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.
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:
Derald D. Nye
Minor Planet Bulletin
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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.
Earlier volumes often contain more papers than listed here. It's recommended to download the
full issue in vol 1-9.
CCD photometric observations of minor planet 1969 Alain by the T17 Telescope in Siding Spring, Australia in March and April 2017 were combined for lightcurve analysis. The combined data set led to a rotation period of P = 32.4 ± 0.4 h.
Lightcurve and Rotational Period Determination for Main Belt Asteroid (13538) 1991 ST
The synodic rotation period has been determined for the near-Earth asteroid (NEA) (143404) 2003 BD44. The asteroid was observed during three intervals with a rotation period on the order of 79 h determined in each case. The lightcurve exhibited rapidly changing morphology as the asteroid approached. Data have submitted to the ALCDEF database.
Lightcurve Analysis for Minor Planet 1581 Abanderada
From 2017 April 8 to 2017 June 9, CCD images were taken with the aim to determine the rotation period of 1581 Abanderada. The data analysis gives a light curve with a rotation period of 102.8 ± 0.1 hours.
Asteroids Lightcurves Analysis: 2016 November - 2017 June
Twelve near-Earth asteroids were observed from 2016 November through 2017 June to find the synodic rotation period and lightcurve amplitudes for each asteroid. Results are reported for 2329 Orthos, (138846) 2000 VJ61, (326683) 2002 WP, (489337) 2006 UM, (494706) 2005 GL9, 2005 TF, 2017 BJ30, 2017 BQ6, 2017 CS, 2017 DC36, 2017 GK4, and 2017 JA2.
Rotational Period Determination of Two Mars-crossing, a Main Belt Asteroid and a PHA: (14309) Defoy, (56116) 1999 CZ7, (5813) Eizaburo and (3122) Florence.
The main-belt asteroids (5813) Eizaburo and two Mars crossing minor bodies, (14309) Defoy and (56116) 1999 CZ7, have been observed over several nights throughout 2017 March-September in order to determine their synodic rotational period. We also took the opportunity of the (3122) Florence close passage with the Earth in September-October to find its lightcurve.
Lightcurve Analysis of Minor Planets Observed at the Oakley Southern Sky Observatory: 2016 October - 2017 March
Photometric observations of the main-belt asteroids 5813 Eizaburo and (11745) 1999 NH3 performed made in 2017 August revealed a bimodal lightcurve phased to 2.876 ± 0.002 h for 5813 Eizaburo and 3.280 ± 0.001 h for (11745) 1999 NH3 as the most likely synodic rotational periods for these asteroids.
Sixteen sessions on 576 Emanuela 2017 Feb. 17 – Apr. 4 provide equally good fits to synodic rotation periods of 20.404 ± 0.003 hours with one maximum and minimum per cycle and 40.812 ± 0.004 hours with a nearly symmetric and somewhat irregular bimodal lightcurve, with amplitude 0.13 ± 0.01 magnitudes.
Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2017 July Through October
Lightcurves for 37 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2017 July through October were analyzed for rotation period and signs of satellites or tumbling. (6053) 1993 BW3 was found to have an ambiguous solution that was resolved to 2.5737 h by using split-halves plots (see Harris et al., 2014). Data from 2016 for (141354) 2002 AJ29 were re-examined in light of new, independent results (Vaduvescu et al., 2017; 10.754 h). The 2016 data now lead to a revised period of 10.801 h. Recent results for (12538) 1998 OH by Vaduvescu et al. (2017, 2.58 h) prompted a reexamination of CS3 data from 2014 and 2016 with the result that the more recent period of 5.151 h (Warner, 2017a) is still more likely correct. Analysis of (66146) 1998 TU3 indicates it is a possible binary asteroid with P1 = 2.37760 h and PORB = 13.58 h. 2012 TC4 and 2017 NH were both found to be tumbling asteroids with short periods and large amplitudes.
Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2017 July Through September
Lightcurves for ten Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2017 July through September. One, (457175) 2008 GO98, was found to be a comet by Leonard (2017). Numerous confirmation reports were made (Green, 2017) but our rotation period of 10.74 hours appears to be the only one reported.
Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2017 July Through October
Lightcurves for 17 main-belt asteroids were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2017 July through October. All but two of the asteroids were targets of opportunity, i.e., in the field of planned targets, demonstrating a good reason for data mining images.
We report on the photometric analysis result of seven near-Earth asteroids (NEA) 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.
Lightcurve Analysis of L4 Trojan Asteroids at the Center for Solar System Studies 2017 July - September
The lightcurves of main-belt asteroids 963, 1025, 2019, and 17814 and near-Earth asteroids (NEAs) 459872, 2014 JO25, and 2017 BS32 were obtained using Xingming Observatory (Code C42) from 2016 March to 2017 March. The absolute magnitudes of these asteroids range from H = 11.6 to 27.3, corresponding to a diameter range of ~14 m to 14 km. The derived synodic rotation periods range between 0.1 to 10 h.
Lightcurve Analysis for Minor Planet 138925 2001 AU43
From 2017 July 27-30, CCD images were collected with the aim to determine the rotation period of (138925) 2001AU43. The data analysis gives a complex lightcurve with a rotation period of 5.251 ± 0.001 h.
