Subaru Main Belt Asteroid Survey (SMBAS)—Size and color distributions of small main-belt asteroids

Yoshida, Fumi; Nakamura, T.

doi:10.1016/j.pss.2006.11.016

Cited by 75 publications

(73 citation statements)

References 13 publications

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“…To set r 0 , we rely on data for asteroids in the solar system, which have radii ranging from 100-300 km to 0.5-1 km (e.g., Yoshida et al 2003;Yoshida & Nakamura 2007;Gladman et al 2009). To sample this range, we consider r 0 = 0.1-100 km.…”

Section: Theoretical Backgroundmentioning

confidence: 99%

Numerical Simulations of Collisional Cascades at the Roche Limits of White Dwarf Stars

Kenyon

Bromley

2017

ApJ

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We consider the long-term collisional and dynamical evolution of solid material orbiting in a narrow annulus near the Roche limit of a white dwarf. With orbital velocities of 300 km s −1 , systems of solids with initial eccentricity e 10generate a collisional cascade where objects with radii r 100-300 km are ground to dust. This process converts 1-100 km asteroids into 1 µm particles in 10 2 − 10 6 yr. Throughout this evolution, the swarm maintains an initially large vertical scale height H. Adding solids at a rateṀ enables the system to find an equilibrium where the mass in solids is roughly constant. This equilibrium depends onṀ and r 0 , the radius of the largest solid added to the swarm. When r 0 10 km, this equilibrium is stable. For larger r 0 , the mass oscillates between high and low states; the fraction of time spent in high states ranges from 100% for largeṀ to much less than 1% for smallṀ . During high states, the stellar luminosity reprocessed by the solids is comparable to the excess infrared emission observed in many metallic line white dwarfs.

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Section: Theoretical Backgroundmentioning

confidence: 99%

Numerical Simulations of Collisional Cascades at the Roche Limits of White Dwarf Stars

Kenyon

Bromley

2017

ApJ

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“…The best two fields observed in good conditions in the ecliptic (2010 XC25 and 2009 CS, both far from opposition) give similar densities to each other and an average of 45 known MBAs and 90 unknown MBAs per square degree, thus a total of 135 Yoshida et al (2003) who counted 208 MBAs per square degree up to R ∼ 23.0 based on the opposition SMBAS-I survey and 182 MBAs per square degree to the same limit from the SMBAS-II survey (Yoshida and Nakamura, 2007). Based on our larger INT dataset, 41 known and 66 unknown MBAs per square degree could be detected in average in the observed fields.…”

Section: Unknown Mba Densitymentioning

confidence: 88%

739 observed NEAs and new 2–4 m survey statistics within the EURONEAR network

Văduvescu¹,

Birlan²,

Tudorica³

et al. 2013

Planetary and Space Science

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“…Since the size distribution changes for different size ranges and for very small objects is not well known, it is not easy to choose values for their parameters in the smaller size end of the distribution. As a first guess we used the size distribution proposed by Yoshida & Nakamura (2007) for objects with a radius between 500 m and 200 or 100 m, in spite that these authors proposed it for objects larger than 250 m. It is possible that this size distribution could be still valid for smaller objects (for example, for r < ∼ 100 m) producing a shallow size distribution and a shortage of small projectiles, making the ACO collisional reactivation process very improbable. Nevertheless, this shallow size distribution extended to very small sizes is difficult to reconcile with the cratering records of (243) Ida, (253) Mathilde, and (951) Gaspra (Chapman 2002).…”

Section: Discussionmentioning

confidence: 99%

“…The size distribution of very small main belt asteroids is not well known, so it is not easy to choose values for the parameters r c , K 0 , b 0 , K 1 , and b 1 . We decide to use two size distributions with r c = 200 m and 100 m, respectively, and to assume the size distribution proposed by Yoshida & Nakamura (2007) in the size range r c < r < 500 m (b 0 = 2.29), and a Dohnanyi (1969) size distribution for objects smaller than r c (b 1 = 3.5). Using this combined size distribution the total number of objects with a radius larger than 0.5 m is 1.42 × 10 13 in the first case and 6.11 × 10 12 in the second.…”

Section: Methodsmentioning

confidence: 99%

Collisional activation of asteroids in cometary orbits

Díaz¹,

Gil-Hutton²

2008

A&A

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Aims. We study the time an asteroid in a cometary orbit must wait to receive a collision producing a crater depth enough to expose subsurface volatiles, aiming to analyze the possibility of collisional reactivation of these objects if they are dormant comets. Methods. We perform a numerical integration of the asteroids in cometary orbits and a population of projectiles to find the mean intrinsic collision probabilities and mean impact velocities of the targets. The projectile population was obtained as a sample with the same distribution of orbital elements as observed for main belt asteroids, and we also take into account that its size distribution changes for different size ranges. Only 206 asteroids in cometary orbits, that are not members of other asteroid groups, with a Tisserand parameter 2 ≤ T J ≤ 2.9 and perihelion distance q > 1.3 AU were considered. Results. A large fraction of the objects in the sample receive at least 1 collision energetic enough to break the comet crust and allow a dormant comet to reach an active state in a period shorter than a Jupiter Family Comet dynamical lifetime. A large fraction of the objects in the sample with r t ≥ 8-9 km receive several collisions and could be active for more than 3 × 10 4 yr. We found an excess in the number of dormant comet candidates from the expected values which is indicative of the presence in the ACOs population of objects that are not comets in a dormant state. These objects could be asteroids with T J < 3 that reach their present orbits by some dynamical mechanism that perturbs the original asteroidal orbit changing its Tisserand invariant.

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Subaru Main Belt Asteroid Survey (SMBAS)—Size and color distributions of small main-belt asteroids

Cited by 75 publications

References 13 publications

Numerical Simulations of Collisional Cascades at the Roche Limits of White Dwarf Stars

Numerical Simulations of Collisional Cascades at the Roche Limits of White Dwarf Stars

739 observed NEAs and new 2–4 m survey statistics within the EURONEAR network

Collisional activation of asteroids in cometary orbits

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