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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Minor Planet Bulletin
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Issue 44-3 (2017 Jul-Sep)
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Certainties, Question Marks and Voids in the Present-day Data Concerning the Rotation Period of Asteroids
Pages 167-171
Alvarez, Eduardo Manuel
2017MPBu...44..167A    Download PDF

There are more than 700,000 asteroids with well-defined orbits. However, the LCDB data base (version Feb 2017) contains rotation period data for only 17,437 asteroids and yet, more than two thirds of those reported measurements still may be uncertain by 30% (U = 2) and another 10% may be completely wrong (U = 1). It should be possible to know the characteristics of asteroid spins without measuring every last one of them, on condition that our sample (1) is unbiased, and (2) it properly includes odd or outlier objects. In principle, U = 2 data should be good enough for both statistical analysis and for identifying oddballs. Wide-field data now comprise the majority (~63%) of spin rates we have. However, due to the overwhelming volume of W-F data, their corresponding reliability is in practice almost impossible to assess on a case-by-case basis, so that a nominal U = 2 has been basically assigned to them. This poses the question whether including W-F data actually improves or degrades statistical analysis performed using only the smaller but more carefully controlled data from the F-D file. This paper shows that for size ranges where both F-D and W-F data samples contains at least 100 values, the W-F mean significantly differs from the F-D value (with only one exception for the narrow range 1 < D < 0.7 km, where W-F data appears to be as almost unbiased). The spin rate percent difference for asteroids having diameters between 3 to 20 km is consistently uniform, and worsens for larger ones. With respect to studies of extremes of rotation, W-F surveys and less controlled samples can be useful, if the limitations are reasonably characterized.

Rotation Period of Asteroid 3494 Purple Mountain
Pages 171-172
Kosiarek, M.; Nisley, I.; Patra, K.; Hatano, R.; Bates, H.; Chavez, E.; Kosiarek, J. L.; Kumari, S.
2017MPBu...44..171K    Download PDF

Data for asteroid 3494 Purple Mountain were collected from 2015 June 25 to 2015 August 17. The rotation period was determined to be 2.928 ± 0.0012 h.

Lightcurve Analysis of Asteroids Observed at the Oakley Southern Sky Observatory: 2016 July - October
Pages 173-176
Linville, Dylan; Jiang, Hao; Michalik, Danielle; Wilson, Sydney; Ditteon, Richard
2017MPBu...44..173L    Download PDF

On forty individual nights from 2016 July 29 to October 9, CCD images were taken in order to collect photometric data for 25 asteroids: 850 Altona, 1267 Geertruida, 1599 Giomus, 1945 Wesselink, 2280 Kunikov, 2428 Kamenyar, 2562 Chaliapin, 2989 Imago, 3038 Bernes, 3777 McCauley, 4103 Chahine, 4336 Jasniewicz, 4405 Otava, 4438 Sykes, 5937 Loden, 7389 Michelcombes, 9033 Kawane, 10287 Smale, 11003 Andronov, 11787 Baumanka, (14686) 1999 XA174, 17770 Baume, (18977) 2000 QK217, (21101) 1992 OJ1, and (69081) 2003 AZ64.

Photometric Observations of the Near-Earth Asteroids (326683) 2002 WP and 2016 LX48
Pages 176-177
Sonka, Adrian Bruno; Popescu, Marcel; Nedelcu, Dan Alin; Gherase, Radu Mihai; Vass, Gheroghe
2017MPBu...44..176S    Download PDF

We obtained photometric results for the near-Earth asteroids (326683) 2002 WP and 2016 LX48 during their close approaches in 2016 December and October, respectively. Our analysis found a synodic period for (326683) 2002 WP of P = 6.2772 ± 0.0479 h and, for 2016 LX48, P = 5.6742 ± 0.0074 h.

Lightcurve Analysis for Minor Planet 703 Noemi
Pages 177-178
Noschese, Alfonso; Vecchione, Antonio; D'Avino, Luca; Izzo, Lucca
2017MPBu...44..177N    Download PDF

CCD images were taken of asteroid 703 Noemi from 2016 November 16 to 2017 January 31 to determine its rotation period. The data analysis gives a complex light curve with a rotation period of 201.7 ± 0.7 hours.

