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Lightcurves of the Karin family asteroids
Yoshida F.a, Ito T.a, Dermawan B.b, Nakamura T.c, Takahashi S.a, Ibrahimov M.A.d, Malhotra R.e, Ip W.-H.f, Chen W.-P.f, Sawabe Y.g, Haji M.g, Saito R.g, Hirai M.g
a National Astronomical Observatory, Mitaka, Tokyo, Japan
b Department of Astronomy, Bandung Institute of Technology, Bandung, 40132, Indonesia
c Teikyo-Heisei University, Toshima, T0okyo, 170-8445, Japan
d Ulugh Beg Astronomical Institute, Tashkent, 700052, Uzbekistan
e Lunar and Planetary Laboratory, The University of Arizona, Tucson, 85721-0092, United States
f Institute of Astronomy, National Central University, Jhongli, Taoyuan, 32001, Taiwan
g Fukuoka University of Education, Munakata, Fukuoka, 811-4192, Japan
[vc_row][vc_column][vc_row_inner][vc_column_inner][vc_separator css=”.vc_custom_1624529070653{padding-top: 30px !important;padding-bottom: 30px !important;}”][/vc_column_inner][/vc_row_inner][vc_row_inner layout=”boxed”][vc_column_inner width=”3/4″ css=”.vc_custom_1624695412187{border-right-width: 1px !important;border-right-color: #dddddd !important;border-right-style: solid !important;border-radius: 1px !important;}”][vc_empty_space][megatron_heading title=”Abstract” size=”size-sm” text_align=”text-left”][vc_column_text]© 2016 Elsevier Inc.The Karin family is a young asteroid family formed by an asteroid breakup 5.8 Myr ago. Since the members of this family probably have not experienced significant orbital or collisional evolution yet, it is possible that they still preserve properties of the original family-forming event in terms of their spin state. We carried out a series of photometric observations of the Karin family asteroids, and here we report on the analysis of the lightcurves including the rotation period of eleven members. The mean rotation rate of the Karin family members turned out to be much lower than those of near-Earth asteroids or small main belt asteroids (diameter D 130 km). We investigated a correlation between the peak-to-trough variation and the rotation period of the eleven Karin family asteroids, and found a possible trend that elongated members have lower spin rates, and less elongated members have higher spin rates. However, this trend has to be confirmed by another series of future observations.[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Author keywords” size=”size-sm” text_align=”text-left”][vc_column_text][/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Indexed keywords” size=”size-sm” text_align=”text-left”][vc_column_text]Asteroids,Photometry,Rotation[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”Funding details” size=”size-sm” text_align=”text-left”][vc_column_text]We greatly appreciate the effort and courtesy extended by all the people who helped us during our observations at the Vatican Observatory’s “VATT” (the Alice P. Lennon Telescope and the Thomas J. Bannan Astrophysics Facility). We thank Elizabeth Green, Paula White, Ed Olszewski, and Andy Odell for allowing our use of the Steward 90-inch “Bok” telescope. FY is deeply thankful to Tom Gehrels who recommended that we use the VATT and the Bok telescopes in Arizona, and particularly for his encouragement of our observing activity and his enormous contribution to asteroid studies. Without his warmth, help, and thoughtful suggestions, we could not have carried out our observations there at all. The staff members at the Maidanak Observatory greatly helped us during our stay and observing activity. The authors thank the two anonymous referees for suggesting directions that significantly improved the quality of this paper. FY also has benefited from stimulating enlightenment by Murier Yoshida. Detailed and constructive review by Yolande McLean has considerably improved the English presentation of this paper. Some part of the data analysis was performed at the National Astronomical Observatory of Japan’s Astronomy Data Center (ADC) and Center for Computational Astrophysics (CfCA). This study is supported by the JSPS Kakenhi grant (16740259/2004–2005, 18540426/2006–2008, 18540427/2006–2008, 21540442/2009–2011, 25400458/2013–2015, 25400238/2013–2015), the JSPS program for Asia–Africa academic platform (2009–2011), the JSPS bilateral open partnership joint research project (2014–2015), the Sumitomo Foundation research funding (030755/2003–2004), and the Heiwa Nakajima Foundation research funding for Asian studies (2009).[/vc_column_text][vc_empty_space][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][vc_empty_space][megatron_heading title=”DOI” size=”size-sm” text_align=”text-left”][vc_column_text]https://doi.org/10.1016/j.icarus.2016.01.004[/vc_column_text][/vc_column_inner][vc_column_inner width=”1/4″][vc_column_text]Widget Plumx[/vc_column_text][/vc_column_inner][/vc_row_inner][/vc_column][/vc_row][vc_row][vc_column][vc_separator css=”.vc_custom_1624528584150{padding-top: 25px !important;padding-bottom: 25px !important;}”][/vc_column][/vc_row]