P/2010 a2 Linear

Kleyna, Jan; Hainaut, Olivier; Meech, К. J.

doi:10.1051/0004-6361/201118428

Cited by 17 publications

(22 citation statements)

References 20 publications

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“…Because the P/2010 A2 dust particles have a composition that is similar to ordinary chondrites (Kim et al 2012), we assumed ρ d = 3000 kg m −3 , which is a typical value for their bulk density (Britt et al 2002). This assumption is consistent with previous research (Jewitt et al 2010Kleyna et al 2013). K = 5.7 × 10 −4 kg m −2 is a constant, and Q pr is a radiation pressure coefficient that we considered to be unity (Burns et al 1979).…”

Section: Model Descriptionsupporting

confidence: 91%

“…There are several ideas for the creation of the arc-like features. For example, assuming little or no radiation pressure, it would be possible to replicate arc features that are consistent with the images at a single epoch or for a certain short time duration Kleyna et al 2013). However, as we mentioned above, these models do not reproduce the morphology and brightness distribution at different epochs.…”

Section: Model Descriptionmentioning

confidence: 99%

“…Later, it became clear that the mass was ejected impulsively rather than continuously on a day in 2009 February or March by either an impact or rotational breakup (Jewitt et al 2010). Kleyna et al (2013) argued that the arcs are associated with an impact hollow cone, suggesting that a decameter-sized crater was formed on the LF. On the other hand, Agarwal et al (2013) studied the motions of subfragments using a series of high-resolution images taken by the Hubble Space Telescope (HST) from 2010 January to May and suggested that the mass was ejected in the equatorial plane of the LF by centrifugal force (called rotational breakup).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid^*

Kim

Ishiguro

Michikami

et al. 2017

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We revisited a mass ejection phenomenon that occurred in asteroid P/2010 A2 in terms of the dynamical properties of the dust particles and large fragments. We constructed a model assuming anisotropic ejection within a solid cone-shaped jet and succeeded in reproducing the time-variant features in archival observational images over ∼3 years from 2010 January to 2012 October. When we assumed that the dust particles and fragments were ejected in the same direction from a point where no object had been detected in any observations, the anisotropic model can explain all of the observations including (i) the unique dust cloud morphology, (ii) the trail surface brightness and (iii) the motions of the fragments. Our results suggest that the original body was shattered by an impact with the specific energy of Q * 350 J kg −1 , and remnants of slow antipodal ejecta (i.e., anisotropic ejection in our model) were observed as P/2010 A2. The observed quantities are consistent with those obtained through laboratory impact experiments, supporting the idea that the P/2010 A2 event is the first evidence of the impact shattering occurred in the present main asteroid belt.-2 -Subject headings: minor planets, asteroids: general -minor planets, asteroids: individual (P/2010 A2)

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Section: Model Descriptionsupporting

confidence: 91%

Section: Model Descriptionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid^*

Kim

Ishiguro

Michikami

et al. 2017

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“…The activity of P/2012 F5 (Stevenson et al 2012;Moreno et al 2012), 596 (Hsieh et al 2012a;Ishiguro et al 2011a,b;Jewitt et al 2011;Moreno et al 2012), and P/2010 A2 (Jewitt et al 2010;Snodgrass et al 2010;Jewitt et al 2011;Hainaut et al 2012b;Kim et al 2012;Kleyna et al 2013) has been interpreted as the effect of impacts by small asteroids.…”