Lightcurve Analysis for Ten Main Belt Asteroids
Pages 178-180
Casalnuovo, Giovanni Battista
2017MPBu...44..178C    Download PDF

Photometric observations of ten main-belt asteroids, 2854 Rawson, 3113 Chizhevskij, 5318 Dientzenhofer, (5563) 1991 VZ1, 7143 Haramura, 10421 Dalmatin, (11386) 1998 TA18, (18429) 1994 AO1, (23496) 1991 VN3, and (31782) 1999 KM6 were made at the Eurac Observatory (MPC C62). Results of lightcurve analysis are presented.

The Rotation Periods of Asteroids 4668 Rayjay, 5152 Labs, 6581 Sobers, and 14917 Taco
Pages 181-182
Odden, Caroline E.; Jusuf, James M.; Keefe, Olivia, R.; Wang, Andrew; Zaeder, Eliot A.
2017MPBu...44..181O    Download PDF

Photometric observations of four asteroids were made over 14 nights from 2016 September to November. The measured synodic periods were: 4668 Rayjay, 6.506 ± 0.001 h; 5152 Labs, 3.8801 ± 0.0001 h; 6581 Sobers, 6.635 ± 0.001 h; and 13917 Taco, 9.7078 ± 0.0001 h.

Rotation Period Determination for 467 Laura
Pages 183
Pilcher, Frederick; Benishek, Vladimir
2017MPBu...44..183P    Download PDF

We find for 467 Laura a synodic rotation period of 70.63 ± 0.01 hours, amplitude 0.15 ± 0.02 magnitudes.

Lightcurve Analysis of Asteroids Observed at the Oakley Southern Sky Observatory: 2016 October
Pages 184-185
Washburn, Kyle; Ditteon, Richard
2017MPBu...44..184W    Download PDF

On seven individual nights between 18 October 2016 and 27 October 2016, CCD images were taken of five asteroids: 2541 Edebono, 2977 Chivilikhin, 5623 Iwamori, (16806) 1997 SB34, and (58143) 1983 VD7. These images were calibrated and measured, and lightcurves were produced for each asteroid.

Rotation Period for 1218 Aster
Pages 185-186
Franco, Lorenzo; Klinglesmith, Daniel A. III; Pilcher, Frederick
2017MPBu...44..185F    Download PDF

A collaborative campaign of lightcurve photometry of main-belt asteroid 1218 Aster was made over six nights in 2017 Jan-Feb. The resulting synodic rotational period is 3.1581 ± 0.0001 h, amplitude 0.30 ± 0.02 mag. From photometric sparse data we derived H = 13.44 ± 0.04 and G = 0.43 ± 0.05.

1943 Anteros: A Possible Near-Earth Binary Asteroid
Pages 186-188
Warner, Brian D.; Benishek, Vladimir; Harris, Alan W.
2017MPBu...44..186W    Download PDF

A collaboration of two observers at widely-separated longitudes made CCD photometric observations of the near-Earth asteroid (NEA) 1943 Anteros from 2016 August to October. Analysis of the data led to the possibility that the asteroid is a binary with P1 = 2.86923 ± 0.00006 h, A1 = 0.07 mag and PORB = 23.548 ± 0.002 h, A2 = 0.05-0.10 mag. The estimated effective diameter ratio is Ds/Dp . 0.22 ± 0.02.

CCD Lightcurves for Main-belt Asteriods 423 Diotima and 925 Alphonsina
Pages 188-189
Alton, Kevin B.
2017MPBu...44..188A    Download PDF

Fourier analysis of a new CCD-derived lightcurves found synodic periods for 423 Diotima (4.775 ±0.001 h) and 925 Alphonsina (7.879 ± 0.001 h).