During 2017 August and September, we observed five spin-shape asteroids: 418 Alemannia, 1095 Tulipa, 2648 Owa, 3122 Florence, and 5040 Rabinowitz. The selections were by listed by Warner et al. (2017) in their regular MPB paper featuring photometric opportunities for the upcoming quarter.
Photometry of the Damocloid asteroid 2006 BZ8 was obtained on two
nights in 2006 February with the University of Arizona Kuiper
1.54-m telescope. Lightcurve analysis yielded a rotation period
of 5.960 ± 0.003 h and amplitude of 0.35 magnitudes. An analysis
of photometry reported by the Catalina Sky Survey, Mount Lemmon
Survey. and Siding Spring Survey to the Minor Planet Center found
a steep phase function slope of βV = 0.054 ± 0.008 which is
consistent with 2006 BZ8 being a very low albedo object.
Period Determination for (23621) 1996 PA, (29564) 1998 ED6, and (31775) 1999 JN122
Photometric observations of three asteroids were conducted from the Astronomical Observatory of the University of Siena (Italy) in order to determine their synodic rotation periods. For (23621) 1996 PA, a Marscrosser asteroid, we found a period of 2.666 ± 0.001 h with an amplitude of 0.10 mag. For the two main-belt asteroids (29564) 1998 ED6 and (31775) 1999 JN122, we found, respectively, a period of 8.434 ± 0.002 h with an amplitude of 0.57 mag and a period of 4.319 ± 0.01 h with an amplitude of 0.12 mag.
Rotation Period Determination for 8994 Kashkashian, (25980) 2001 FK53 and (29128) 1985 RA1
Photometric observations of three main-belt asteroids were made from the Astronomical Observatory of the University of Siena (Italy) in order to determine their rotation periods. For 8994 Kashkashian, we found a period of 11.761 ± 0.001 h with an amplitude of 0.24 ± 0.01 mag. For (25980) 2001 FK53 the period was 2.762 ± 0.002 h with an amplitude of 0.10 ± 0.02 mag. For (29128) 1985 RA1 we found a period of 5.056 ± 0.004 h with an amplitude of 0.18 ± 0.04 mag.
Lightcurve Analysis for Minor Planets 1322 Coppernicus and 9148 Boriszaitsev
From 2017 March 16 to 2017 June 23, CCD images were taken with the aim to measure the rotation period of 1322 Coppernicus and 9148 Boriszaitsev. The data analysis gives a lightcurve with a rotation period of 8.125 ± 0.009 hours for Boriszaitsev, in agreement with other measurement recently published. On the contrary, the rotation period of 4.354 ± 0.005 measured for 1322 Coppernicus is rather different than the previous data collected in 1991 and 2006.
Koronis Family Member (3032) Evans: Photometric Reconnaissance and Lightcurves in 2008, 2009, and 2016
We observed rotation lightcurves of (3032) Evans during three apparitions using the 0.6-m telescope at Whitin Observatory. The lightcurve amplitude was consistently rather low (~ 0.15 mag.) during all three apparitions, and although we can construct credible doubly-periodic composite lightcurves from our data, we discuss why we favor a rotation period of 3.3970 ± 0.0002 h even though the resulting composite lightcurves are quadruply periodic. The observations from 2008 are calibrated to a standard system, enabling us to measure the absolute magnitude HR, slope parameter GR, and V–R color, from which we calculate H = 11.75 ± 0.05.
The Rotation Period of 1773 Rumpelstilz is Reexamined
Analysis of forty-one sessions of CCD photometric observations on 1773 Rumpelstilz obtained from 2017 Jan 9 through Apr 10 provide a good fit to a synodic rotation period of 105.44 ± 0.01 hours with a bimodal lightcurve of amplitude 0.62 ± 0.04 magnitudes.
Twenty-one Asteroid Lightcurves at Asteroids Observers (OBAS) - MPPD: Nov 2016 - May 2017
We report on the analysis of photometric observations of 21 main-belt asteroids (MBA) done by Asteroids Observers (OBAS). This work is part of the Minor Planet Photometric Database task 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.
Lightcurve and Rotation Period Determinations for 29 Asteroids
Lightcurves of six Mars-crossing and eight main-belt asteroids were obtained at APT-Observatory Group from 2017 April to September. In addition, two more asteroids were captured in 2014 and 2015 during the EURONEAR project. Analysis of rotation period, lightcurve amplitude, and physical parameters (size and axis size relationship) are presented.
The near-Earth asteroid (NEA) 1993 RA was observed with the 2.5-m Isaac Newton Telescope (INT) in full Moon conditions for 8h total during three successive nights (2017 Oct 3-6). The composite lightcurve could be fit by a 3-order period P = 5.64 ± 0.01 h with amplitude of 0.13 mag; other solutions are possible.
The Minor Planet Bulletin home page has a new URL: http://www.MinorPlanet.info/MPB/mpb.php. The new home page features free access (data rates may apply) to almost all papers from Volume 1 (1973) to present. Also included are a basic search feature that allows finding papers by title/abstract and/or authors and links to download the MPB authors guide and cumulative indices.
Minor Planets at Unusually Favorable Elongations in 2018
The following list is a very small subset of the results of a
search for asteroid-deepsky appulses for 2018, presenting only
the highlights for the year based on close approaches of brighter
asteroids to brighter DSOs. The complete set of predictions is
available at http://www.minorplanet.info/ObsGuides/Appulses/DSOAppulses.htm
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.