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Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Modelling and scaling neglected asteroids A. Marciniak1 with V. Alí-Lagoa, T. Müller, P. Bartczak, R. Behrend, M. Butkiewicz-B ˛ak, G. Dudzinski,´ R. Duffard, K. Dziadura, S. Fauvaud, M. Ferrais, S. Geier, J. Grice, R. Hirsch, J. Horbowicz, K. Kaminski,´ P. Kankiewicz, D.-H. Kim, M.-J. Kim, I. Konstanciak, V. Kudak, L. Molnár, F. Monteiro, W. Ogłoza, D. Oszkiewicz, A. Pál, N. Parley, F. Pilcher, E. Podlewska - Gaca, T. Polakis, J. J. Sanabria, T. Santana-Ros, B. Skiff, K. Sobkowiak, R. Szakáts, S. Urakawa, M. Zejmo,˙ K. Zukowski˙ 1. Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Poznan,´ Poland ESOP XXXIX, 29 August 2020 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Asteroid lightcurves (219) Thusnelda P = 59.74 h 487 Venetia P = 13.355h 2014 -2,1 Oct 11.1 Suhora 2012/2013 -2,2 Oct 12.1 Suhora Oct 29.0 Bor Oct 24.1 Bor. -2,05 Nov 10.2 Suh Oct 28.1 Bor. Nov 11.1 Suh CCCCCC Nov 4.0 Bor. CCCCCCCCC CC C C Nov 7.4 Organ M. Dec 28.8 Bor C Mar 2.8 Bor C Nov 8.4 Organ M. AAAA -2 Mar 3.8 Bor AAAAAA C Nov 13.4 Organ M. AAAA C CCC Nov 14.4 Organ M. A -2,1 AAA CCC A Nov 15.4 Organ M. A AA Nov 21.4 Winer -1,95 Dec 2.1 OAdM Dec 3.0 OAdM Dec 5.0 Bor. Dec. 10.0 OAdM -1,9 Dec. 11.0 OAdM -2 Dec. 12.3 Organ M. A Dec 12.6 Bisei Relative R magnitude C Dec 13.7 Bisei -1,85 Relative C and R magnitude Dec 17.0 OAdM Dec 20.0 OAdM Dec 21.0 OAdM Dec 22.0 OAdM -1,8 Dec 23.0 OAdM -1,9 Dec 24.0 OAdM Zero time at: 2012 Nov 11.9962 UT, LT corr. Dec 24.9 OAdM -1,75 Zero time at: 2014 Dec 9.8788 UTC, LT corr. 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase (806) Gyldenia P = 16.852 h 9,8 487 Venetia P=13.342 h -4,75 2014 9,85 Feb 5.1 Bor. -4,7 Feb 6.1 Bor. Feb 23.1 Bor. Feb 23.8 Kie. Mar 9.1 Bor Mar 10.1 Bor 9,9 -4,65 Mar 30.0 Suh. Apr 11.9 Suh. Apr 12.9 Suh. -4,6 May 21.9 Bor. 9,95 -4,55 2013 Mar 5.1 Bor. Relative C magnitude Relative C magnitude 10 Mar 16.1 Bor. Apr 13.0 Bor. -4,5 Apr 16.3 Organ M. Apr 21.3 Organ M. 10,05 Apr 22.3 Organ M. -4,45 Apr 23.2 Organ M. May 8.2 Organ M. Zero time at: 2014 Feb 4.8867 UT, LT corr. May 14.9 Bor. -4,4 Zero time at: 2013 Apr 21.125 UTC, LT corr. 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 10,1 Phase 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase Marciniak et al. 2015, 2018 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Selection effects in Main Belt Asteroids models, year 2012 All 1230 asteroids with H≥11 mag Division values: P = 12 h, amax = 0.25 mag. Marciniak et al. 2015 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Selection effects in MBA models, 2020 update All 1195 asteroids with H≥ 11 mag Division values: P = 12 h, amax = 0.25 mag. Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Selected lightcurves (329) Svea P = 22.778 h 10 10,05 10,1 10,15 2013 Feb 27.4 Organ M. Mar 6.1 Bor. Mar 14.1 Bor. Relative C magnitude 10,2 Mar 24.1 Bor. Mar 24.4 Organ M. Mar 25.4 Organ M. Mar 26.4 Organ M. 10,25 Mar 27.4 Organ M. Apr 1.4 Organ M. Apr 4.3 Organ M. Zero time at: 2013 Feb 27.3066 UTC, LT corr. Apr 7.3 Organ M. 10,3 Apr 9.3 Organ M. 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8Apr 16.0 0,9 Bor. 1 Phase May 16.0 Bor. 227 Philosophia P=26.466 h -3,8 -3,75 -3,7 -3,65 2015 Apr 15.4 Winer Apr 17.4 Winer Apr 19.4 Winer relative R magnitude -3,6 Apr 30.3 Winer May 6.3 Winer May 10.3 Winer May 12.3 Winer -3,55 May 13.3 Winer May 14.3 Winer May 28.2 Winer Zero time at: 2015 Apr 15.2479 LT corr. Jun 29.9 Teide -3,5 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase Marciniak et al. 2015, 2018 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Selected lightcurves 335 Roberta 109 Felicitas P=12.027 h 2013 P = 13.188 h -4,5 29 Sep, Bor. 2017 18 Oct, Organ M. Jan 22.3 CTIO 19 Oct, Bor. Jan 27.1 Bor. -3,3 19 Oct, Organ M. Jan 29.1 Bor. 25 Oct, Bor. Feb 16.1 Bor. 21 Nov, Organ M. Feb 22.4 Tempe 18 Dec, Organ M. -4,4 Feb 23.4 Tempe 23 Dec, Bor. Feb 24.4 Tempe Feb 25.4 Tempe Feb 27.4 Tempe Mar 1.4 Tempe -3,2 -4,3 Relative C magnitude Relative C and R magnitude -3,1 -4,2 Zero time at: 2013 Sep 28.9158 UTC, LT corr. Zero time at 2017 Jan 28.9650 UTC, LT corr. 