P/2010 a2 Linear

Hainaut, Olivier; Kleyna, Jan; Sarid, Gal; Hermalyn, B.; Zenn, A.; Meech, К. J.; Schultz, P. H.; Hsieh, Henry H.; Trancho, Gelys; Pittichová, J.; Yang, Bin

doi:10.1051/0004-6361/201118147

Cited by 27 publications

(35 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Moreover, the dust morphology is very different from that of impacttriggered emissions, such as that in P/2010 A2 (Hainaut et al 2012b) or in (596) Scheila (Ishiguro et al 2011a). We consider a series of impacts hitting P5 several times during 2013 as implausible.…”

Section: Discussionmentioning

confidence: 99%

“…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%

“…Rotational light curves of asteroids suggest that objects larger than 150 m in diameter are inside the limit for losing mass at the equator (Pravec et al 2002), which suggests that this process might be in effect. Because P/2012 A2 is a very small object (∼100 m radius postemission, Jewitt et al 2010;Hainaut et al 2012b, the matter ejected amounts to a very small change of the radius), this is quite plausible. For completeness, the YORP effect is also believed to be able to cause a catastrophic break-up of the object, a scenario incompatible with these observations.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Continued activity in P/2013 P5 PANSTARRS

Hainaut

Boehnhardt

Snodgrass

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Continued activity in P/2013 P5 PANSTARRS

Hainaut

Boehnhardt

Snodgrass

et al. 2014

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Various approaches have been used for this type of general dust and debris fitting. For example, Jorda et al (2007) modeled 1 β is the ratio of radiation pressure to gravity, as defined in Hainaut et al (2012).…”

Section: Modeling the Dust Distribution -A Simple Binary Envelope Fitmentioning

confidence: 99%

P/2010 a2 Linear

Kleyna

Hainaut

Meech

2012

A&A

Self Cite

View full text Add to dashboard Cite

P/2010 A2 is an object on an asteroidal orbit that was observed to have an extended tail or debris trail in January 2010. In this work, we fit the outburst of P/2010 A2 with a conical burst model, and verify previous suspicions that this was a one-time collisional event rather than a sustained cometary outburst, implying that P/2010 A2 is not a new main belt comet driven by ice sublimation. We find that the best-fit cone opening angle is ∼40• to ∼50• , in agreement with numerical and laboratory simulations of cratering events. Mapping debris orbits to sky positions suggests that the distinctive arc features in the debris correspond to the same debris cone inferred from the extended dust. From the velocity of the debris, and from the presence of a velocity maximum at around 15 cm s −1 , we infer that the surface of A2 probably has a very low strength ( 1 kPa), comparable to lunar regolith.

show abstract

“…Other active asteroids have also been associated with other asteroid families including 311P/PANSTARRS, 313P/Gibbs, 354P/LINEAR, 358P/PANSTARRS, and (62412) 2000 SY 178 (Hainaut et al 2012;Hsieh et al 2013Hsieh et al , 2015aJewitt et al 2013;. However, only some of these associations were formally established using standard family-linking techniques.…”

Section: Asteroid Family Associationsmentioning

confidence: 99%

Asteroid Family Associations of Active Asteroids

Hsieh

Novaković

Kim

et al. 2018

View full text Add to dashboard Cite

We report on the results of a systematic search for associated asteroid families for all active asteroids known to date. We find that 10 out of 12 main-belt comets (MBCs) and 5 out of 7 disrupted asteroids are linked with known or candidate families, rates that have ∼0.1% and ∼6% probabilities, respectively, of occurring by chance, given an overall family association rate of 37% for asteroids in the inner solar system. We find previously unidentified family associations between 238P/Read and the candidate Gorchakov family, 311P/PANSTARRS and the candidate Behrens family, 324P/La Sagra and the Alauda family, 354P/LINEAR and the Baptistina family, P/2013 R3-B (Catalina-PANSTARRS) and the Mandragora family, P/2015 X6 (PANSTARRS) and the Aeolia family, P/2016 G1 (PANSTARRS) and the Adeona family, and P/2016 J1-A/B (PANSTARRS) and the Theobalda family. All MBCs with family associations belong to families that contain asteroids with primitive taxonomic classifications and low average reported albedos (p V 0.10), while disrupted asteroids with family associations belong to families that contain asteroids that span wider ranges of taxonomic types and average reported albedos (0.06 < p V < 0.25). These findings are consistent with MBC activity being closely correlated to composition (i.e., whether an object is likely to contain ice), while disrupted asteroid activity is not as sensitive to composition. Given our results, we describe a sequence of processes by which the formation of young asteroid families could lead to the production of present-day MBCs.

show abstract

P/2010 a2 Linear

Cited by 27 publications

References 72 publications

Continued activity in P/2013 P5 PANSTARRS

Continued activity in P/2013 P5 PANSTARRS

P/2010 a2 Linear

Asteroid Family Associations of Active Asteroids

Contact Info

Product

Resources

About