The Lightcurve Period for the Asteroid 201 Penelope
Pages 190
Mizoguchi, Tomoki; Tanaka, Aki; Nakata, Atsushi; Hirono, Kayo; Moriuchi, Shota; Nakamura, Shunsuke; Watanabe, Ayumu; Koyago, Haruka; Koyama, Ibuki; Morimoto, Kazunari; Nakai, Maria; Kitora, Sayaka; Tanigawa, Tomoyasu
2017MPBu...44..190M    Download PDF

Photometric observations of the main-belt asteroid 201 Penelope were made in 2017 January. Analysis found a rotation period of 3.75 ± 0.01 h and amplitude of 0.16 mag.

Near-IR Minor Planet Photometry from Burleith Observatory
Pages 191-192
Schmidt, Richard E.
2017MPBu...44..191S    Download PDF

Near-IR observations from a bright-sky urban area provide rotation periods for six main-belt minor planets: 450 Brigitta, 556 Phyllis, 849 Ara, 984 Gretia, 1152 Pawona and 1310 Villigera.

Lightcurve Analysis of Binary and Potential Binary Asteroids in 2015
Pages 193-199
Oey, Julian; Williams, Hasen; Groom, Roger; Pray, Donald; Benishek, Vladimir
2017MPBu...44..193O    Download PDF

It was known that asteroids with diameter of 15km (derived mainly from MPC estimated absolute magnitude (H)) or smaller were more likely to be binary systems than were larger objects. From a set of selection criteria, we used CCD photometry to determine whether the asteroids were binary systems.

Rotation Period Determination of Asteroids 6199 Yoshiokayayoi and 9671 Hemera
Pages 199-200
Brincat, Stephen A.
2017MPBu...44..199B    Download PDF

Synodic rotation periods and amplitudes are reported for 6199 Yoshiokayayoi 3.373 ± 0.002 hours, 0.10 ± 0.03 magnitudes; and 9671 Hemera 2.532 ± 0.001 hours, 0.10 ± 0.03 magnitudes.

Lightcurve Analysis of Asteroids from BMO and DRO in 2015
Pages 200-204
Oey, Julian; Williams, Hasen; Groom, Roger
2017MPBu...44..200O    Download PDF

Photometric observations of selected asteroids were done from Blue Mountains Observatory (BMO) and Darling Range Observatory (DRO) in 2015. The observations were made during a favorable apparition for each asteroid. Most of these objects had poorly defined lightcurves or were never worked in the past.

The Lightcurve and Rotation period of 9414 Masamimurakami
Pages 206
Odden, Caroline E.; Durrett, O. Nicole; Dolan, Patrick E.; Wang, Tianqi
2017MPBu...44..205O    Download PDF

Photometric observations of 9414 Masamimurakami were made at the Phillips Academy Observatory over eleven nights during 2016 March thru May. The rotation period of 9414 Masamimurakami was determined to be 15.623 ± 0.001 hrs with amplitude 0.29 mag.

Preliminary Pole and Shape Models for Three Near-Earth Asteroids
Pages 203-212
Warner, Brian D.; Pravec, Petr; Kusnirak, Peter; Benishek, Vladimir, Ferrero, Andrea
2017MPBu...44..206W    Download PDF

Observations of three near-Earth asteroids (NEAs) were made between 1993 and 2016. The resulting data were used to find preliminary pole and shape models for 1863 Antinous, (5836) 1993 MF, and (154244) 2002 KL6.

Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2016 December thru 2017 March
Pages 213-219
Warner, Brian D.
2017MPBu...44..213W    Download PDF

Lightcurves for 18 main-belt asteroids were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2016 December thru 2017 March. Many of the asteroids were “strays” in the field of planned targets, demonstrating a good reason for data mining images. Analysis shows that the Hungaria asteroid (45878) 2000 WX29 may be binary.