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase Phase 100 Hekate 538 Friederike P=27.068 h P=46.74 h 8,35 -3,5 2018 Feb 1.1 Kepler Feb 2.1 Kepler Feb 3.3 Kepler 8,4 Feb 4.0 Kepler Feb 5.0 Kepler Feb 5.9 Kepler -3,4 May 19.1 Kepler 8,45 May19.8 Kepler May 20.8 Kepler May 21.8 Kepler May 22.5 Kepler 2018 8,5 -3,3 Oct 18.1 Bor. Oct 19.0 Bor. Nov 1.1 Bor. Nov 4.1 OAdM Relative R magnitude 8,55 Nov 6.1 Bor. Nov 7.1 Bor. Relative R and C magnitude -3,2 Nov 10.4 Organ M. Nov 17.4 Organ M. Nov 18.0 Bor. 8,6 Nov 29.3 Organ M. Dec 5.9 Bor. Dec 11.2 OAdM Zero time at: 2018 Jan 31.7150 UTC, LT corr. Zero time at: 2018 Oct 17.9492 UTC, LT corr. Dec 14.3 Organ M. 8,65 -3,1 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 0 0,1 0,2 0,3 0,4 0,5 0,6 0,7 0,8 0,9 1 Phase Phase Marciniak et al., 2019 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Thermophysical modelling Insolation [W] and temperature distribution [K] - 159 Aemilia Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary O-C plots for (159) Aemilia model applied in TPM Marciniak et al. 2018 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Thermal inertia of Main Belt Asteroids Harris & Drube 2016 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Rotation Radiometricsolutionforcombineddata. Target period Taxonomic Diameter Albedo Thermalinertia [h] type [km] [Jm−2s−0.5K−1] 159Aemilia 24.4787 Ch 137 0.054 50 ±0.0001 ±8 ±0.015 ±50 227 Philosophia 26.4614 C 101 0.041 125 ±0.0001 ±5 ±0.005 ±90 329Svea 22.7670 C 78 0.055 75 ±0.0001 ±4 ±0.015 ±50 478Tergeste 16.10312 L 87 0.15 75 ±0.00003 ±6 ±0.02 ±45 487Venetia 13.34133 S 70 0.21 100 ±0.00002 ±4 ±0.02 ±75 Marciniak et al. 2018 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Thermal inertia of slow rotators after: Harris & Drube 2016 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Thermal inertia of (even more) slow rotators after: Harris & Drube 2016 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Fitting asteroid shape models to (poorly covered) occultations Figure: Fitting to occultation with only two positive chords. Pole, shape, and size are poorly constrained. Diameters of equivalent volume spheres: Pole 1: 116 ± 14 km; Pole 2: 108 ± 10 km Marciniak et al., 2012 Asteroid studies via lightcurves Selection effects TPM Shape models vs. occultations Summary Fitting the shape models to (good) occultations Diameters of equivalent volume sphere: CONVEX (pole 1): 130 ± 7 km; CONVEX (pole 2): 130 ± 8 km SAGE (pole 1): 135 ± 7 km; SAGE (pole 2): 138 ± 7 km Marciniak et al.
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  • The Minor Planet Bulletin, It Is a Pleasure to Announce the Appointment of Brian D

    The Minor Planet Bulletin, It Is a Pleasure to Announce the Appointment of Brian D

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 33, NUMBER 1, A.D. 2006 JANUARY-MARCH 1. LIGHTCURVE AND ROTATION PERIOD Observatory (Observatory code 926) near Nogales, Arizona. The DETERMINATION FOR MINOR PLANET 4006 SANDLER observatory is located at an altitude of 1312 meters and features a 0.81 m F7 Ritchey-Chrétien telescope and a SITe 1024 x 1024 x Matthew T. Vonk 24 micron CCD. Observations were conducted on (UT dates) Daniel J. Kopchinski January 29, February 7, 8, 2005. A total of 37 unfiltered images Amanda R. Pittman with exposure times of 120 seconds were analyzed using Canopus. Stephen Taubel The lightcurve, shown in the figure below, indicates a period of Department of Physics 3.40 ± 0.01 hours and an amplitude of 0.16 magnitude. University of Wisconsin – River Falls 410 South Third Street Acknowledgements River Falls, WI 54022 [email protected] Thanks to Michael Schwartz and Paulo Halvorcem for their great work at Tenagra Observatory. (Received: 25 July) References Minor planet 4006 Sandler was observed during January Schmadel, L. D. (1999). Dictionary of Minor Planet Names. and February of 2005. The synodic period was Springer: Berlin, Germany. 4th Edition. measured and determined to be 3.40 ± 0.01 hours with an amplitude of 0.16 magnitude. Warner, B. D. and Alan Harris, A. (2004) “Potential Lightcurve Targets 2005 January – March”, www.minorplanetobserver.com/ astlc/targets_1q_2005.htm Minor planet 4006 Sandler was discovered by the Russian astronomer Tamara Mikhailovna Smirnova in 1972. (Schmadel, 1999) It orbits the sun with an orbit that varies between 2.058 AU and 2.975 AU which locates it in the heart of the main asteroid belt.