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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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.
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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)..."
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In this paper we present one of the first lightcurves of near-Earth asteroid 2012 DA14. This is a very interesting near-Earth asteroid, which approached the Earth at a very close distance on Feb. 15 2013. From our measurements we find a rotational period of 9.485 ± 0.144 h with an amplitude of 1.79 mag.
Lightcurve Photometry, H-G Parameters and Estimated Diameter for 1412 Lagrula
Photometric observations of main-belt asteroid 1412 Lagrula were made over ten nights during 2013 March and April, with filtered system. The resulting synodic period is 5.9176 ± 0.0001 h with an amplitude of 0.28 ± 0.05 mag. The color index V-R = 0.37 ± 0.05 mag. The measured absolute visual magnitude, Hv = 11.81 ± 0.04 mag. and the slope parameter, G = 0.135 ± 0.049, are consistent with a low albedo object, e.g., type C. The diameter is estimated to be D = 23 ± 3 km.
Rotation Period Determination for 26 Proserpina, 31 Euphrosyne, and 681 Gorgo
Synodic rotation periods and amplitudes have been found for 26 Proserpina 13.109 ± 0.001 hours, 0.20 ± 0.01 mag. and 31 Euphrosyne 5.5293 ± 0.0001 hours, 0.10 ± 0.01 mag. Both results for these low numbered objects are consistent with previous findings. A new result for 681 Gorgo is a period of 6.4606 ± 0.0001 hours, amplitude 0.42 ± 0.02 mag.
The main-belt asteroid 4527 Schoenberg (1982 OK) has been observed between June 28 and July 1, 2012 at Maidanak astronomical observatory of the Ulugh Beg Astronomical Institute (UBAI), Uzbekistan Academy of Sciences. On the basis of data analysis it is found a synodic rotation period of 2.6928„b0.0384 hour (0.1122±0.0016 day) and lightcurve amplitude of 0.31±0.05 mag.
Inversion Model Candidates
Pages 190-193 Klinglesmith III, Daniel A.; Hanowell, Jesse; Risley, Ethan; Turk, Janek; Vargas, Angelica; Warren, Curtis Alan 2013MPBu...40..190KDownload PDF
We present lightcurves for ten asteroids that were selected because they are potential candidates for lightcurve inversion modeling.
Photometric observations of the main-belt asteroid 6479 Leoconnolly were made over two nights in 2013 April. Lightcurve analysis shows a synodic period of 5.11 ± 0.01 h with an amplitude of 0.75 ± 0.03 mag.
The synodic rotation period and amplitude have been found for 730 Athanasia 5.7345 ± 0.0002 hours, 0.14 ± 0.02 magnitudes, with a slightly unsymmetrical bimodal lightcurve. The period spectrum between 2.5 hours and 12.5 hours is presented, and the plausibility of all local minima in the period spectrum as potential alias periods is investigated.
Photometric observations of the main-belt asteroid 2050 Francis were made over three nights during 2013 May and June. Analysis shows a synodic period of 3.069 ± 0.001 h with an amplitude 0.20 ± 0.03 mag.
A Troop of Trojans: Photometry of 24 Jovian Trojan Asteroids
Pages 198-203 French, Linda M; Stephens, Robert, D.; Coley, Daniel R.; Wasserman, Lawrence H.; Vilas, Faith; La Rocca, Daniel 2013MPBu...40..198FDownload PDF
Lightcurves for 24 Jupiter Trojan asteroids were obtained from Cerro Tololo Inter-American Observatory, Lowell Observatory and the Center for Solar System Studies from September 2012 to May 2013.
CCD photometric observations of three Phocaea family asteroids were obtained from the Center for Solar System Studies in 2013 June. 5040 Rabinowitz has a period of 4.691 ± 0.001 h and an amplitude of 0.35 ± 0.02 mag. while 6487 Tonyspear has a period of 74.91 ± 0.02 h and an amplitude of 1.24 ± 0.02 mag., and (70126) 1999 NT2 has a period of 5.41 ± 0.01 h and an amplitude of 0.83 ± 0.03 mag.
Lightcurve Photometry, H-G Parameters, and Estimated Diameter for 15621 Erikhovland
Photometric observations of main-belt asteroid 15621 Erikhovland were made over seven nights during May and June 2013 with a filtered system. The resulting synodic period is 5.3426 ± 0.0001 h with a high amplitude of 0.81 ± 0.02 mag. The color index V-R = 0.33 ± 0.03 mag. The measured absolute visual magnitude, Hv = 12.14 ± 0.09 mag. and the slope parameter, G = 0.08 ± 0.09, are consistent with a low albedo object, e.g., type C. The diameter is estimated to be D = 20 ± 3 km.
Lightcurve of the Potentially Hazardous Asteroid (163249) 2002 GT
Photometric observations of the potentially hazardous asteroid (PHA) (163249) 2002 GT were made on 2013 June 16 and 17, before the object’s relatively close approach to the Earth. Analysis of the resulting data found a synodic period P = 3.77 ± 0.01 h with an amplitude A = 0.36 ± 0.03 mag.
