The Minor Planet Bulletin

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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.

Print subscriptions are no longer available to individuals. Institutions (e.g., college libraries) can still obtain print copies via a special subscription. See details in MPB 37-4 or contact the editor, Richard Binzel.

Annual voluntary contributions of $5.00 or more in support of the publication are welcome.
Please send a check, drawn on a U.S. bank and payable in U.S. funds, to "Minor Planet Bulletin" and send it to:

Minor Planet Bulletin
c/o Melissa Hayes-Gehrke
UMD Astronomy Department
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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. For example,
  • 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)..."

Cumulative Index to Volumes 1-45
Cumulative Asteroid Lightcurve Index (Volumes 1 through 46-2)

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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.

Volume 47 (2020)

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Issue 47-1 (2020 Jan-Mar)
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Collaborative Asteroid Photometry for Asteroid 2051 Chang
Pages 1-2
Marchini, Alessandro; Papini, Riccardo; Banfi, Massimo; Salvaggio, Fabio; Hayes-Gehrke, Melissa N.; Yates, Eric

Photometric observations of this main-belt asteroid were conducted in order to determine its rotation period. The authors found a synodic rotation period of 12.013 ± 0.001 h and a light curve amplitude of 0.64 ± 0.01 mag.

Section News: Staffing Changes for the Minor Planet Bulletin
Pages 1
Pilcher, Frederick

One staffing change and one staffing addition for The Minor Planet Bulletin are announced effective with this issue.

Measured Lightcurves and Rotational Periods of 3122 Florence, 3830 Trelleborg, and (131077) 2000 YH105
Pages 3-4
Abrams, Natasha S.; Bieryla, Allyson; Gomez, Sebastian; Huang, Jane; Lewis, John A. ; Garrison, Lehman H.; Carmichael, Theron

We determined the rotational periods of 3122 Florence, 3830 Trelleborg, and (131077) 2000 YH105 with the Harvard Clay Telescope and KeplerCam at the Fred L. Whipple Observatory. We found the rotational periods to be 2.3580 ± 0.0015 h, 17.059 ± 0.017 h, and 1.813 ± 0.00003 h, respectively. Our measurement of 3122 Florence’s period agrees with Warner (2016), who reported 2.3580 ± 0.0002 h.

Rotational Period Determination For Asteroids 2460 Mitlincoln, 3070 Aitken and (11116) 1996 EK
Pages 5-6
Mannucci, Massimiliano; Montigiani, Nico

CCD photometric observations of three main-belt asteroids were obtained in order to measure their rotation period. These measures were performed during several nights from 21/3/2019 to 6/5/2019, using the instrumentation available at the Osservatorio Astronomico Margherita Hack located on the hills near Florence (Italy).

Twelve Main Belt Asteroids, One Near Earth and One Potentially Hazardous Asteroid Lightcurves at Asteroids Observers (OBAS) – MPPD: 2017 May-2019 Jan
Pages 7-10
Carreño, Alfonso; Fornas, Gonzalo; Arce, Enrique; Mas, Vicente

We report on the photometric analysis result of twelve main-belt asteroids (MBA), one near-Earth asteroid (NEA) and one potentially hazardous asteroid (PHA) 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.

Rotation Period Determination for Asteroid 2602 Moore
Pages 11
Casalnuovo, Giovanni Battista; Chinaglia, Benedetto

Photometric observations of main-belt asteroid, 2602 Moore, were made at the Filzi School Observatory (School in country Laives - Italy). Results of lightcurve analysis are presented.

Photometric Observations of Main-Belt Asteroid (10422) 1999 AN22
Pages 12
Brincat, Stephen M.; Hills, Kevin; Galdies, Charles

Photometric observations of main-belt asteroid (10422) 1999 AN22 were obtained from May 20 to July 09, 2019, in order to determine its synodic rotation period. Observations were acquired from two observatories in Malta and one from Spain. Through our observational campaign, we present our results obtained for this asteroid that were based on 30 sessions.

Photometric Observations of Ten Minor Planets
Pages 13-17
Polakis, Tom

Phased lightcurves and synodic rotation periods are presented for eight main-belt asteroids. Results are: 243 Ida, 4.634 ± 0.002 h; 874 Rotraut, 14.311 ± 0.010 h; 1686 De Sitter, 11.292 ± 0.012 h; 2285 Ron Helin, 52.77 ± 0.07 h; 2302 Florya, 16.557 ± 0.024 h; 3306 Byron, 6.999 ± 0.005 h; 5391 Emmons, 3.029 ± 0.001 h; and 7365 Sejong, 2.579 ± 0.001 h. No period solutions were found for 1466 Mundleria or 5199 Dortmund. All the data have been submitted to the ALCDEF database.

Photometric Observations of 2096 Vaino and 5104 Skripnichenko
Pages 18-19
Fauerbach, Michael; Fauerbach, Matthew

Photometric observations of 2096 Vaino and 5104 Skripnichenko were obtained on two nights, 2019 July 3 and 29. The following rotational periods were determined: 2096 Vaino, 5.55 ± 0.01 h, amplitude 0.10 ± 0.02; 5104 Skripnichenko, 2.84 ± 0.01 h, amplitude 0.22 ± 0.02.