Lightcurve Analysis of 1773 Rumplestilz and 2040 Chalonge
Pages 219-220
Odden, Caroline E.; Caso, Maria; Dettorre, Christopher; Dial, Preston J.; Hoang, Kaitlin; Hughes, Riley; Lazar, Trevor T.; Morss, Paige P.; Mundra, Akshay R.; Naiyapatana, Abhichana; Rooney, Morgan
2017MPBu...44..219O    Download PDF

Photometric observations of asteroids 2040 Chalonge and 1773 Rumplstilz were made at the Philips Academy Observatory from 2016 December 2016 through 2017 February. 1773 Rumelstilz was found to have rotational period 106.075 ± 0.001 h with amplitude 0.78 mag. 2040 Chalonge was found to have rotational period 10.383 ± 0.001 h with amplitude 0.22 mag.

Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2016 December thru 2017 April
Pages 220-222
Warner, Brian D.; Stephens, Robert D.
2017MPBu...44..220W    Download PDF

Lightcurves for four Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2016 December thru 2017 April.

Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2016 December thru 2017 April
Pages 223-237
Warner, Brian D.
2017MPBu...44..223W    Download PDF

Lightcurves for 36 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2016 December through 2017 April were analyzed for rotation period and signs of satellites or tumbling. In addition, using the recent and previously obtained dense data along with sparse data from NEA surveys, lightcurve inversion was used to produce spin axis and shape models for four asteroids: 3103 Eger, 4055 Magellan, (40267) 1999 GJ4, and (90075) 2002 VU94. Analysis of the observations of 2102 Tantalus and (5693) 1993 EA indicates that they might each be a singly-asynchronous binary. There is some evidence that (5626) 1991 FE may be another socalled “very wide binary.”

Rotation Period Determination for 393 Lampetia
Pages 238
Pilcher, Frederick; Marciniak, Anna; Oey, Julian
2017MPBu...44..238P    Download PDF

CCD photometry of minor planet 393 Lampetia shows that it has a synodic rotation period of 38.455 ± 0.004 h, amplitude 0.08 ± 0.01 mag.

Results of the 2016 Mexican Asteroid Photometry Campaign
Pages 239-242
Sada, Pedro V.; Olguin, Lorenzo; Saucedo, Julio C.; Loera-Gonzalez, Pablo; Cantu-Sanchez; Laura; Garza, Jaime R.; Ayala-Gomez, Sandra A.; Aviles, Andres; Perez-Tijerina, Eduardo; Navarro-Meza, Samuiel; Silva, J. S.; Reyes-Ruiz, Mauricio; Segura-Sosa, Juan; Lopez-Valdivia, Ricardo; Alvarez-Santana, F.
2017MPBu...44..239S    Download PDF

We report the results of the 2016 Mexican Asteroid Photometry Campaign. This year observers from seven different research institutions carried out 34 nights of observations at three Mexican observatories. An uncertain, but long, period of ~115.108 ± 0.014 h was estimated for 703 Noėmi from sparse data. A nearly complete lightcurve was obtained for 1305 Pongola (P = 8.0585 ± 0.0003 h). Asteroid 2535 Hämeenlinna turned out to be a binary system where the primary exhibits a rotation period of 3.2311 ± 0.0001 h and the secondary shows an orbital period of 21.20 ± 0.004 h. Asteroid 4775 Hansen (P = 3.1186 ± 0.0001 h) was well observed and showed variations of its lightcurve between two sets of observations separated by about six weeks.

Asteroid 4296 Van Woerkom: A Newly Discovered Asynchronous Binary
Pages 242-243
Odden, Caroline E.; Caso, Maria; Dettorre, Christopher; Dial, Preston J.; Hoang, Kaitlin; Lazar, Travor T.; Morss, Paige P.; Mundra, Akshay R.; Naiyapatana, Abhichana; Rooney, Morgan; Pravec, Petr; Benishek, Vladimir; Klinglesmith, Dan; Pilcher, Frederick
2017MPBu...44..242O    Download PDF

We report that asteroid 4296 van Woerkom is a binary asteroid. Lightcurve analysis for images taken from 2016 November through December reveals a primary rotational period of 2.80868 ± 0.00005 h and a secondary orbital period of 26.22 ± 0.01 h.

