Physical properties of near-Earth asteroids with a low delta-<i>v</i>: Survey of target candidates for the Hayabusa2 mission

Hasegawa, Susumu; Kuroda, D.; Kitazato, K.; Kasuga, Toshihiro; Sekiguchi, T.; Takato, Naruhisa; Aoki, Kentaro; Arai, Akira; Choi, Young Jun; Fuse, Tetsuharu; Hanayama, H.; Hattori, Takashi; Hsiao, Hsiang Yao; Kashikawa, Nobunari; Kawai, N.; Kawakami, Kimihiro; Kinoshita, Daisuke; Larson, S. M.; Lin, Chih-Hong; Miyasaka, Seidai; Miura, N.; Nagayama, S.; Nagumo, Yu; Nishihara, S.; Ohba, Yoshiki; Ohta, Kouji; Ohyama, Youichi; Okumura, S.; Sarugaku, Yuki; Shimizu, Yasuhiro; Takagi, Y.; Takahashi, Jun; Toda, H.; Urakawa, Seitaro; Usui, Fumihiko; Watanabe, Makoto; Weissman, P. R.; Yanagisawa, K.; Yang, Hyunah; Yoshida, Michitoshi; Yoshikawa, Makoto; Ishiguro, Masateru; Abe, Masanao

doi:10.1093/pasj/psy119

Cited by 12 publications

(3 citation statements)

References 135 publications

(200 reference statements)

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“…Radar, thermal-IR, and many light curve studies have been conducted on this asteroid to date. Hasegawa et al (2018) derive a synodic rotation period of 7.911 ± 0.0001 hours, in agreement with the synodic period of 7.908 ± 0.001 hours from Franco et al (2010). This is also consistent with more recent observations by Warner & Stephens (2021), who report synodic rotation periods of 7.9219 ± 0.0003 hours and 7.9144 ± 0.0004 hours.…”

Section: Convex Shape Modelling and Phase Curve Variability Of (15940...supporting

confidence: 89%

The effect of aspect changes on Near-Earth Asteroid phase curves

Jackson

Rozitis

Dover

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Phase curves of asteroids are typically considered to depend solely on the scattering properties of airless particulate surfaces and the size of the object being studied. In this study, we demonstrate the additional dependence of phase curves on object shape, rotation pole orientation, and viewing geometry over an apparition. Variations in the phase curve of near-Earth asteroid (159402) 1999 AP10 over its apparition from July 2020 - January 2021 are verified to be due to aspect changes over the apparition. This is achieved through shape modelling of the asteroid and simulation of the phase curve over the apparition. We present simulations of asteroid phase curves over a range of geometries to understand the potential magnitude of this aspect effect, and under which circumstances it can begin to dominate in the phase curves. This dependence on aspect may introduce significant additional uncertainty in the properties derived from phase curve data. We provide and demonstrate software code to estimate the aspect-related uncertainty in near-Earth asteroid phase curves through simulation and model fitting of a randomly generated sample of ellipsoidal asteroid models over the observed viewing geometry. We demonstrate how ignoring this effect may lead to misleading interpretations of the data and underestimation of uncertainties in further studies, such as those in the infrared that use phase curve derived parameters when fitting physical properties of an asteroid.

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Section: Convex Shape Modelling and Phase Curve Variability Of (15940...supporting

confidence: 89%

The effect of aspect changes on Near-Earth Asteroid phase curves

Jackson

Rozitis

Dover

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…A-type asteroids are considered olivine-dominated asteroids and originated from the mantle of differentiated bodies (e.g., Cruikshank & Hartmann 1984;Sunshine et al 2007). Most A-type asteroids have very red spectra (e.g., DeMeo et al 2009DeMeo et al , 2019, but olivine-dominated asteroids with an unweathered surface (flatter spectra) have been found among NEAs (Reddy et al 2011;Hasegawa et al 2018).…”

Section: Discussionmentioning

confidence: 99%

Candidate Main-belt Asteroids for Surface Heterogeneity

Hasegawa,

Marsset,

DeMeo

et al. 2024

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Large terrestrial bodies in our solar system like the Earth, Mars, Mercury, and the Moon exhibit geologically complex surfaces with compositional heterogeneity. From past studies using large telescopes and spacecraft, it was shown that asteroids with diameters larger than 100 km also show surface heterogeneity at hemispheric scales, while on smaller objects, such features remain to be detected. Here, we investigate candidates for surface heterogeneity in a sample of 130 main-belt asteroids using multiepoch spectroscopic data from the MIT–Hawaii Near-Earth Object Spectroscopic Survey, which has been observing asteroids for about 20 yr using a self-consistent observation technique. Twelve conservative candidates with spectra more than 3σ apart from each other at 2.4 μm and 52 optimistic candidates for surface heterogeneity are detected. These candidates include eight objects already reported as being heterogeneous. Our study suggests that the size boundary between small homogeneous asteroids and larger heterogeneous objects, if it exists, is lower than 100 km. A-type asteroids have a higher proportion of heterogeneous candidates than other asteroids. This may be because olivine, which is the main surface constituent of these objects, reacts more efficiently to space weathering with respect to pyroxene, such that a similar range of surface ages will translate into a wider range of optical-to-near-infrared spectral slopes in the case of A-type bodies.

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“…The key aspect of this work is the combination between the dynamical evolution of the particles and the modelling of the impact ejecta in order to estimate the number of potentially collectable particles. In an effort to have a more general understanding of the in-orbit collection scenarios, we compare different target asteroids based on their size and density, which can be derived and inferred from ground observations [29]. Additionally, we compare three different types of materials and several strength levels to understand the sensitivity of the collection scenarios to these parameters that have and intrinsically higher level of uncertainty.…”

Section: Introductionmentioning

confidence: 99%