Rotational Period Determination of Two Main Belt Asteroid: 4807 Noboru and 1435 Garlena
Pages 20
Tomassini, Angelo; Scardella, Maurizio; Franceschini, Francesco; Pierri, Fernando

The main-belt asteroids 4807 Noboru and 1435 Garlena have been observed over several nights throughout December 2018 to February 2019 in order to determine their synodic rotational periods.

Trappist-North and -South Combined Lightcurves of Near-Earth Asteroid 3122 Florence
Pages 21-22
Ferrais, Marin; Jehin, Emmanuël; Moulane, Youssef; Pozuelos, Francisco J.; Barkaoui, Khalid; Benkhaldoun, Zouhair

A long lightcurve of the near-Earth asteroid 3122 Florence was obtained by combining observations from the TRAPPIST-South (TS) and TRAPPIST-North (TN) telescopes during the night of 2017 September 3. We found its synodic rotation period and amplitude to be 2.352 ± 0.005 h and 0.19 mag. All the data have been submitted to the ALCDEF database.

Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies: 2019 July-September
Pages 23-34
Warner, Brian D.; Stephens, Robert D.

Lightcurves for 28 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2019 July to September were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling. 2059 Baboquivari, (90403) 2003 YE45, and 2016 AU130 are candidates for membership within the very wide binary asteroids class. The 2019 data led to a seemingly unambiguous period of 4.7906 h for (441987) 2010 NY65, which overturned previous results that have now been updated.

Lightcurves and Rotation Periods of 33 Polyhymnia, 206 Hersilia, 395 Delia, 400 Ducrosa, 900 Rosalinde, and 1066 Lobelia
Pages 34-36
Pilcher, Frederick

Synodic rotation periods and amplitudes are found for 33 Polyhymnia: 18.602 ± 0.001 h, 0.25 ± 0.02 mag; 206 Hersilia: 11.113 ± 0.002 h, 0.17 ± 0.01 mag; 395 Delia: 19.681 ± 0.001 h, 0.16 ± 0.02 mag; 400 Ducrosa: 6.8678 ± 0.0001 h, 0.57 ± 0.03 mag; 900 Rosalinde: 16.689 ± 0.001 h, 0.29 ± 0.02 mag; and 1066 Lobelia: 5.0176 ± 0.0001h, 0.42 ± 0.02 mag.

Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2018 September – 2019 September
Pages 37-41
Warner, Brian D.; Stephens, Robert D.

CCD photometric observations of three Hilda asteroids were made at the Center for Solar System Studies (CS3) in 2019 September. Analysis of the 2019 data for 4495 Dassanowsky, a reported binary (Warner and Stephens, 2019), found three periods, one being very long (431 h). The long period and a secondary one made it a potential member of the very wide binary asteroids but, for the first time for a member of this class, a third period seems to be present. A review of the 2018 data set using comparison star magnitudes from the ATLAS catalog (Tonry et al., 2018) found the previously unnoticed very long period. The secondary and tertiary periods were still in good agreement with the original two-period solution found in 2018. Though the odds are remote and considerable more data are required, the new results from the 2018 data are encouraging in the on-going effort to find evidence that validates claims of the existence of the very wide binary asteroid class.

Asteroid-DeepSky Appulses in 2020
Pages 42
Warner, Brian D.

The following list is a very small subset of the results of a search for asteroid-deepsky appulses for 2020, presenting only the highlights for the year based on close approaches of brighter asteroids to brighter DSOs.

Lightcurve Analysis of L4 Trojan Asteroids at the Center for Solar System Studies: 2019 July To September
Pages 43-47
Stephens, Robert D.; Warner, Brian D.

CCD Photometric observations of 11 Trojan asteroids from the L4 (Trojan) Lagrange point were obtained at the Center for Solar System Studies (CS3, MPC U81). For several years, CS3 has been conducting a study of Jovian Trojan asteroids. This is another in a series of papers reporting data analysis being accumulated for family pole and shape model studies. It is anticipated that for most Jovian Trojans, two to five dense lightcurves per target at oppositions well distributed in ecliptic longitudes will be needed and can be supplemented with reliable sparse data for the brighter Trojan asteroids. For all of these targets we were able to get preliminary pole positions and create shape models from sparse data and the dense lightcurves obtained to date. These preliminary models will be improved as more data are acquired at future oppositions and will be published at a later date.

Minor Planets at Unusually Favorable Elongations in 2020
Pages 47-49
Pilcher, Frederick

A list is presented of minor planets which are much brighter than usual at their 2020 apparitions.

Main-belt Asteroids Observed from CS3: 2019 July to September
Pages 50-60
Stephens, Robert D.; Warner, Brian D.

CCD photometric observations of 25 main-belt asteroids were obtained at the Center for Solar System Studies (CS3) from 2019 July to September.

