidad de Sonora in Hermosillo, México.
Photometric Observations and Rotation Periods of Asteroids 2376 Martynov, (7335) 1989 JA, 12923 Zephyr, and (85184) 1991 JG1
Photometric observations of asteroids 2376 Martynov, (7335) 1989 JA, 12923 Zephyr, and (85184) 1991 JG1 were conducted in order to determine their synodic rotation period, the absolute brightness with its amplitude, and estimate their diameter. For 2376 Martynov we found P = 11.133 ± 0.005 h, H = 11.07 ± 0.05 mag, A = 0.38 ± 0.05 mag, D = 47.583 ± 0.529 km (for albedo a = 0.0364) and D = 39.212 ± 0.588 km (for albedo a = 0.0536). For (7335) 1989 JA we found P = 5.177 ± 0.005 h, H = 17.48 ± 0.05 mag, A = 0.27 ± 0.05 mag, D = 0.849 ± 0.009 km (for albedo a = 0.25) and D = 0.748 ± 0.010 km (for albedo a = 0.322). For 12923 Zephyr we found P = 3.894 ± 0.002 h, H = 15.73 ± 0.05 mag, A = 0.21 ± 0.05 mag, D = 2.260 ± 0.025 km (for albedo a = 0.1764) and D = 2.072 ± 0.027 km (for albedo a = 0.21). For (85184) 1991 JG1 we found P = 24.14 ± 0.02 h, H = 18.37 ± 0.07 mag, A = 0.65 ± 0.07 mag, D = 0.631 ± 0.008 km (for albedo a = 0.20).
Rotational Period and Lightcurve Determination for Four Asteroids
Photometric observations were conducted of four mainbelt asteroids. The results of lightcurve analysis gave synodic rotation periods and amplitudes shown in the table below.
Photometric measurements of CCD observations on 16 main-belt asteroids were made from 2022 April through May. Phased lightcurves were created for twelve asteroids, while four did not yield period solutions. All the data have been submitted to the ALCDEF database.
Asteroid Photometry and Lightcurve Analysis for Six Asteroids
Densely sampled lightcurves of 25 large main-belt asteroids were obtained with the TRAPPIST-South (TS) and TRAPPIST-North (TN) telescopes from 2017 to 2021. Those observations took place in support of an ESO large program aiming at observing a representative sample of large asteroids with the ESO VLT for precise shape determination from adaptive optics high-resolution imaging. Synodic rotation periods and lightcurve amplitudes have been determined for all but one target. Six asteroids were observed during two different apparitions. The data have been submitted to the ALCDEF database.
Main-belt Asteroids Observed from CS3: 2022 April-June
CCD photometric observations of 22 main-belt asteroids were obtained at the Center for Solar System Studies (CS3) from 2022 April-June. One revised period from observations obtained in 2005 is also reported.
Rotational Period Determination and Taxonomic Classification for Asteroids 417 Suevia, 554 Peraga, and 747 Winchester
CCD photometric observations of three main-belt asteroids were made between 2022 January and March in order to measure their rotation periods and define their taxonomic class. The observations used instrumentation available at our two observatories.
Lightcurve Analysis of Three Main Belt Astreroids: 2265 Verbaandert, 3787 Aivazovskij, and 4528 Berg
2265 Verbaandert was imaged on seven nights between 2022 Feb 13 and 2022 Apr 03. A period of 2.8143 ±0.0001 hours and amplitude of 0.105 magnitude are reported. 3787 Aivazovskij was imaged five nights between 2022 Jan 06 and 2022 Feb 07. A period of 2.9532±0.0001 hours and amplitude of 0.191 magnitude are reported. 4528 Berg was imaged on eight nights from 2022 Apr 07 to 2022 May 07. A period of 3.5630±0.0001 hours and amplitude of 0.345 magnitude are reported.
CCD Photometry of 35 Asteroids at Sopot Astronomical Observatory: 2021 November - 2022 July
Lightcurves and synodic rotation periods were established for 35 asteroids using photometric observations carried out at Sopot Astronomical Observatory between 2021 November and 2022 July are presented in this paper.
Collaborative Asteroid Photometry from UAI: 2022 April-June
Photometric observations of ten asteroids were made in order to acquire lightcurves for shape/spin axis modeling. The synodic period and lightcurve amplitude were found for 323 Brucia, 342 Endymion, 542 Susanna, 578 Happelia, 1656 Suomi, 4221 Picasso, (5693) 1993 EA, (7335) 1989 JA, 2022 BT and 2022 MP. We also found color indices for 323 Brucia and (7335) 1989 JA.
Lightcurves and Rotation Periods of 233 Asterope, 240 Vanadis, 275 Sapientia, 282 Clorinde, 414 Liriope, and 542 Susanna
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 using lightcurve inversion. We have changed the presentation of the “Radar-Optical Opportunities” section to include a list of potential radar targets as well as some that are in critical need of astrometric data and, if found, might also be targets for radar. These can have ephemeris errors on the order of tens to thousands of arcseconds and, despite the current surveys, have not been observed for several years. This makes them a double challenge: first to be found and, second, to determine astrometric positions and photometric properties.
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.