We observed the main-belt asteroid (4507) 1990 FV from 2002 November to December at three observatories in eastern Asia. Its synodic rotation period turned out to be 6.58 ± 0.04 h and its lightcurve amplitude was 0.40 ± 0.03 mag when reduced to zero solar phase angle. Since our observations covered a relatively large solar phase angle range (2.3-13.7 degrees), we were able to make a phase curve to estimate the absolute magnitude (H) and slope parameter (G) in the R band: HR = 11.64 ± 0.02, GR = 0.19 ± 0.05.
Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2013 May-June
Lightcurves for eleven asteroids were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2013 May and June. The asteroids were mostly a mix of Hungaria and Phocaea members along with some outer main-belt asteroids. New data failed to remove the existing rotation period ambiguity for the Hungaria asteroid 1355 Magoeba, although the number of possibilities may have been reduced. A new period is proposed for 4436 Ortizmoreno, 8.24 h (or 16.48 h), superseding the one reported by Birlan et al. (1996). The Hungaria member 26074 Carlwirtz may be a binary with a primary rotation period of P1 = 2.5493 ± 0.0003 h and a satellite orbital period of Porb = 16.11 ± 0.02 h. The Phocaea member (125742) 2001 XT117 shows signs of a low amplitude precision period, i.e., it is possibly in nonprincipal axis rotation (NPAR).
Photometric Study of Four Asteroids at Texas A&M Commerce Observatory
Lightcurves for nine asteroids were obtained at the Palmer Divide Observatory (PDO) in 2013 February and March. These represent the final objects out of more than 1100 lightcurves measured at PDO over fourteen years. Of the nine objects reported here, six were Hungaria members, two were NEAs, and the remaining two were main belt members. Analysis of the data resulted in a revised rotation period for the Hungaria member 4531 Asaro. The near-Earth asteroid (5828) 1991 AM was found to be a possible binary system with an unusual lightcurve for the secondary period, while follow-up on known Hungaria binary 5899 Jedicke lead to a revised period for the primary and confirmation of the orbital period of the satellite.
One New and One Suspected Hungaria Binary Asteroid
CCD photometry observations were made of two Hungaria asteroids in 2013 April and May. 4765 Wasserburg was found to be a previously undiscovered binary with a primary period of 3.6231 ± 0.0005 h and a satellite orbital period of 15.97 ± 0.02. What makes this a particularly interesting find is that the asteroid is one member of an asteroid pair (Vokrouhlický and Nesvorný 2008). The suspected Hungaria binary is (12390) 1994 WB1. Data from 2013 indicate the possibility of a satellite with an orbital period of 15.94 h and a primary rotation period of 2.462 h. However, analysis of data from 2008 does not show a satellite and found a period of 15.20 h. At best, 1994 WB1 is an “asteroid of interest.”
Photometry of Minor Planets. I. Rotation Periods from Lightcurve Analysis for Seven Main-belt Asteroids
CCD photometric measurements of the main-belt asteroids 417 Suevia, 453 Tea, 904 Rockefellia, 933 Susi, 1269 Rollandia, 1318 Nerina, and 1465 Autonoma were performed during the period 2010 August to 2012 March. The brightness amplitude and synodic rotation period of the composite lightcurves are presented and commented for each asteroid.
We present shape and spin axis model for main-belt asteroid 38 Leda. The model was obtained with lightcurve inversion process, using combined dense photometric data from apparitions in 1979, 1995, 2000, 2008, 2009-10, 2011, 2012 and sparse data from USNO Flagstaff. Analysis of the resulting data found a sidereal period P = 12.836164 ± 0.000016 h and two possible pole solution at (lambda = 160°, beta = -17°) and (lambda = 343°, beta = -6°), with an error of ± 10 degrees. From sparse data from the USNO Flagstaff station we find H = 8.61 ± 0.04, G = 0.09 ± 0.04.
3 Asteroids' Lightcurve Analysis from Bassano Bresciano Observatory
Asteroids to be observed by the Target Asteroids! program during the period of July to September 2013 are presented. In addition to asteroids on the original Target Asteroids! list of easily accessible spacecraft targets, an effort has been made to identify other asteroids that are 1) brighter and, hence, easier to observe for small telescope users and 2) analogous to (101955) Bennu, the target asteroid of the OSIRIS-REx sample return mission.
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 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.
Period Determination for the Slow Rotator 2546 Libitina
Period and amplitude results for asteroid 2546 Libitina were determined from observations during 2013. The synodic rotation period was found to be 132.71 ± 0.07 h and the lightcurve amplitude was 0.35 ± 0.03 mag.
Lightcurve of 3422 Reid Using Star Subtraction Techniques
Lightcurves measurements obtained in June 2013 for asteroid 3422 Reid suggest 2.91 ± 0.02 h as an update to the rotation period. The observed amplitude was 0.52 ± 0.05 mag. A significant reduction in the point-to-point scatter within the lightcurve was achieved when star subtraction were employed to eliminate the contaminating effects of background stars.