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:

Derald D. Nye
Minor Planet Bulletin
10385 E. Observatory Drive
Corona de Tucson, AZ 85641-2309

Authors Guide and Word Templates   (v.2.7: updated 2019 March 4)
Please read this updated guide since there are a number of changes from previous guides.
The ZIP file contains the Authors Guide PDF as well as a "starter" paper in Word 97 (DOT) and Word 2007+ (DOTX).

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 46 (2019)

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Volume 15 (1988)

Volume 14 (1987)

Volume 13 (1986)

Volume 12 (1985)

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Volume 1 (1973)

Issue 35-4 (2008 Oct-Dec)
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The Lightcurve of Asteroid 5331 Erimomisaki
Pages 143
Boe, Caleb; Durkee, Russell I.; Casulli, Silvano; Vincent, Fiona; Higgins, David
2008MPBu...35..143B    Download PDF

Asteroid 5331 Erimomisaki was observed between 2007 Nov. 30 and 2008 Jan. 9. A synodic period of 24.26 ± 0.02 h with a mean amplitude of 0.27 ± 0.02 mag was derived.

A Collection of Lightcurves from Modra: 2007 December- 2008 June
Pages 144-146
Galad, Adrian; Kornos, Leonard
2008MPBu...35..144G    Download PDF

Lightcurve analysis led to rotation periods of main-belt asteroids 651 Antikleia, 653 Berenike, 2363 Cebriones, 12482 Pajka, 23327 Luchernandez, (28292) 1999 CX54, and (74424) 1999 BN. Only tentative results were obtained for rotation periods of 17102 Begzhigitova, 27270 Guidotti, and (74056) 1998 KM9.

Period Determination for 161 Athor
Pages 147
Pilcher, Frederick; Higgins, David
2008MPBu...35..147P    Download PDF

New observations at Organ Mesa and Hunters Hill Observatories 2008 March and April show that 161 Athor has a synodic period of 7.281 ± 0.001 h and, during that time, a monomodal lightcurve with amplitude of 0.08 ± 0.02 magnitudes. An approximate pole position is also reported.

Lightcurve Analysis of 788 Hohensteina
Pages 148
Oey, Julian; Marks, Scott, A.; Fauerbach, Michael
2008MPBu...35..148O    Download PDF

A collaborative effort from two widely-separated geographical longitudes resulted in three nights of long, continuous observations of 788 Hohensteina. The 14-hour, non-overlapping lightcurve allowed us to constrain the synodic period of the asteroid to 37.176 ± 0.004 h with an amplitude of 0.18 ± 0.03 mag.

Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory: 2008 March
Pages 149-150
Oliver, Robert Lemke; Shipley, Heath; Ditteon, Richard
2008MPBu...35..149O    Download PDF

Photometric data for 17 asteroids were collected over ten nights of observing during 2008 February and March at the Oakley Southern Sky Observatory. The asteroids were: 170 Maria, 266 Aline, 426 Hippo, 441 Bathilde, 619 Triberga, 701 Oriola, 840 Zenobia, 1175 Margo, 1232 Cortusa, 1297 Quadea, 1309 Hyperborea, 1355 Magoeba, 1505 Koranna, 2120 Tyumenia, 2606 Odessa, 3428 Roberts, and 4254 Kamel.

Lightcurve Analysis of 102 Miriam, 1433 Geramtina, and 2648 Owa
Pages 151-152
Johnson, Thomas; Pech, Katherin; van Schilfgaarde, Ryan; Chase, Matt; Burns, M. Shane
2008MPBu...35..151J    Download PDF

Asteroids 102 Miriam, 1433 Geramtina,and 2648 Owa were observed from NURO facilities in Flagstaff, AZ. Synodic rotation periods were estimated for each asteroid. Miriam’s period was estimated to be 15.789 h. We were able to estimate a lower limit the period of Geramtina to be 14 h. Owa’s period is 3.563 h

Asteroid Lightcurve Observations
Pages 152-154
Clark, Maurice
2008MPBu...35..152C    Download PDF

Asteroid period and amplitude results obtained at the Montgomery College Observatory in Rockville, Maryland, are presented.

Asteroid Lightcurve Analysis at Menke Observatory
Pages 155-160
Menke, John; Cooney, Walt; Gross, John; Terrell, Dirk; Higgins, David
2008MPBu...35..155M    Download PDF

The lightcurves for the following asteroids are reported: 305 Gordonia, 316 Goberta, 608 Adolfine, 707 Steina, 710 Gertrud, 1187 Afra, 1216 Askania, 1325 Inanda, 1462 Zamenhoff, 1559 Kustaanheimo, 1671 Chaika, 1999 Hirayama, 2075 Martinez, 2094 Magnitka, 2444 Lederle, 3156 Ellington, 4264 Karljosephine, and 7895 Kaseda. Three of these (707, 1325, and 4264) are slow rotators.

