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
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.
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Photometric observations of two main-belt asteroids were conducted from the Astronomical Observatory of the University of Siena, in Italy, in order to determine their synodic rotation periods. For 992 Swasey we found: P = 13.305 ± 0.007 h, A = 0.16 ± 0.02 mag; and for 3096 Bezruc we found P = 27.350 ± 0.004 h, A = 0.62 ± 0.03 mag.
We present a preliminary shape and spin axis model for main-belt asteroid 755 Quintilla. The model was derived using lightcurve inversion that combined dense photometric data acquired from three apparitions between 2004 and 2020 and sparse data from USNO Flagstaff. Analysis of the resulting data found a sidereal period P = 4.55204 ± 0.00001 h and two mirrored pole solutions at (l, b) = (109°, –12°) and (288°, –3°) with an uncertainty of ± 20°.
Pages 269 Franco, L.; Marchini, A.; Saya, L.-F.; Galli, G.; Baj, G.; Ruocco, N.; Mannucci, M.; Montigiani, N.; Tinelli, L.; Scarfi, G.; Aceti, P.; Banfi, M.; Bacci, P.; Maestripieri, M.; Papini, R.; Salvaggio F.; Mortari, F.; Bachini, M.; Casalnuovo, G.B.; Chinaglia, B.
Incorrect values were given for the lower limit of the secondaryto- primary mean diameter ratio Ds/Dp for the asteroids 1052 Belgica and 7132 Casulli. The correct values are: 1052 Belgica, 0.39 ± 0.02; 7132 Casulli, 0.33 ± 0.02.
Collaborative Asteroid Photometry from UAI: 2020 April-June
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 58 Concordia: 9.8953 ± 0.0007 h, 0.08 mag; 781 Kartvelia: 19.050 ± 0.005 h, 0.22 mag; 913 Otila: 4.8717 ± 0.0007 h, 0.18 mag; 3317 Paris: 7.0812 ± 0.0004 h, 0.10 mag; and 3800 Karayusuf: 2.2319 ± 0.0001 h, 0.15 mag.
Spin-Shape Model for 50 Virginia
Pages 272-274 Franco, Lorenzo; Pilcher, Frederick
We present a shape and spin axis model for main-belt asteroid 50 Virginia. The model was achieved with the lightcurve inversion process, using combined dense photometric data acquired from seven apparitions between 1995-2020 and sparse data from USNO Flagstaff. Analysis of the resulting data found a sidereal period P = 14.31233 ± 0.00005 h and two mirrored pole solutions (ecliptic coordinates) at (l, b) = (112°, 41°) and (295°, 47°) with an uncertainty of ± 10 degrees.
Main-Belt Asteroids Observed from CS3: 2020 April to June
Pages 275-284 Stephens, Robert D.; Warner, Brian D.
CCD photometric observations of 18 main-belt asteroids were obtained at the Center for Solar System Studies (CS3) from 2020 April to June.
Lightcurve Analysis of L5 Trojan Asteriods at the Center for Solar System Studies: 2020 April to June
Pages 285-289 Stephens, Robert D.; Warner, Brian D.
Lightcurves for nine L5 Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2020 April to June.
Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2020 April - June
Pages 290-304 Warner, Brian D.; Stephens, Robert D.
Lightcurves for 29 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2020 April to June were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling.
Binary Asteroids at the Center for Solar System Studies
Pages 305-308 Warner, Brian D.; Stephens, Robert D.; Harris, Alan W.
We report on the discovery at the Center for Solar System Studies of four confirmed binary asteroids: 1656 Suomi, (85275) 1994 LY, (85628) 1998 KV2, and (539940) 2017 HW1 along with the suspected candidate (184990) 2006 KE89.
Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 1529 Oterma And 17428 Charleroi
Pages 309-313 Warner, Brian D.; Stephens, Robert D.
New CCD photometric observations of 1529 Oterma were made in 2020 May, leading to a preferred period of 14.317 h. This differs from one of our earlier results by an almost exact 8:5 ratio. The data for 17428 Charleroi from 2020 allowed both 4.8 and 6.0 h periods, which are nearly an exact 5:4 ratio. A review of data from 2016 found an alternate period of 4.793 h but could not formally exclude a solution near 5.99 h, which was the only period possible from the 2017 data. Both cases suggest that rotational aliasing is at play and so make it difficult to find a secure solution.
Photometric Observations of Twenty-Seven Minor Planets
Pages 314-321 Polakis, Tom
Phased lightcurves and synodic rotation periods for 26 main-belt asteroids are presented, based on CCD observations made from 2020 March through 2020 June. A raw lightcurve is included for one asteroid for which no period solution was found. All the data have been submitted to the ALCDEF database.
A Search for Mutual Eclipse Events of the Asynchronous Binary Asteroid 1016 Anitra
Pages 322-323 Lang, Kim
Asteroid 1016 Anitra was observed extensively between 2020 March 13 and April 24. Mutual eclipse events were searched for but none were observed. Data are analyzed in two sub sets. The March subset found two bimodal lightcurves with periods and amplitudes of P1= 5.9292 ± 0.0002 h, A1 = 0.30 mag and P2 = 2.6092 ± 0.0002 h, A2 = 0.11 mag. The April subset found P1= 5.9281 ± 0.0002 h, A1 = 0.34 mag and P2 = 2.6091 ± 0.0001 h, A2 = 0.11 mag.
