Regular ArticleCeres Surface Properties by High-Resolution Imaging from Earth
References (0)
Cited by (43)
Porous dust particles in astrophysics and their thermal properties
2023, Planetary and Space ScienceLow-temperature reflectance spectra of brucite and the primitive surface of 1-Ceres?
2015, IcarusCitation Excerpt :In Fig. 1b, the 3.06 μm feature of Ceres is compared to that of brucite under different temperature. For a distance to the Sun of 2.72 a.u. and given its low geometric albedo (0.09 ± 0.03 in the V-band, Li et al., 2006), the equilibrium surface temperature is about 164 K. Direct measurements of the thermal flux arising from Ceres has shown that the maximum temperature achieved on Ceres is about 235 ± 4 K (Saint-Pe et al., 1993). This implies that the quality of the match which was found between Ceres 3.06 μm feature and that of brucite measured at ambient temperature (Milliken and Rivkin, 2009) could possibly decrease if the effect of temperature is taken into account.
Shape modeling technique KOALA validated by ESA Rosetta at (21) Lutetia
2012, Planetary and Space ScienceCitation Excerpt :For instance, the possible migration of the regolith at the surface of a fast-rotating asteroid triggered by YORP spin-up (Walsh et al., 2008) was suggested by the detailed 3-D shape of the NEO (66391) 1999 KW4 (Ostro et al., 2006). Since the 1990s, with the advent of the Hubble Space Telescope and large ground-based telescopes equipped with adaptive optics (AO: Lick, CFHT, Keck, ESO VLT, and Gemini), we have access to the angular resolution required to resolve the apparent disk of asteroids (e.g., Saint-Pé et al. 1993a,b; Drummond et al., 1998; Parker et al., 2002, 2006). From a time-series of disk-resolved images, spin-vector coordinates can be derived (using previous knowledge of the rotation period) by analyzing the changes in the apparent shape of the asteroid profile (see for instance Thomas et al., 1997b; Drummond and Christou, 2008), or by following the apparent path taken by an albedo patch on the surface during the rotation (e.g., Thomas et al., 2005; Carry et al., 2008).
Physical properties of (2) Pallas
2010, Icarus