The Minor Planet Bulletin BULLETIN OF THE MINOR PLANETS SECTION OF THE ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS
Click on image to zoom
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
1113 PSC Bldg 415
College Park, MD 20742
Authors Guide and Word Templates
(v.3.0: updated 2024 February 2)
The ZIP file contains the Authors Guide PDF as well as a "starter" paper in Word 2007+ (DOTX).
Those using Word 97 (DOC/DOT) are encouraged to download
OpenOffice and convert their files to
the most recent Word format (DOCX). Please read this updated guide since there are a number of changes from previous guides.
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.
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.
Full issues and individual papers from vol 1 (1973) to present are available via links on this page.
Important: If the ADS bibcode and "Download PDF" links are missing for the latest issue, it is because the ADS has
not processed the files. The links will be made available after the ADS processes the files.
If the "Download PDF" link is visible and there is no PDF available, clicking the link will download an arbitrary
page. We are working with ADS to make sure all papers are available and, if not, being able to diasable the link.
The "Download Full Issue" link does retrieve the correct file.
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.
Pages 373 Franco, Lorenzo; Marchini, Alessandro; Papini, Riccardo; Banfi, Massimo; Salvaggio, Fabio; Noschese, Alfonso; Becchione, Antonio; Catapano, Antonio 2019MPBu...46..373FDownload PDF
For the asteroid (37652) 1994 JS1 the absolute (R band) magnitude and slope parameter was determined from the photometric data: HR = 14.47 ± 0.02 mag, G = 0.25 ± 0.04. The slope parameter value is consistent with a medium albedo asteroid.
CCD photometric observations of the outer main-belt asteroid 1711 Sandrine were performed over eight nights between 2019 February 23 and March 31. A synodic rotation period of 33.02 ± 0.02 h and lightcurve amplitude of 0.19 ± 0.05 mag were found.
The Rotation Period of 5351 Diderot
Pages 377 Izzo, Luca; de Franciscis, Sebastiano; de Rodrigáñez, Francisco Javier Rollin Sáenz; Romero, Alvaro Castro; García, Andrés Marín; Martinez, María Sánchez; Roa, Andrea García; Antonio, José; Rodríguez, Gallego; Lopez, Paula Fabiola Freundlinger; Muñoz, Jaime Gómez; Noschese, Alfonso; Mollica, Maurizio; Vecchione, Antonio 2019MPBu...46..377IDownload PDF
We present an analysis of the rotation period of 5351 Diderot. We found a period of P = 9.99 ± 0.01 h by using data collected on five nights of observations between April 19th and April 24th. Our result independently confirms the recent finding by Marchini et al. (2019) who found a period of P = 9.984 ± 0.003 h.
A Model of Minor Planet Number Distributions: Visual Observations
In two earlier papers (Salthouse 2019a, 2019b) the author noted two specific patterns of minor planet number distributions within a large set of visual observations. These patterns revealed a strong relationship between the minor planet numbers and the total number of objects observed. The author introduces a probability model to explain this behavior.
Six Asteroids from the 2018 Mexican Asteroid Photometry Campaign
Pages 381-383 Contreras, M.E.; Olguín, L.; Loera-González, P.; Saucedo, J.C.; Schuster, W.J.; Valdés-Sada, P.; Segura-Sosa, Juan 2019MPBu...46..381CDownload PDF
We present photometric optical lightcurves and derived rotation periods for a sample of six asteroids: 767 Bondia (8.3402 ± 0.0007 h), 1229 Tilia (7.0353 ± 0.0005 h), 1475 Yalta (28.29 ± 0.01 h), 4807 Noboru (4.0415 ± 0.0005 h), 6582 Flagsymphony (70.288 ± 0.024 h), and 7305 Ossakajusto (15.3838 ± 0.0003 h). These observations were carried out at the Observatorio Astronómico Nacional at Sierra San Pedro Mártir (OAN-SPM), Baja California, México and at the Carl Sagan Observatory (OCS) of the Universidad de Sonora, México.
Lightcurve analysis using MPO Canopus was completed by University of Maryland undergraduates and faculty. Data for 2638 Gadolin were collected over four nights in 2019 April. We found the rotation period to be 7.2174 ± 0.0149 h and the lightcurve amplitude to be 0.37 mag.