CCD Asteroid Photometry from Etscorn Observatory
Pages 244-246
Klinglesmith III, Daniel A.; Hendrickx, Sebastian; Kimber, Cameron; Madden, Karl
2017MPBu...44..244K    Download PDF

We provide lightcurves for six asteroids from the Spin/Shape Modeling Opportunities listed in the “Lightcurve Photometry Opportunities: 2017 January- March” article by Warner et al. (2017)

Period Determination for 703 Noemi
Pages 247-248
Franco, Lorenzo; Scardella, Maurizio; Tomassini, Angelo; Franceschini, Francesco; Pierri, Fernando; Marchini, Alessandro
2017MPBu...44..247F    Download PDF

Collaborative lightcurve photometry observations of main-belt asteroid 703 Noemi were made over 16 nights in 2016 November thru 2017 January. The resulting synodic rotation period is 200 ± 1 h, amplitude 0.62 ± 0.10 mag, HR = 12.24 ± 0.12 and GR = 0.16 ± 0.10.

Rotation Period Determination for 9671 Hemera
Pages 248-249
Salvaggio, Fabio; Marchini, Alessandro; Papini, Riccardo
2017MPBu...44..248S    Download PDF

Photometric observations of main-belt asteroid 9671 Hemera were made at the Astronomical Observatory of the University of Siena (Italy) in 2017 March. Analysis of the data revealed a bimodal lightcurve with a synodic period of 2.532 ± 0.001 h as the most likely solution. Some anomalies in the lightcurve suggest that 9671 Hemera could be binary.

Rotation Period Determinations for 49 Pales, 96 Aegle, 106 Dione, 375 Ursula, and 576 Emanuela
Pages 249-251
Pilcher, Frederick
2017MPBu...44..249P    Download PDF

Synodic rotation periods and amplitudes are found for 49 Pales: 20.705 ± 0.002 h, 0.18 ± 0.01 mag with 4 maxima and minima per cycle; 96 Aegle: 13.868 ± 0.001 h, 0.11 ± 0.01 mag; 106 Dione: 16.210 ± 0.001 h, 0.18 ± 0.01 mag; 375 Ursula: 16.899 ± 0.001 h, 0.11 ± 0.01 mag. All of these objects have irregular lightcurves. For 576 Emanuela the period is 40.812 ± 0.004 h, amplitude is 0.13 ± 0.01 mag with a slightly asymmetric bimodal lightcurve.

Lightcurve Analysis of Trojan Asteroids at the Center for Solar System Studies 2017 January - March
Pages 252-257
Stephens, Robert D.; Coley, Daniel R.
2017MPBu...44..252S    Download PDF

Lightcurves for 18 Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2017 January to March.

Asteroids Observed from CS3: 2017 January - March
Pages 257-258
Stephens, Robert D.
2017MPBu...44..257S    Download PDF

CCD photometric observations of two Hungaria asteroids were obtained from the Center for Solar System Studies from 2017 January to March.

Photometric Observations of Asteroid 4742 Caliumi, 5267 Zegmott, (18429) 1994 AO1, (26421) 1999 XP113, and (27675) 1981 CH
Pages 259-260
Zeigler, Kenneth; Banshaw, Bryce; Gass, Janelle
2017MPBu...44..259Z    Download PDF

CCD photometric observations conducted from the George West ISD Mobile Observatory of asteroids 4742 Caliumi, 5267 Zegmott, (18429) 1994 AO1, (26421) 1999 XP113, and (27675) 1981 CH are described. This represents the research results for the 2016-17 school year. Analysis of our data found the synodic period and lightcurve amplitudes for each asteroid: 4742 Caliumi, 5.475 ± 0.005 h, 0.80 mag; 5267 Zegmott 5.209 h ± 0.002 h, 0.32 mag; (18429) 1994 AO1, 3.911 ± 0.002 h, 0.23 mag; (26421) 1999 XP113, 4.320 ± 0.005 h, 0.23 mag; and (27675) 1981 CH, 3.085 ± 0.002 h, 0.13 mag.

