Physical properties of asteroid 308635 (2005 YU₅₅) derived from multi-instrument infrared observations during a very close Earth approach ^⋆

¹ Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany
e-mail: tmueller@mpe.mpg.de
² Institute of Astronomy, School of Science, the University of Tokyo, 2-21-1 Osawa, Mitaka, 181-0015 Tokyo, Japan
e-mail: tmiyata@ioa.s.u-tokyo.ac.jp
³ Konkoly Observatory, Research Center for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly Thege 15-17, 1121 Budapest, Hungary
⁴ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
⁵ Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Kanagawa, Japan
⁶ Department of Astronomy, Graduate School of Science, The University of Tokyo, Hongo 7-3-1, Bunkyo-ku, 113-0033 Tokyo, Japan
⁷ Planetary Plasma and Atmospheric Research Center, Tohoku University, Aramaki, Aoba-ku, 980-8578 Sendai, Japan
⁸ Astronomical Institute, Graduate School of Science, Tohoku University, Aramaki, Aoba-ku, 980-8578 Sendai, Japan
⁹ European Space Astronomy Centre (ESAC), European Space Agency, Apartado de Correos 78, 28691 Villanueva de la Cañada, Madrid, Spain

Received: 8 April 2013
Accepted: 29 July 2013

Abstract

The near-Earth asteroid 308635 (2005 YU₅₅) is a potentially hazardous asteroid which was discovered in 2005 and passed Earth on Nov. 8, 2011 at 0.85 lunar distances. This was the closest known approach by an asteroid of several hundred metres in diameter since 1976 when an object of similar size passed at 0.5 lunar distances. We observed 2005 YU₅₅ from the ground with a recently developed mid-IR camera (miniTAO/MAX38) in N and Q bands and with the Submillimeter Array (SMA) at 1.3 mm. In addition, we obtained space observations with Herschel/PACS at 70, 100, and 160 μm. Our thermal measurements cover a wide range of wavelengths from 8.9 μm to 1.3 mm and were taken after opposition at phase angles between –97° and –18°. We performed a radiometric analysis via a thermophysical model and combined our derived properties with results from radar, adaptive optics, lightcurve observations, speckle, and auxiliary thermal data. We find that 308635 (2005 YU₅₅) has an almost spherical shape with an effective diameter of 300 to 312 m and a geometric albedo p_V of 0.055 to 0.075. Its spin axis is oriented towards celestial directions (λ_ecl, β_ecl) = (60° ± 30°, –60° ± 15°), which means it has a retrograde sense of rotation. The analysis of all available data combined revealed a discrepancy with the radar-derived size. Our radiometric analysis of the thermal data together with the problem to find a unique rotation period might be connected to a non-principal axis rotation. A low to intermediate level of surface roughness (rms mean slope in the range 0.1–0.3) is required to explain the available thermal measurements. We found a thermal inertia in the range 350−800 Jm^-2 s^-0.5 K^-1, very similar to the rubble-pile asteroid 25 143 Itokawa and indicating a surface with a mixture of low conductivity fine regolith with larger rocks and boulders of high thermal inertia.