Collaborative Asteroid Photometry from UAI: 2019 July-September
Pages 61-63
Franco, Lorenzo; Marchini, Alessandro; Arena, Claudio; Casalnuovo, Giovanni Battista; Chinaglia, Benedetto; Valvasori, Adriano; Bacci, Paolo; Maestripieri, Martina; Baj, Giorgio; Galli, Gianni

Photometric observations of five main-belt and one near-Earth asteroid were made in order to acquire lightcurves for shape/spin axis models. The synodic period and lightcurve amplitude were found for: 289 Nenetta, 6.916 ± 0.001 h, 0.19 mag; 472 Roma, 9.792 ± 0.002 h, 0.29 mag.; 635 Vundtia, 11.794 ± 0.002 h, 0.21 mag; 869 Mellena, 6.528 ± 0.008 h, 0.30 mag; 2131 Mayall, 2.5677 ± 0.0001 h, 0.08 mag; 2019 NN3, 0.03750 ± 0.00003 h, 0.98 mag. We also confirmed the binary nature of the asteroid 2131 Mayall.

Rotational Periods of Five Asteroids
Pages 64-65
Ferrero, Andrea; Bonamico, Roberto

Here we present the result of a photometric work on five asteroids: 2548 Leloir, P = 3.206 ± 0.001 h, A = 0.15 mag; 6527, P = 3.016 ± 0.002 h, A = 0.22 mag; 7527 Marples, P = 9.091 ± 0.002 h, A = 0.46 mag; (58285) 1993 YN, P = 51.81 ± 0.02 h, A =0.43 mag; (354030) 2001 RB18, P = 13.27 ± 0.02 h, A = 0.11 mag.

Rotational Properties of Three Hilda Asteroids
Pages 66-68
Williamson, B.; Sonnett, S.; Witry, J.; Chatelain, J.; Grav, T.; Reddy, V.; Lejoly, C.; Kramer, E.; Mainzer, A.; Masiero, J.; Gritsevich, M.; Bauer, J.

We determine the rotation periods, lightcurve amplitudes, and H-G parameters for three Hilda asteroids with previously measured large brightness variations. We measured a rotation period of 8.4070 ± 0.0009 h and amplitude of 0.64 ± 0.04 R-mag, HR = 14.56 ± 0.03 mag, and GR = 0.44 ± 0.08 for (64390) 2001 UY149. For (16927) 1998 FX68, we measure a rotation period of 33.85 ± 0.07 h, an amplitude of 0.68 ± 0.04 R-mag, HR = 12.02 ± 0.06 mag, and GR = 0.7 ± 0.2. For (209512) 2004 RO2, we determine a rotation period of 15.78 ± 0.02 h, an amplitude of 0.30 ± 0.04 r’ mag, Hr’ = 15.40 ± 0.06 magnitudes, and Gr’ = 0.4 ± 0.1.

Rotation Period Determination for Asteroids 3295 Murakami and 4961 Timherder
Pages 69-70
Marchini, Alessandro; Bernardi, Eleonora; Saya, Leonella Filippa; Papini, Riccardo; Banfi, Massimo; Salvaggio, Fabio

Photometric observations of two main-belt asteroids were conducted from the Astronomical Observatory of the University of Siena and the Wild Boar Remote Observatory, both located in Italy, in order to determine the synodic rotation periods for the asteroids. For 3295 Murakami we found P = 3.534 ± 0.002 h, A = 0.14 ± 0.02 mag; for 4961 Timhelder we found P = 4.121 ± 0.001 h, A = 0.45 ± 0.02 mag.

Lightcurves of Six Asteroids from 2018 December Through 2019 April
Pages 71-73
Lang, Kim

Lightcurves of six asteroids were obtained from 2018 December through 2019 April. Synodic periods and amplitudes were found for: 4148 McCartney, P = 20.799 ± 0.002 h, A = 0.27 mag; 4807 Noboru, P = 4.0415 ± 0.0005 h, A = 0.19 mag; 6843 Heremon, P = 8.2875 ± 0.002 h, A = 0.16 mag; and (7520) 1990 BV, P = 3.826 ± 0.002 h, A = 0.32 mag. For asteroids 5522 De Rop and (12416) 1995 TS, no definitive periods could be determined.

Lightcurve for Asteroid 4717 Kaneko
Pages 74
Singh, Ajay; Sackalosky, Corey; Sefik, Yavuz; Yates, Eric; Moore, Conor; Pagan, Alyssa; Malwitz, Andrew

A team of observers associated with the University of Maryland, College Park conducted observations to determine the rotation period of 4717 Kaneko. Lightcurve analysis using MPO Canopus on photometric data retrieved from multiple nights of observations was conducted in order to determine its rotation period. Using seven nights of data, 4717 Kaneko was found to have a rotation period of 12.7082 ± 0.0113 h and an amplitude of 0.61 mag.

Asteroid Photometry at Sopot Astronomical Observatory: 2019 June-October
Pages 75-83
Benishek, Vladimir

A summary on the lightcurve and synodic rotation period determinations for 29 asteroids observed at Sopot Astronomical Observatory form 2019 June-October is presented in this paper.

Lightcurve Photometry Opportunities: 2020 January-March
Pages 83-87
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.

In This Issue
Pages 87-88
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.

copyright©2017 Brian D. Warner. Funding to support this web site is provided by NASA grant NSSC 80NSSC18K0851