Lightcurve Analysis of Five Main-Belt Asteroids: 3446 Combes, (9410) 1995 BJ1, (17780) 1998 FY13, (24491) 2000 YT 123, and 28341 Bingaman
Pages 385-386 Hayes-Gehrke, Melissa N.; Singh, Ajay; Malwitz, Andrew; Wilson, Caleb; Huang, Daniel; Nava, Diego; Yu, Iris; Chappell, Nick; Lin, Jonathan; Du, Lynn; Vijaykumar, Aishwarya; Dries, Robert; Lou, Yifan; Brincat, Stephen M.; Galdies, Charles; Grech, Winston 2019MPBu...46..385HDownload PDF
An observing campaign was conducted among teams at the University of Maryland, College Park, and in Malta to determine the rotation period of 3446 Combes during 2019 March and April. Lightcurve analysis using MPO Canopus of the asteroid was conducted in order to determine its rotation period. Using the eight nights of data, 3446 Combes was found to have a rotation period of 5.6990 ± 0.0005 h and an amplitude of 0.18 mag. The University of Maryland team also observed four additional asteroids that serendipitously appeared in the images: (9410) 1995 BJ, (17780) 1998 FY13, (24491) 2000 YT123, and 28341 Bingaman. These were observed only one night each and only the raw data for them are presented.
Lightcurve analysis using MPO Canopus of multiple nights of observations of 3816 Chugainov was unable to produce a rotation period due to a lack of fluctuations in the phased lightcurves.
Lightcurve Analysis and Rotation Period of 6372 Walker
From 2019 March-May, images of minor planet 6372 Walker were captured to investigate its rotation period. Our analysis found a period of 44.25 ±0.01 h.
Lightcurve Analysis of L5 Trojan Asteroids at the Center for Solar System Studies: 2019 April to June
We present shape and spin axis model results for mainbelt asteroid 131 Vala. The model was achieved with the lightcurve inversion process, using combined dense photometric data acquired from four apparitions, between 2007-2018 and sparse data from USNO Flagstaff. Analysis of the resulting data found a sidereal period P = 5.180810 ± 0.000023 h and two mirrored pole solutions at l = 54°, b = 29° and l = 243°, b = 30° with an uncertainty of ± 15 degrees.
Mainbelt Asteroids Lightcurve Analysis from TAR Telescope Network: 2018 October - 2019 May
Lightcurves of twelve main-belt asteroids (MBA) obtained with the Telescopio Robótico Abierto network (TAR) and the Isaac Aznar Observatory from 2018 October to 2019 May are presented and analyzed to derive the rotation period, lightcurve amplitude, and axis size relationship.
Photometric Observations of Seventeen Minor Planets
CCD photometric observations of seven Hilda asteroids were made at the Center for Solar System Studies (CS3) from 2019 April and June. Analysis of data for 1269 Rollandia and 3843 OISCA based on 2019 data led to review of our earlier results. For both objects, this resulted not in solving but deepening the mystery of the their true rotation periods.
Potential Binary and Tumbling Asteroids from the Center for Solar System Studies
CCD photometric observations of four main-belt and one near-Earth asteroid were made in 2019. Of these, the Vestoid 2602 Moore and Hungaria (27568) 2000 PT6 were confirmed to be binary asteroids. The Hungaria 3880 Kaiserman is a suspected binary. Near-Earth asteroid (142040) 2002 QE15 was found to have a long period (46.4 h). Re-evaluation of data for the asteroid from two previous apparitions found a secondary period that is consistent with the system being a candidate for the rare class of very wide binary asteroids. New analysis of the data from 2016 for Phocaea member 2937 Gibbs found two periods (the second being ambiguous). It could not be determined if the asteroid is binary or in a tumbling state.
Photometric Observations for 7 Main-belt Asteroids: 2019 February - May
Photometric observations of seven main-belt asteroids were obtained on four nights between 2019 February 13 and May 26. The following rotational periods were determined: 1551 Argelander, 4.066 ± 064 h; 1677 Tycho Brahe, 3.86 ± 0.01 h; 1774 Kulikov, 3.823 ± 0.001 h; 2564 Kayala, 3.01 ± 0.01 h; 26355 Grueber, 4.495 ± 0.028 h; and (47369) 1999 XA88, 2.56 ± 0.09 h. No well-defined period could be derived for 11155 Kinpu.
