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THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 1, A.D. 2017 JANUARY-MARCH 1. EDITORIAL ANNOUNCEMENTS: (http://www.minorplanet.info/minorplanetbulletin.html) along MPB VOLUME 44 with MPB templates in Microsoft Word (Word 97) DOT and Word 2007 and above (DOTX) files. The templates include Richard P. Binzel, Editor instructions for using them as “starter papers” or to import MPB Brian D. Warner, Associate Editor paragraph styles into new or existing Word documents. David Polishook, Assistant Editor We welcome Dr. David Polishook as a new Assistant Editor and describe a new manuscript submission LIGHTCURVE ANALYSIS FOR requirement of a Summary Table for lightcurve results. THREE MAIN-BELT ASTEROIDS Stephen M. Brincat As evidenced by the figure below, rapid growth continues for the Flarestar Observatory (MPC 171) Minor Planet Bulletin. Volume 43 (2016) had a record number of San Gwann SGN 3160, MALTA 366 pages and results for more than 700 asteroids. [email protected] (Received: 2016 August 13) Photometric observations of three main-belt asteroids were made from 2016 March to June. The results of the lightcurve analysis are reported for 1154 Astronomia (1927 CB), 3680 Sasha (1987 MY), and (6138) 1991 JH1. The purpose of this research was to obtain the lightcurves of three main-belt asteroids: 1154 Astronomia (1927 CB), 3680 Sasha (1987 MY), and (6138) 1991 JH1 in order to determine the rotation period for each asteroid. A search of the asteroid lightcurve database (LCDB; Warner et al., 2009) and other sources did not find previously reported lightcurve results for these asteroids. Two editorial adjustments are needed to manage this growth. The All observations were obtained at Flarestar Observatory (MPC first is that we welcome Dr. David Polishook of the Weizmann Code: 171) at San Gwann, Malta. A Meade f/6.3 0.25-m Schmidt Institute of Science as a new Assistant Editor. Brian D. Warner Cassegrain Telescope (SCT) coupled to a Moravian G2-1600 continues as an Associate Editor and Professor Richard P. Binzel CCD was used. The pixel scale was 0.99 arcsec/pix at 1x1 as Editor. Dr. Robert A. Werner and Derald D. Nye continue in binning. This provided a field-of-view of 25.6x17.1 arcmin. All their service as MPB Producer and Distributor, respectively. asteroid images were obtained through a clear filter with integration times varying between 180 to 360 seconds depending The second adjustment is a requirement for all submitted on the brightness of the asteroid. All observing sessions were manuscripts, when appropriate, to contain a Summary Table of operated remotely through Sequence Generator Pro (SGP). All results that is constructed using a standard format. The table is images were dark and flat-field corrected. required to facilitate the entry of results into the Asteroid Lightcurve Data Base (LCDB). Lightcurve results manuscripts Differential photometry measurements were made in MPO not containing this Summary Table will be returned to the author. Canopus (Warner, 2015) using the FALC routine (Harris et. al., 1989) to derive the asteroid synodic periods. The StarBGone The table format is fully described in the “Authors Guide” utility in MPO Canopus was applied to measure images when appearing on page 81 of this issue and posted online asteroids where located in the vicinity of stars. The MPO Canopus Minor Planet Bulletin 44 (2017) Available on line http://www.minorplanet.info/mpbdownloads.html 2 Comp Star Selector utility was employed to select comparison 6138 (1991 JH1). This main-belt asteroid was discovered on 1991 stars of near solar-colour for differential photometry for all the May 14 by Otomo and Muramatsu at Kiyosato. It was reported as three asteroids. Information about discovery circumstances were a lightcurve photometry opportunity on the CALL website and obtained from the JPL small bodied Database, (JPL, 2016). All the observed on the nights of 2016 March 27, 30, and April 10. targets were selected from the CALL website (CALL, 2015). Exposures were 240 s for March 27 and 300 s for the remaining nights. Based on 218 data points, the derived synodic period is Observing circumstances and results are summarized in Table I. 5.4578 ± 0.006 h with an amplitude of 0.30 ± 0.09 