Asteroid 21 Lutetia: Low Mass, High Density

Abstract

42The Rosetta flyby geometry at Lutetia on 10 July 2010 was suboptimal 43 because of the large flyby distance d=3168 +/-7.5 km, the high relative 46 Frequency Prediction 47The received carrier frequency from the actual flyby is compared with a 61The frequency prediction is routinely computed for radio science data 151The Doppler contributions from the HGA slew are evident in Figure 2b. 152The increase in frequency shortly before closest approach contrasts 174The rotation rates and angles were provided via the spacecraft housekeeping 175 telemetry data. 177 Filtering and adjustment 178The frequency residuals in Figure 2d were filtered at an integration time 179 of 18 seconds for noise reduction. 226The error of each parameter is derived from the diagonal terms of the 227 covariance matrix. 229The value of GM from the above described fitting procedure and 230 considering further error sources is determined to be GM = (11.34 ± 2311 The SPICE Kernel ORHR_______________00109.BSP is available from ssols01.esac.esa.int for all Rosetta experiment teams and is considered as a long term planning orbit file for experimental purposes. Comparison and discussion 246The values for GM and ∆f agree within the error with the analytical of Lutetia from astrometry (Baer et al., 2011; Fienga et al., 2008; Fienga 258 et al., 2010; Folkner et al., 2009 decreased by little more than a factor of 2. 294The volume leads to a bulk density of (3.4 ± 0.

AKARI/IRC near-infrared asteroid spectroscopic survey: AcuA-spec

“…Lutetia is an Xc-type asteroid (or M-type in the Tholen taxonomy), its bulk density was determined from the spacecraft Rosetta flyby as 3.4 ± 0.3 g cm −3 (Pätzold et al 2011). Rosetta also performed spectroscopy of Lutetia (Coradini et al 2011) and reported no absorption features in the spectral range from 0.4 to 3.5 µm.…”

Photometric analysis of Asteroid (21) Lutetia from Rosetta-OSIRIS images

“…The mass of Lutetia has been determined to be 1:700 AE 0:017 Â 10 18 kg (Pätzold et al, 2011), which gave a density of 3.4 ± 0.3 g/cm 3 (Sierks et al, 2011). Although Lutetia has been examined from Earth prior to this flyby (Belskaya et al, 2010), details of the taxonomy is limited, hindered by the complex surface composition (Barucci et al, 2012).…”

Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies

“…Indeed, both current collisional models (Bottke et al 2005a;Morbidelli et al 2009) as well as the recent measurements performed by Rosetta on the asteroid Lutetia (Pätzold et al 2011;Sierks et al 2011) and by Dawn on the asteroid Vesta (Marchi et al 2012) minimize the possibility that large bodies (D > 100 km) are collisional fragments themselves; instead these objects are predominantly primordial (undisrupted) planetesimals, which means they are unlikely to have undergone a catastrophic disruption since their formation. Specifically, an impactor population capable of producing widespread collisional disruption among D = 100-200 km asteroids would 1. strongly affect asteroids like Vesta by creating ∼9-10 basinforming events equivalent to the one that made the D ∼ 500 km Rheasilvia basin.…”