Lightcurve Analysis of Asteroids 3036 Krat, 3285 Ruth Wolfe and 5448 Siebold
Pages 160-161
Hummel, Jacob; Postma, Angela; Sumter, George C.; Moore, Harold; Sweet, Samantha; Beaky, Matthew M.
2008MPBu...35..160H    Download PDF

Main-belt asteroids 3036 Krat, 3285 Ruth Wolfe, and 5448 Siebold were observed by the authors. 3036 Krat, observed at Lowell Observatory in 2007 December, was found to have a period of 9.61 ± 0.01 h. For the other two asteroids, both observed at the Truman Observatory in 2007, we found 3285 Ruth Wolfe to have a period of 3.919 ± 0.001 h and 5448 Siebold was determined to have a period of 2.929 ± 0.001 h.

CCD Photometry of Three Short-period Asteroids from the Universidad de Monterry Observatory
Pages 161-162
Sada, Pedro V.
2008MPBu...35..161S    Download PDF

CCD photometry of three asteroids was obtained at the Universidad de Monterrey Observatory during 2007 April and 2008 March. These asteroids were observed on only one or two nights, but complete lightcurves were obtained due to relatively short rotation periods. The resulting synodic rotation periods and amplitudes are as follows: 811 Nauheima, 4.011 ± 0.006 h, 0.11 ± 0.03 mag; 3787 Aivazovskij, 2.97 ± 0.01 h, 0.18 ± 0.02 mag; and 5474 Gingasen, 3.628 ± 0.005 h, 0.16 ± 0.03 mag.

Asteroid Lightcurve Analysis at the Palmer Divide Observatory: February-May 2008
Pages 163-166
Warner, Brian D.
2008MPBu...35..163W    Download PDF

Lightcurves for 22 asteroids were obtained at the Palmer Divide Observatory (PDO) from February to May 2008: 578 Happelia, 1093 Freda, 1324 Knysna, 1528 Conrada, 1817 Katanga, 2001 Einstein, 2048 Dwornik, 2150 Nyctimene, 2491 Tvashtri, 3198 Wallonia, 3800 Karayusuf, 4425 Bilk, (5559) 1990 MV, (6394) 1990 QM2, 6435 Daveross, (11398) 1998 YP1, (12390) 1994 WB1, (24094) 1999 UN60, 26887 Tokyogiants, (27068) 1998 SU74, (31827) 1999 VJ13, and 2002 TD66.

Shape and Spin Models for Four Asteroids
Pages 167-171
Warner, Brian D.; Durech, Josef; Fauerbach, Michael; Marks, Scott
2008MPBu...35..167W    Download PDF

The authors present shape and spin axis models for four asteroids: 54 Alexandra, 167 Urda, 409 Aspasia, and 1022 Olympiada. The models were constructed using a combination of dense lightcurves and sparse data sets from USNO observations for lightcurve inversion. The use of combined dense and sparse data sets in order to find asteroid models will become more common as next-generation large surveys come on line.

A Preliminary Shape and Spin Axis Model for 595 Polyxena
Pages 171-172
Warner, Brian D.
2008MPBu...35..171W    Download PDF

Photometric observations made at the Palmer Divide Observatory during the 2006 and 2008 apparitions of the main-belt asteroid 595 Polyxena were combined with dense lightcurves from 1993 included in the Uppsala Asteroid Photometric Catalog and a sparse lightcurve based on data from the USNO to determine a preliminary shape and spin axis model. Two solutions dominated the result set, one prograde (? = 42°, ß = 8°) and one retrograde (l = 222°, l = -4°). The uncertainty in each coordinate is ± 5°. The sidereal period was found to be 11.794162 ± 0.000023 h.

Lightcurve Analysis of 7233 Majella
Pages 173
Crawford, Greg
2008MPBu...35..173C    Download PDF

7233 Majella was observed over eight nights in May 2008. The synodic period was determined as 3.812 ± 0.004 h. The peak-to-peak amplitude was ~0.5 mag.