A New Photometric Workflow and Lightcurves of Fifteen Asteroids
Pages 324-330 Dose, Eric V.
A new data reduction workflow makes intense use of the recent ATLAS refcat2 catalog, with the intent of using every eligible comparison star available in the sky field of view. By applying this workflow to CCD observations made late 2019 and early 2020, we generated lightcurves and synodic rotation periods, also presented here, for fifteen asteroids of various families.
Pages 330-335 Warner, Brian D.; Harris, Alan W.; Durech, Josef; Benner, Lance A.M.
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.
Rotational Period and Lightcurve of 7910 Aleksola
Pages 336-337 Noschese, Alfonso; Ruocco, Nello; Vecchione, Antonio
The lightcurve and rotation period determination for 7910 Aleksola are reported. The results are: P = 6.420 ± 0.002 h and A = 0.17 mag.
Asteroid Photometry and Lightcurve Analysis at Gora’S Observatories – Part II.
Synodic rotation periods and amplitudes are reported for 414 Liriope, 949 Hel, 952 Caia, and 1145 Robelmonte.
The 2019 Mexican Asteroid Photometry Campaign
Pages 340-342 Olguín, L.; Saucedo, J. C.; Loera-González, P.; Contreras, M. E.; Valdés, J. R.; Guichard, J.; López-González, R.; Michimani-García, J.; Cerdán-Hernández, G.; Schuster, W. J.; Valdés-Sada, P.; Núñez-López, R.; Ayala-Gómez, S. A.
We present photometric optical lightcurves and derived rotation periods for a sample of five asteroids: 722 Frieda (30.06 ± 0.02 h), 1239 Queteleta (10.278 ± 0.003 h), 2162 Anhui (8.101 ± 0.001 h), 4148 McCartney (20.756 ± 0.0006 h), and 4408 Zlata Koruna (4.392 ± 0.001 h). These observations were carried out at the Observatorio Astronómico Nacional at Sierra San Pedro Mártir (OAN-SPM), Baja California, Mexico, the Carl Sagan Observatory (OCS) of the Universidad de Sonora, México, and at the INAOE Tonantzintla Observatory (TONA), Puebla, México.
Measured Lightcurves and Rotational Periods of 1132 Hollandia and 1184 Gaea
Pages 343-344 Fauerbach, Michael
Photometric observations of 1132 Hollandia and 1184 Gaea were obtained on three nights 2020 January 27 to 2020 February 16. The following rotational periods were determined: 1132 Hollandia 5.322 ± 0.001 h; 1184 Gaea 2.873 ± 0.001 h.
Lightcurves and Rotation Periods of 50 Virginia, 57 Mnemosyne, 58 Concordia, 59 Elpis, 78 Diana, and 529 Preziosa
Determining the Rotational Periods and Lightcurves of Three Main-Belt Asteroids
Pages 347-348 Bonamico, Roberto
CCD photometric observations of three main-belt asteroids were made from 2020 March to May. We report the results of lightcurve analysis for 1784 Benguella: P = 41.035 ± 0.008 h, A = 0.87 mag; 4582 Hank: P = 6.446 ± 0.001 h, A = 0.58 mag; and 5947 Bonnie: P = 13.414 ± 0.003 h, A = 0.10 mag.
Lightcurve Based Rotational Period Determination for Asteroids 1579 Herrick and 2171 Kiev
We present results for rotational period determination using lightcurves for two asteroids observed during the first half of 2020. For 1579 Herrick we obtained P = 9.196 ± 0.002 h and amplitude A = 0.12 ± 0.03 mag, for 2171 Kiev we obtained P = 3.1714 ± 0.0002 h and amplitude A = 0.14 ± 0.08 mag. We also found evidence for the presence of a secondary period P2 = 23.38 ± 0.03 h.
Call for Observations of the Active Centaur 29P/Schwassmann-Wachmann
29P/Schwassmann-Wachmann is the most famous resident of the Centaur-JFC (Jupiter Family Comet) “gateway” region just beyond Jupiter. It may eventually become the brightest JFC in human history (Sarid et al., 2019). Its nucleus has exhibited a dust coma for more than 90 years, and it undergoes explosive outbursts several times a year. It is a strong candidate for a future space mission, and long-term dedicated and coordinated surveys from amateur and professional astronomers are needed to characterize the near-nucleus region and monitor material produced during outbursting events and quiescent outgassing activity. Through long-term monitoring we also seek to constrain the nucleus’ rotation period and spin pole orientation. We request multi-wavelength, multi-modality observations, including visible lightcurves, photometry, broadband filter imaging, astrometry, spectroscopy, interferometry and occultations. This article provides suggested observing dates, guidance about useful observations, predictions for a minimum visual magnitude, and a link to an observing campaign planning website. Interested observers are also welcome to contact the first author.
Rotational Periods of Three Main-Belt Asteroids
Pages 352-353 Ferrero, Andrea
Here are reported the result of photometric work on three asteroids: 3222 Liller, P = 12.576 ± 0.001 h, A = 0.31 mag; (8278) 1991 JJ, P = 75.028 ± 0.007 h, A = 1.50 mag; and 10111 Fresnel, P = 7.421 ± 0.001 h, A = 0.20 mag.
Index to Volume 47
Pages 354-357 Valdés-Sada, Pedro
The index to papers published in volume 47 (2020)
In This Issue
Pages 356-357 Warner, Brian D.
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.