mag. 1154 Astronomia (1927 CB) was discovered on 1927 February 8 by K. Reinmuth at Heidelberg. The asteroid was observed during eight nights from 2016 May 5 to June 14. Exposures were 300 seconds, except on June 14 when exposures were 360 seconds. A total of 347 data points were used to find the synodic period of 18.1154 ± 0.0139 h and amplitude of 0.39 ± 0.05 mag. Acknowledgements I would like to thank Brian Warner his work in the development of MPO Canopus and for his efforts in maintaining the CALL website. References 3680 Sasha (1987 MY) is a main-belt asteroid that was discovered on 1987 June 28 by E.F. Helin at Palomar. It was reported as a CALL (2015). Collaborative Asteroid Lightcurve Link. lightcurve photometry opportunity on the CALL website and http://www.MinorPlanet.info/call.html observed on four nights in 2016 March. The lightcurve is based on 329 data points with exposures of 180 s. The derived synodic Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., period is 5.8145 ± 0.005 h with an amplitude of 0.30 ± 0.05 mag. Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. JPL (2016). Small-Body Database Browser - JPL Solar System Dynamics web site. http://ssd.jpl.nasa.gov/sbdb.cgi Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid lightcurve database.” Icarus 202, 134-146. Updated 2016 Sept. http://www.MinorPlanet.info/lightcurvedatabase.html Warner, B.D. (2015). MPO Canopus software v10.7.0.6. Bdw Publishing. http//www.MinorPlanetObserver.com Number Name 2016 mm/dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 1154 Astronomia 05/05-06/14 347 1.2,12.7 225 3 18.1154 0.0139 0.39 0.05 3680 Sasha 03/05-03/19 329 6.0,2.8,5.9 169 4 5.8145 0.0047 0.30 0.05 6138 1991 JH 03/28-04/10 218 7.5,2.2,2.3 199 3 5.4578 0.0006 0.30 0.09 Table I. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is the second of three values. If a single value is given, the phase angle did not change significantly and the average value is given. LPAB and BPAB are each the average phase angle bisector longitude and latitude. Minor Planet Bulletin 44 (2017) 3 ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2015 FEBRUARY – MARCH Kylie Hess, Madison Bruner, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected] (Received: 2016 September 5) Photometric data were taken over four nights in 2015 February and one night in 2015 March for six asteroids: 507 Laodica, 583 Klotilde, 1911 Schubart, 2136 Jugta, 4958 Wellnitz, and (70171) 1999 OL2. In 2015 March, data were taken over five nights for 1027 Aesculapia, thirteen nights for 2522 Triglav, seven nights for 2581 Radegast and 4856 Seaborg, twelve nights for 10143 Kamogawa, and six nights for (16029) 1999 DQ6, 3733 Yoshitomo, 4963 Kanroku, and (7588) 1992 FJ1. Photometric observations of a number of asteroids were made from the Oakley Southern Sky Observatory in New South Wales, Australia, using an f/8.1 0.5-m Ritchey-Chretien telescope and STX-16803 camera, binned 3x3, with a luminance filter. The image scale was 1.344 arcsec/pix. The images were calibrated in MaxIM DL using bias, dark, and twilight flat frames. The images were measured and lightcurves were made using MPO Canopus. Table I gives the observing circumstances, exposure (seconds), and derived period and amplitude – if found – for each asteroid. The period determined for 507 Laodica matched the period determined by Black et al. (2016) to within experimental error. For the seven objects where a period could not be found, only the amplitude is reported. References Black, S., Linville, D. Michalik, D., Wolf, M., Ditteon, R. (2016). “Lightcurve Analysis of Asteroids Observed at the Oakley Southern Sky Observatory: 2015 December – 2016 April.” Minor Planet Bulletin 43, 287-289. EDITOR’S NOTE: It seems appropriate to add some commemoration to the lightcurve observations of 2136 Jugta presented here and recently by G. B. Casalnuovo (2015; MPB 43, 112). Long-time readers will recall J. U. Gunter (1911-1994), who was a retired pathologist who self-published a bimonthly newsletter named Tonight’s Asteroids in the 1970’s and 80’s. (“JUGTA” is a concatenation of Gunter’s initials and those of his newsletter.) It was Gunter who sparked amateur and professional astronomers’ interest in asteroids (including MPB Staff members Binzel, Werner, Nye