Large Particles in Active Asteroid P/2010 A2

Jewitt, David; Ishiguro, Masateru; Agarwal, Jessica

doi:10.1088/2041-8205/764/1/l5

Cited by 30 publications

(41 citation statements)

References 23 publications

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“…where H R is the R-band absolute magnitude, D is the diameter inkilometers, p R is the R-band geometric albedo, and 1130 is the conversion constant adopted from Jewitt et al (2013). Three empirical albedo values, p R = 0.20, 0.08, and 0.04, were assumed for asteroids in the inner (2.1<a<2.5 au), mid (2.5<a<2.8 au), and outer (a>2.8 au) main belts, respectively (Tedesco et al 2005).…”

Section: Rotation-period Analysismentioning

confidence: 99%

Large Super-Fast Rotator Hunting Using the Intermediate Palomar Transient Factory

Lin

et al. 2016

ApJS

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In order to look for large super-fast rotators, in late 2014 and early 2015, five dedicated surveys covering ∼188deg 2 in the ecliptic plane have been carried out in the R-band, with ∼10 minute cadence using the intermediate Palomar Transient Factory. Among 1029 reliable rotation periods obtained from the surveys, we discovered 1 new large super-fast rotator, (40511) 1999 RE88, and 18 other candidates. (40511) 1999 RE88 is an S-type inner main-belt asteroid with a diameter of D=1.9±0.3 km, a rotation period of P=1.96±0.01 hr, and a light curve amplitude of Δm∼1.0 mag. To maintain such fast rotation, an internal cohesive strength of ∼780 Pa is required. Combining all known large super-fast rotators, their cohesive strengths all fall in the range of 100-1000 Pa of lunar regolith. However, the number of large super-fast rotators seems to be far less than the whole asteroid population. This might indicate a peculiar asteroid group for them. Although the detection efficiency for a long rotation period is greatly reduced due to our two-day observation time span, the spin-rate distributions of this work show consistent results with Chang et al. (2015), after considering the possible observational bias in our surveys. It shows a number decrease with an increase of spin rate for asteroids with a diameter of 3D15 km, and a number drop at a spin rate of f=5 rev day −1 for asteroids with D3 km.

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Section: Rotation-period Analysismentioning

confidence: 99%

Large Super-Fast Rotator Hunting Using the Intermediate Palomar Transient Factory

Lin

et al. 2016

ApJS

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“…The rapid rotation of the primary body has been considered to be a key feature of rotationally disrupted asteroids. For a strengthless elongated body, the critical spin period for breakup (at which the gravitational acceleration equals the centripetal acceleration at the equator) is given by Jewitt (2012)…”

Section: Discussionmentioning

confidence: 99%

New Observational Evidence of Active Asteroid P/2010 A2: Slow Rotation of the Largest Fragment

Kim

Ishiguro

Lee

2017

ApJL

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We report new observations of the active asteroid P/2010 A2 taken when it made its closest approach to the Earth (1.06 au in 2017 January) after its first discovery in 2010. Despite a crucial role of the rotational period in clarifying its ejection mechanism, the rotational property of P/2010 A2 has not yet been studied due to the extreme faintness of this tiny object (∼120 m in diameter). Taking advantage of the best observing geometry since the discovery, we succeed in obtaining the rotational light curve of the largest fragment with Gemini/GMOS-N. We find that (1) the largest fragment has a double-peaked period of 11.36 ± 0.02 hr spinning much slower than its critical spin period; (2) the largest fragment is a highly elongated object (a/b 1.94) with an effective radius of 61.9 +16.8 −9.2 m; (3) the size distribution of the ejecta follows a broken power law (the power indices of the cumulative size distributions of the dust and fragments are 2.5 ± 0.1 and 5.2 ± 0.1, respectively); (4) the mass ratio of the largest fragment to the total ejecta is around 0.8; and (5) the dust cloud morphology is in agreement with the anisotropic ejection model in Kim et al. (2017). These new characteristics of the ejecta obtained in this work are favorable to the impact shattering hypothesis. Subject headings: minor planets, asteroids: individual (P/2010 A2)

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“…large particles, and therefore does not necessarily indicate that ongoing dust production was actually present at the time (e.g., Jewitt et al 2013). …”

Section: Discussionmentioning

confidence: 99%

The reactivation of main-belt Comet 324P/La Sagra (P/2010 R2)

Hsieh¹,

Sheppard²

2015

Monthly Notices of the Royal Astronomical Society: Letters

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We present observations using the Baade Magellan and Canada-France-Hawaii telescopes showing that main-belt comet 324P/La Sagra, formerly known as P/2010 R2, has become active again for the first time since originally observed to be active in [2010][2011]. The object appears point-source-like in March and April 2015 as it approached perihelion (true anomaly of ν ∼ 300• ), but was ∼1 mag brighter than expected if inactive, suggesting the presence of unresolved dust emission. Activity was confirmed by observations of a cometary dust tail in May and June 2015. We find an apparent net dust production rate ofṀ d 0.1 kg s −1 during these observations. 324P is now the fourth main-belt comet confirmed to be recurrently active, a strong indication that its activity is driven by sublimation. It now has the largest confirmed active range of all likely main-belt comets, and also the most distant confirmed inbound activation point at R ∼ 2.8 AU. Further observations during the current active period will allow direct comparisons of activity strength with 324P's 2010 activity.

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Large Particles in Active Asteroid P/2010 A2

Cited by 30 publications

References 23 publications

Large Super-Fast Rotator Hunting Using the Intermediate Palomar Transient Factory

Large Super-Fast Rotator Hunting Using the Intermediate Palomar Transient Factory

New Observational Evidence of Active Asteroid P/2010 A2: Slow Rotation of the Largest Fragment

The reactivation of main-belt Comet 324P/La Sagra (P/2010 R2)

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