Here we present the result of an observing campaign for asteroid 349 Dembowska. In addition to period determination, we show how to use the result to determine absolute magnitude using the H-G system and how to derive the diameter for an equivalent spherical shape.
Near-Earth Asteroid Lightcurve Analysis at the Center for Solar System Studies
Lightcurves for 38 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2019 March-July were analyzed for rotation period, peak-topeak amplitude, and signs of satellites or tumbling.
Lightcurve Analysis, Rotation Period and H-G Parameters Determination for 2727 Paton
Data for asteroid 2727 Paton were collected from February 5th to March 4th 2019. The lightcurve analysis obtained has led to a bimodal curve with a period of 5.325 ± 0.001 h, amplitude 0.26 mag, with a full coverage. We have also obtained data in V and Rc filters, alternately, for color index V-R found to be 0.50 ±0.06 mag. Maximum reduced magnitudes have been extrapolated from each session in order to determine H and G parameters, found to be, respectively, 12.46±0.05 mag and 0.25 ±0.09 mag. Values found are consistent with an S-type taxonomy.
Collaborative Asteroid Photometry from UAI: 2019 May-June
Photometric observations of four main-belt and one near-Earth
asteroids were made in order to acquire lightcurves for shape/spin
axis models. The synodic period and lightcurve amplitude were found
for: 234 Barbara: 26.482 ± 0.006 h, 0.21 mag; 1166 Sakuntala: 6.2918 ±
0.0006 h, 0.24 mag.; 1914 Hartbeespoortdam: 6.3398 ± 0.0006 h, 0.10
mag; 2433 Sootiyo: 7.235 ± 0.005 h, 0.35 mag; (66391) 1999 KW4: 2.7644
± 0.0002 h, 0.15 mag. We also confirmed the binary nature of the
asteroid (66391) 1999 KW4.
This paper presents the results of photometric observations with standard broad-band Bessel filters B, V, R and I, on near-Earth asteroid (66391) 1999 KW4. The analysis shows that the mean color indices are the following: B-V = 0.85 ± 0.01 mag, V-R = 0.44 ± 0.02 mag, B-R = 1.29 ± 0.01 mag and V-I = 0.65 ± 0.03 mag.
New Lightcurves of 50 Virginia, 57 Mnemosyne, 59 Elpis, 194 Prokne, 444 Gyptis, and 997 Priska
Minor planet 1744 Harriet has a synodic rotation period near 724 hours, amplitude increasing from 0.95 ± 0.05 magnitudes to 1.10 ± 0.05 magnitudes.
Lowell Observatory Near-Earth Asteroid Photometric Survey (NEAPS): Paper 4
Pages 458-503 Skiff, Brian A.; McLelland, Kyle P.; Sanborn, Jason J.; Pravec, Petr; Koehn, Bruce W. 2019MPBu...46..458SDownload PDF
Revised photometry and lightcurves are reported for 144 asteroids from the NEAPS project and later work at Lowell Observatory. This completes revision of objects from Paper 1 and 2 and adds previously unpublished data acquired between 2008 and 2019. In several cases we provide lightcurves over several lunations within an apparition and also at multiple apparitions with different phase-angle bisectors.
Collaborative Asteroid Photometry for 3653 Klimishin, 4748 Tokiwagozen and 9951 Tyrannosaurus
Pages 504-505 Marchini, Alessandro; Franco, Lorenzo; Papini, Riccardo; Banfi, Massimo; Salvaggio, Fabio; Galdies, Charles; Brincat, Stephen M. 2019MPBu...46..504MDownload PDF
Photometric observations of three main-belt asteroids were made in order to acquire lightcurves. The synodic period and light curve amplitude were found for: 3653 Klimishin 6.783 ± 0.001 h, 0.21 mag; 4748 Tokiwagozen 39.78 ± 0.01 h, 0.42 mag.; 9951 Tyrannosaurus 3.767 ± 0.004 h, 0.21 mag. Asteroid 4748’s lightcurve shows a few interesting features which suggest the opportunity of further observations in order to verify a possible ”tumbling” nature.
Lightcurves and Synodic Rotation Periods for Seven Asteroids: 2019 April-July
Results are given on lightcurve and synodic rotation period determinations for seven asteroids from data collected at Sopot Astronomical Observatory between 2019 April to July.
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 also include lists of objects that will or might be radar targets. 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.