Follow-up Observations of 788 Hohensteina
Pages 261
Coley, Daniel
2017MPBu...44..261C    Download PDF

CCD photometric observations were made in 2016 November and December of the suspected tumbler and Hungaria group member 788 Hohensteina. The goal was to find a definitive rotation period, which would presumably match one of several reported periods.

Lightcurve and Rotation Period Determination for 1773 Rumpelstilz
Pages 262
Benishek, Vladimir; Pilcher, Frederick
2017MPBu...44..262B    Download PDF

Photometric observations from two locations in Europe and North America in 2017 February-April revealed that the main-belt asteroid 1773 Rumpelstilz was a slow rotator with a synodic period of 105.49 ± 0.01 h.

General Report of Position Observations by the ALPO Minor Planets Section fro the Year 2016
Pages 263-264
Pilcher, Frederick
2017MPBu...44..263P    Download PDF

Observations of positions of minor planets by members of the Minor Planets Section in calendar year 2016 are summarized.

Measurements of 100 'Critical' Minor Planets from NEAT Archive
Pages 265-269
Deshmukh, Shishir
2017MPBu...44..265D    Download PDF

Uncertainties associated with the orbits of minor planets can be reduced by analyzing archival imagery as attempted in the current investigation. Archival images from NEAT and NASA’s Skymorph database were analyzed using standard software to identify the minor planets listed in the critical list. Findings of each minor planet were submitted to Minor Planet Center (MPC) to offer better orbital solutions.

299 Thora and 496 Gryphia: Two More Very Slowly Rotating Asteroids
Pages 270-274
Pilcher, Frederick; Franco, Lorenzo; Pravec, Petr
2017MPBu...44..270P    Download PDF

CCD observations of the asteroids 299 Thora and 496 Gryphia were made to determine the synodic rotation periods. For 299 Thora, the period is 272.9 ± 0.9 h with a maximum amplitude 0.47 mag. No evidence of tumbling was found. We measured a color index of V-R = 0.52. Using average lightcurve magnitude, we found H = 11.68 ± 0.06, G = 0.27 ± 0.06. For 496 Gryphia, we found a rotation period near 1072 h and amplitude of 1.25 mag. Tumbling behavior was found but not quantified. The color index is V-R = 0.48. Using average lightcurve magnitudes, we found H = 12.21 ± 0.05, G = 0.18 ± 0.04.

Rotation Period Determination for 2411 Zellner, 5293 Bentengahama, and 9148 Boriszaitsev
Pages 274-276
Marchini, Alessandro; Ballini, Edoardo; Chianese, Edoardo; Maggioni, Edoardo; Scali, Stefano; Trefoloni, Bartolomeo; Papini, Riccardo; Salvaggio, Fabio
2017MPBu...44..274M    Download PDF

Photometric observations of three main-belt asteroids were made from the Astronomical Observatory of the University of Siena (Italy) in order to determine their synodic rotation periods. For 2411 Zellner, we found a period of 2.975 ± 0.002 h with an amplitude of 0.33 mag. For 5293 Bentengahama, the period was 15.781 ± 0.002 h with an amplitude of 0.18 mag. For 9148 Boriszaitsev, we found 8.124 ± 0.02 h with an amplitude of 0.23 mag.

Density and Axis-size Relationship of Five Main-belt Asteroids: 2017 January - March
Pages 276-279
Aznar Macias, Amadeo
2017MPBu...44..276A    Download PDF

Despite many decades of minor planet studies focused on external and dynamical properties, there are still hundreds of asteroids that have never been measured. Presented here are the results of photometric analysis applied to five main-belt asteroids. In addition to calculating rotation period, axis ratios assuming a simple ellipsoidal shape and the estimated minimum density of each asteroid are reported.

Lightcurve Photometry Opportunities: 2017 July-September
Pages 279-287
Warner, Brian D.; Harris, Alan W.; Durech, Josef; Benner, Lance A. M.
2017MPBu...44..279W    Download PDF

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 285
MPB Editorial Staff
2017MPBu...44..285M    Download PDF

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 in part by National Science Foundtation grant AST-1507535