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195 Minor Planet Bulletin 41 (2014) Diameter of 187 ± 6 Km and 2.03 195 diameter of 187 ± 6 km and 2.03 ± 0.39 g/cm3 respectively for a Observations of Main Belt Asteroids.” The Astrophysical Journal diameter value of 165 ± 5 km. If we assume an average grain Letters 759, L8 (5pp). density of ~2.9 g/cm3 for a C-type asteroid (Consolmagno et al., 2008), the bulk densities yield to a macroscopic porosity of about Mignard, F., Froeschlé (2000). “Global and local bias in the FK5 52% and 30%, respectively. from the Hipparcos data.” Astron. Astrophys. 354, 732-739. Test asteroid Used observations RMS M (Hermione) Schwan, H. (1988). “A computer program for evaluating the count (oppositions) arcsec solar masses MS analytical representation of the systematic differences between the 278 Paulina 790 (108) 0.20 2.37 ± 0.26 ' 10–12 FK4 and the FK5 or other catalogues of star positions or proper 5750 Kandatai 1014 (44) 0.10 2.33 ± 0.44 ' 10–12 motions.” Astron. Astrophys. 198, 363-364. Average: 2.35 ± 0.35 ' 10–12 Table 3. Individual mass results for 121 Hermione. Shampine, L.F., Gordon, M.K. (1975). “Computer Solution of Ordinary Differential Equations: the Initial Value Problem.” W. H. Conclusion Freeman and Co., San Francisco. The mass of 121 Hermione was estimated from the analysis of the Sitarski, G. (1971). “Correction of Cometary Orbits Including the motion of the asteroids 278 Paulina and 5750 Kandatai. An Perturbations in Differential Coefficients.” Acta Astronomica 21, –12 averaged mass value M = 2.4 ± 0.4 ' 10 solar masses was 87-100. –12 obtained from that. The value M = 3.3 ± 1.1 ' 10 MS which was found by the author in the previous work (Kretlow, 2005) is still Sitarski, G. (1983). “Effects of General Relativity in the Motion of consistent with these new value within the formal errors. This Minor Planets and Comets.” Acta Astronomica 33, 295-304. independent solution is in a good agreement with the mass value derived from the motion of Hermione’s satellite, M = 2.36 ± 0.10 ' Tedesco, E.F., Noah, P.V., Noah, M., Proce, S.D. (2002). “The –12 10 MS, by Descamps et al. (2009), which was based on an Supplemental IRAS Minor Planet Survey (SIMPS).” Astronomical effective diameter 187 ± 6 km. Journal 123, 1056-1085. References Usui, F., Kuroda, D., Müller, T.G., Hasegawa, S., Ishiguro, M., Ootsubo, T., Ishihara, D., Kataza, H., Takita, S., Oyabu, S., Ueno, Baer, J., Chesley, S.R., Matson, R.D. (2011). “Astrometric Masses M., Matsuhara, H., Onaka, T. (2011). “Asteroid Catalog Using of 26 Asteroids and Observations on Asteroid Porosity.” Akari: AKARI/IRC Mid-Infrared Asteroid Survey.” Publications Astronomical Journal 141, 143-155. of the Astronomical Society of Japan 63, 1117-1138. Consolmagno, G., Britt, D., Macke, R. (2008). “The significance of meteorite density and porosity.” Chemie der Erde – Geochemistry 68, 1-29. PHOTOMETRIC STUDY OF SELECTED ASTEROIDS Descamps, P., Marchis, F., Durech, J., Emery, J., Harris, A.W., Vasilij G. Shevchenko, Feodor P. Velichko, Kaasalainen, M., Berthier, J., Teng-Chuen-Yu, J.-P., Peyrot, A., Vitaly A. Checha, Yurij N. Krugly Hutton, L., Greene, J., Pollock, J., Assafin, M., Vieira-Martins, R., Institute of Astronomy of Kharkiv Karazin National University Camargo, J.I.B., Braga-Ribas, F., Vachier, F., Reichart, D.E., Sumska Street 35, Kharkiv 61022, Ukraine Ivarsen, K.M., Crain, J.A., Nysewander, M.C., Lacluyze, A.P., [email protected] Haislip, J.B., Behrend, R., Colas, F., Lecacheux, J., Bernasconi, L., Roy, R., Baudouin, P., Brunetto, L., Sposetti, S., Manzini, F. (Received: 15 April) (2009). “New insights on the binary Asteroid 121 Hermione.” Icarus 203, 88-101. We performed photometric observations for eleven Kretlow, M. (2005). Asteroid Mass Determination. Talk given on asteroids. New rotation periods were determined for five the annual Minor Planet Meeting, Heppenheim (Germany), 2005 asteroids: 2812 Scaltriti (7.596 h), 4716 Urey (6.2 h), June 17-19. http://space.kretlow.de/? 7446 Hadrianus (3.402 h), (26657) 2000 SX293 (2.8 - Solar_System_Dynamics:Asteroid_Masses 3.8 h), and (54063) 2000 GC136 (5.154 h). Mainzer, A., Grav, T., Masiero, J., Hand, E., Bauer, J., Tholen, D., McMillan, R.S., Spahr, T., Cutri, R.M., Wright, E., Watkins, J., Photometric observations of asteroids were carried out at the Mo, W., Maleszewski, C. (2011). “NEOWISE Studies of Chuguev Station (MPC 121) of the Institute of Astronomy Kharkiv Spectrophotometrically Classified Asteroids: Preliminary Results.” Karazin National University with a 0.7-m telescope using a one- The Astrophysical Journal 741, A90 (25pp). channel photoelectric photometer in 1995 and CCD cameras in other years. Methods of the photoelectric data reduction were