Section: Introductionmentioning

confidence: 99%

Continued activity in P/2013 P5 PANSTARRS

Hainaut

Boehnhardt

Snodgrass

et al. 2014

A&A

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The object P/2013 P5 PANSTARRS was discovered in August 2013, displaying a cometary tail, but its orbital elements indicated that it was a typical member of the inner asteroid main belt. We monitored the object from 2013 August 30 until 2013 October 05 using the CFHT 3.6 m telescope (Mauna Kea, HI), the NTT (ESO, La Silla), the CA 1.23 m telescope (Calar Alto), the Perkins 1.8m (Lowell) and the 0.6 m TRAPPIST telescope (La Silla). We measured its nuclear radius to be r < ∼ 0.25−0.29 km, and its colours g − r = 0.58 ± 0.05 and r − i = 0.23 ± 0.06, typical for an S-class asteroid, as expected for an object in the inner asteroid belt and in the vicinity of the Flora collisional family. We failed to detect any rotational light curve with an amplitude <0.05 mag and a double-peaked rotation period <20 h. The evolution of the tail during the observations was as expected from a dust tail. A detailed Finson-Probstein analysis of deep images acquired with the NTT in early September and with the CFHT in late September indicated that the object was active since at least late January 2013 until the time of the latest observations in 2013 September, with at least two peaks of activity around 2013 June 14 ± 10 d and 2013 July 22 ± 3 d. The changes of activity level and the activity peaks were extremely sharp and short, shorter than the temporal resolution of our observations (∼1 d). The dust distribution was similar during these two events, with dust grains covering at least the 1-1000 µm range. The total mass ejected in grains <1 mm was estimated to be 3.0 × 10 6 kg and 2.6 × 10 7 kg around the two activity peaks. Rotational disruption cannot be ruled out as the cause of the dust ejection. We also propose that the components of a contact binary might gently rub and produce the observed emission. Volatile sublimation might also explain what appears as cometary activity over a period of 8 months. However, while main belt comets best explained by ice sublimation are found in the outskirts of the main belt, where water ice is believed to be able to survive buried in moderately large objects for the age of the solar system deeply, the presence of volatiles in an object smaller than 300 m in radius would be very surprising in the inner asteroid belt.

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“…The disrupted P/2010 A2 went unobserved from this initial event to (pre-discovery) observations taken in 2009 November 22 (Jewitt et al 2011a). The basic features and possible interpretation of P/2010 A2 have been confirmed by a number of independent investigators (Paper 1; Snodgrass et al 2010;Hainaut et al 2012;Kim et al 2012;Kleyna et al 2013). In particular, Kleyna et al (2013) have presented a detailed impact model that purports to fit many of the observed properties of the tail structure.…”

Section: Introductionmentioning

confidence: 77%

Dynamics of Large Fragments in the Tail of Active Asteroid P/2010 A2

Agarwal

Jewitt

Weaver

2013

ApJ

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We examine the motions of large fragments at the head of the dust tail of active asteroid P/2010 A2. In previous work we showed that these fragments were ejected from the primary nucleus in early 2009, either following a hypervelocity impact or by rotationally induced break-up. Here, we follow their positions through a series of Hubble Space Telescope images taken during the first half of 2010. The orbital evolution of each fragment allows us to constrain its velocity relative to the main nucleus after leaving its sphere of gravitational influence.We find that the fragments constituting a prominent X-shaped tail feature were emitted in a direction opposite to the motion of the asteroid and towards the south of its orbital plane. Derived emission velocities of these primary fragments range between 0.02 and 0.3 m s −1 , comparable to the ∼0.08 m s −1 gravitational escape speed from the nucleus. Their sizes are on the order of decimeters or larger. We obtain the best fits to our data with ejection velocity vectors lying in a plane that includes the nucleus. This may suggest that the cause of the disruption of P/2010 A2 is rotational break-up.Subject headings: minor planets, asteroids: general -minor planets, asteroids: individual (P/2010 A2)

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P/2010 a2 Linear

Cited by 17 publications

References 20 publications

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid^*

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid^*

Continued activity in P/2013 P5 PANSTARRS

Dynamics of Large Fragments in the Tail of Active Asteroid P/2010 A2

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P/2010 a2 Linear

Cited by 17 publications

References 20 publications

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid*

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid*

Continued activity in P/2013 P5 PANSTARRS

Dynamics of Large Fragments in the Tail of Active Asteroid P/2010 A2

Contact Info

Product

Resources

About

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid^*

Anisotropic Ejection from Active Asteroid P/2010 A2: An Implication of Impact Shattering on an Asteroid^*