and Section Recorder Pilcher). A more detailed description of Gunter’s contributions may be found in MPB 22, page 1 (1995). Minor Planet Bulletin 44 (2017) 4 Number Name 2015 mm/dd Pts Exp Phase LPAB BPAB Period P.E. Amp A.E. 507 Laodica 02/17-03/09 66 45 3.5,9.8 139 -5 4.7064 0.0007 0.18 0.04 583 Klotilde 02/17-03/09 78 30 4.7,11.0 144 -10 9.2134 0.0012 0.17 0.01 1027 Aesculapia 03/16-03/21 71 120 8.8,10.7 154 1 13.529 0.042 0.09 0.03 1911 Schubart 02/17-03/09 66 150 4.5,10.4 134 -1 - - 0.10 0.05 2136 Jugta 02/17-03/09 67 180 3.2,10.6 140 -1 6.4571 0.0007 0.45 0.05 2522 Triglav 03/11-03/27 248 180 4.5,7.7 170 -11 6.774 0.002 0.29 0.05 2581 Radegast 03/11-03/21 102 180 4.0,9.1 164 -3 8.753 0.002 0.82 0.06 3733 Yoshitomo 03/22-03/27 111 120 5.4,6.4 180 -8 - - 0.06 0.02 4856 Seaborg 03/11-03/21 111 150 3.8,6.6 168 -7 15.853 0.007 0.41 0.06 4958 Wellnitz 02/17-03/09 79 180 5.0,10.8 143 -11 - - 0.14 0.04 4963 Kanroku 03/22-03/27 107 150 3.9,5.7 175 -6 - - 0.10 0.04 7588 1992 FJ1 03/22-03/27 129 180 9.1,8.7 190 -20 - - 0.21 0.04 10143 Kamogawa 03/16-03/27 240 180 9.2,9.9 179 -18 - - 0.09 0.05 16029 1999 DQ6 03/16-03/21 89 180 5.7,7.8 163 -3 5.95 0.01 0.76 0.02 70171 1999 OL2 02/17-03/09 69 180 6.5,17.9 141 -8 - - 0.17 0.07 Table I.
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    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 37, NUMBER 2, A.D. 2010 APRIL-JUNE 41. LIGHTCURVE AND PHASE CURVE OF 1130 SKULD Robinson (2009) from his data taken in 2002. There is no evidence of any change of (V-R) color with asteroid rotation. Robert K. Buchheim Altimira Observatory As a result of the relatively short period of this lightcurve, every 18 Altimira, Coto de Caza, CA 92679 (USA) night provided at least one minimum and maximum of the [email protected] lightcurve. The phase curve was determined by polling both the maximum and minimum points of each night’s lightcurve. Since (Received: 29 December) The lightcurve period of asteroid 1130 Skuld is confirmed to be P = 4.807 ± 0.002 h. Its phase curve is well-matched by a slope parameter G = 0.25 ±0.01 The 2009 October-November apparition of asteroid 1130 Skuld presented an excellent opportunity to measure its phase curve to very small solar phase angles. I devoted 13 nights over a two- month period to gathering photometric data on the object, over which time the solar phase angle ranged from α = 0.3 deg to α = 17.6 deg. All observations used Altimira Observatory’s 0.28-m Schmidt-Cassegrain telescope (SCT) working at f/6.3, SBIG ST- 8XE NABG CCD camera, and photometric V- and R-band filters. Exposure durations were 3 or 4 minutes with the SNR > 100 in all images, which were reduced with flat and dark frames.
  • Yrfthesis.Pdf

    Yrfthesis.Pdf

    ABSTRACT Title of Dissertation PHYSICAL PROPERTIES OF COMETARY NUCLEI Yanga Rolando Fernandez Do ctor of Philosophy Dissertation directed by Professor Michael F AHearn Department of Astronomy I present results on the physical and thermal prop erties of six cometary nuclei This is a signicant increase in the numb er of nuclei for which physical information is available I have used imaging of the thermal continuum at midinfrared and radio wavelengths and of the scattered solar continuum at optical wavelengths to study the eective radius reectivity rotation state and temp erature of these ob jects Traditionally the nucleus has b een dicult to observe owing to an obscuring coma or extreme faintness I have taken advantage of new midinfrared array detectors to observe more comets than were p ossible b efore I have also codevelop ed a technique to separate the coma and nucleus from a comet image I develop ed a simple mo del of the thermal b ehavior of a cometary nucleus to help interpret the thermal ux measurements the mo del is an extension to the Standard Thermal Mo del for aster oids We have enough nuclei now to see the rst demarcations of the cometary region on an alb edodiameter plot I make a comparison of the cometary nuclei with outer Solar System small b o dies and nearEarth asteroids All of the cometary nuclei studied in this thesis are dark with geometric alb edos b elow and have eective diameters of around to km except for comet HaleBopp C O which is in the next order of magnitude higher I give an extensive discussion of the nuclear