Asteroid Lightcurve Analysis of Suspected Binary Asteroids
Pages 173-175
Higgins, David; Pravec, Petr; Kusnirak, Peter; Hornoch, Kamil; Pray, Donald P.; Vilagi, Jozef; Kornos, Leonard; Gajdos, Sefan; Husarik, Marek; Pikler, Michal; Cervak, Gabriel
2008MPBu...35..173H    Download PDF

Photometric observations undertaken by collaborating observatories in the BINAST group have uncovered strong evidence of asynchronous binary nature of minor planet 5474 Gingasen and the synchronous binary nature of minor planet 7369 Gavrilin.

Do What You Can Do Photometry: Unfiltered Photometry of NEOs 2005 PJ2, 2005 WC1, and 2006 GY2
Pages 175-177
Higley, Steven; Hardersen, Paul; Dyvig, Ron
2008MPBu...35..175H    Download PDF

The authors made observations of three Near-Earth Objects (NEOs), 2005 PJ2, 2005 WC1 and 2006 GY2, using clear filter photometry and instrumental magnitude relationships to determine preliminary rotation periods. This study demonstrates the potential utility of what is referred to as “do what you can do” photometry.

Asteroids Observed from GMARS and Santana Observatories: Eary 2008
Pages 178-179
Stephens, Robert D.
2008MPBu...35..178S    Download PDF

Lightcurve period and amplitude results from Santana and GMARS Observatories are reported for 2008 January to March: 411 Xanthe (11.344 ± 0.002 h and 0.10 mag), 655 Briseis (160.66 ± 0.12 h and 0.40 mag), and (5851) 1991 DM1 (367.52 ± 0.5 h and 0.90 mag).

Asteroid Lightcurve Analysis at the Via Capote Observatory: 2nd Quarter 2008
Pages 179-181
Brinsfield, James W.
2008MPBu...35..179B    Download PDF

Lightcurves for ten asteroids were measured at the Via Capote Observatory from 2008 April through June: 411 Xanthe (7.56 h), 455 Bruchsalia (11.85 h), 742 Edisona (18.52 h), 1633 Chimay (6.58 h), 1793 Zoya (5.753 h), 4215 Kamo (11.67 h), 4399 Ashizuri (2.829 h), 4585 Ainonai (38.31 h), 6274 Taizaburo (3.13 h), and 8132 Vitginzburg (7.28 h).

Lightcurve of Binary Minor Planet 2005 NB7
Pages 181-182
Vander Haagen, Gary A.
2008MPBu...35..181V    Download PDF

Lightcurve 2005 NB7 revealed binary characteristics with an orbital period of 15.267 ± 0.094 h with amplitude 0.26 ± 0.05 mag and a primary rotation period of 3.472 ± 0.003 h with amplitude 0.15 ± 0.05 mag. No secondary period was detected indicating tidal lock.

A Study of the Trinary NEA 2001 SN263
Pages 182-184
Betzler, Alberto Silva; Novaes, Alberto Brum; Celedon, Julian Hermogenes Quesada
2008MPBu...35..182B    Download PDF

The trinary NEA, 2001 SN263, was observed by the authors in 2008 February in Salvador, Bahia, Brazil. Based on the data obtained, the synodic period of the primary body was estimated to be 3.20 ± 0.01h with a lightcurve amplitude of 0.27 ± 0.07 mag. The orbital period of the smaller satellite (0.4 Km) was estimated to be 46.1 ± 0.3 h. The NIR spectrum suggests the object is of type C according to DeMeo classification. Lance, a CO3 type meteorite, is the best analogous meteorite.

The Rotation Period of 1231 Auricula
Pages 185-186
Bembrick, Colin; Crawford, Greg; Allen, Bill
2008MPBu...35..185B    Download PDF

The synodic rotation period of minor planet 1231 Auricula was found to be 3.9816 ± 0.0006 h. Assuming a near equatorial aspect, the overall amplitude of 0.75 mag implies an axial ratio a/b = 1.99.

Lightcurve Photometry Opportunities: October-December 2008
Pages 186-189
Warner, Brian D.; Harris, Alan W.; Pravec, Petr; Durech, Josef; Benner, Lance A. M.
2008MPBu...35..186W    Download PDF

We present here four lists of “targets of opportunity” for the period 2008 October-December. The first list is those asteroids reaching a favorable apparition during this period, are <15m at brightest, and have either no or poorly constrained lightcurve parameters. By “favorable” we mean the asteroid is unusually brighter than at other times and, in many cases, may not be so for many years. The goal for these asteroids is to find a welldetermined rotation rate. Don’t hesitate to solicit help from other observers at widely spread longitudes should the initial findings show that a single station may not be able to finish the job.

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