Marchis, F., Enriquez, J.E., Emery, J.P., Mueller, M., Baek, M., described by Shevchenko et al. (1992); the method of CCD Pollock, J., Assafin, M., Vieira Martins, R., Berthier, J., Vachier, observations is explained in Krugly et al. (2002). The CCD-images F., Cruikshank, D.P., Lim, L.F., Reichart, D.E., Ivarsen, K.M., were reduced with the aperture photometry package (ASTPHOT) Haislip, J.B., LaCluyze, A.P. (2012). “Multiple asteroid systems: developed at DLR (Berlin) by S. Mottola (Mottola et al., 1995). Dimensions and thermal properties from Spitzer Space Telescope The observations were obtained in the V and R bands of the and ground-based observations.” Icarus 221, 1130-1161. standard Johnson-Cousins photometric system. The absolute calibrations of the comparison stars were performed with standard Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., sequences from Landolt (1992) and Skiff (2007). The accuracy of Nugent, C., Cabrera, M.S. (2012). “Preliminary Analysis of absolute photometry is equal to 0.02-0.03 mag. Our observations WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic are mainly presented as composite lightcurves which are Minor Planet Bulletin 41 (2014) 196 constructed according to the procedures described by Harris and 7446 Hadrianus. We observed this asteroid for two apparitions in Lupishko (1989). The data are composited with the period value 2011 and 2014. We determined a rotation period of 3.402 ± shown in the figures. Data from each night, denoted by different 0.005 h. The amplitudes of the lightcurves are similar for the two symbols in the figure, were shifted along the ordinate (magnitude apparitions: A = 0.70 ± 0.02 and 0.67 ± 0.02 mag, respectively. scale) in order to obtain the best fit with the data points of other The measured color index is V-R = 0.44 ± 0.02 mag. lightcurves. The dispersion of lightcurves was used as a criterion of our combining. The accuracy of measured brightness of an (26657) 2000 SX293. This asteroid has a diameter of about 7.0 km asteroid for the individual nights is not worse than 0.03 mag. The and albedo 0.14 (Masiero et al., 2011). We observed it for one time scale is not corrected for a light time for asteroids observed night in 2007 April. The rotation period lies in range of 2.8 to 3.8 for one night. hours, if the lightcurve is symmetrical to a half period. The average amplitude of the lightcurve is A = 0.30 ± 0.05 mag. Lightcurve Observations and Rotational Periods (54063) 2000 GC136. This asteroid has a diameter of 6.5 km and 44 Nysa. There are many photometric data for this E-type asteroid albedo 0.10 (Masiero et al., 2011). It was observed for three nights (see, for example, Warner et al., 2013). Our data are consistent in 2014 March. The composite lightcurve is consistand with a with the rotation period of 6.422 ± 0.001 h found by Harris et al. rotation period of 5.154 ± 0.005 h. The maximum amplitude is A = (1989). We observed Nysa in 2011 for three nights. The composite 0.45 ± 0.03 mag. The V-R is equal to 0.47 ± 0.04 mag. lightcurve has an average amplitude A = 0.27 ± 0.03 mag. Acknowledgments 69 Hesperia. Many photometric data were obtained for this M-type asteroid (see, for example, Warner et al., 2013). We observed We are grateful to the DLR Institute of Planetary Exploration, Hesperia in 1995 March-April with a one-channel photoelectric (Germany, Berlin) for providing us the CCD-camera and the photometer. The composite lightcurve constructed with a rotation ASTPHOT software. Since 2006 June, observations on the 0.7-m period of 5.655 ± 0.005 h has an average amplitude A = 0.18 ± telescope were carried out with the CCD camera obtained thanks to 0.02 mag. INTAS grant Ref. No 03-70-567. This research was partly supported by the Ukrainian Ministry of Education and Science. 184 Dejopeja. There are many photometric data for this asteroid (see, for example, Marciniak et al., 2007; Warner et al., 2013). We References observed Dejopeja in 1995 for two nights. The composition lightcurve is constructed with a rotation period of 6.44 ± 0.01 h Harris, A.W., Lupishko, D.F. (1989). “Photometric lightcurve and has a maximum amplitude A = 0.25 ± 0.03 mag. observations and reduction techniques.” In Asteroids II (R.P. Binzel, T. Gehrels, M.S. Matthews, eds.) pp 39-53. Univ. of 212 Medea. Many photometric data were obtained for this asteroid Arizona Press, Tucson. (see, for example, Warner et al., 2013). We observed Medea in 1995 for four nights. The composite lightcurve is constructed with Harris, A.W., Young, J.W., Contreiras, L., Dockweiler, T., a rotation period of 10.288 ± 0.010 h. The average amplitude is Belkora, L., Salo, H., Harris, W.D., Bowell, E., Poutanen, M., equal to 0.15 ± 0.03 mag. Binzel, R.P., Tholen, D.J., Wang, S.
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