Active Asteroid P/2017 S5 (ATLAS)

Jewitt, David; Kim, Yoonyoung; Rajagopal, Jayadev; Ridgway, Susan E.; Kotulla, Ralf; Liu, Wilson; Mutchler, Max; Li, Jing; Weaver, H. A.; Larson, S. M.

doi:10.3847/1538-3881/aaf563

“…This corresponds to the dust velocity V = 40 β/1.78 = 30 √ β m s −1 , broadly consistent with V ⊥ ∼ 20 √ β m s −1 inferred from the perpendicular profile (Section 3.3). Similar model parameters were found for MBCs 238P, 324P, 358P, and P/2017 S5 (Hsieh et al 2009;Moreno et al 2011Moreno et al , 2013Jewitt et al 2019), indicating that these objects share similar properties of the ejected dust.…”

Section: Particle Propertiessupporting

confidence: 68%

Sublimation origin of active asteroid P/2018 P3

Kim

¹

,

Agarwal

²

,

Jewitt

³

et al. 2022

A&A

Self Cite

3

1

0

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Context. Active asteroids show (typically transient) cometary activity, driven by a range of processes. A sub-set, sometimes called main-belt comets, may be driven by sublimation and so could be useful for tracing the present-day distribution of asteroid ice. Object P/2018 P3 has a Tisserand parameter 3.096 but a high eccentricity 0.415, placing it within the dynamical boundary between asteroids and comets. Aims. We aim to determine the cause of activity (sublimation or something else) and assess the dynamical stability of P3, in order to better constrain the intrinsic ice content in the main belt. Methods. We obtained Hubble Space Telescope images of P3 at the highest angular resolution. We compared the observations with a Monte Carlo model of dust dynamics. We identified and analyzed archival CFHT (2013) and NEOWISE (2018) data. In addition, we numerically integrated the orbits of P3 clones for 100 Myr. Results. P3 has been recurrently active near two successive perihelia (at 1.76 AU), indicative of a sublimation origin. The absence of 4.6 µm band excess indicates zero or negligible CO or CO 2 gas production from P3. The properties of the ejected dust are remarkably consistent with those found in other main-belt comets (continuous emission of ∼0.05-5 mm particles at 0.3-3 m s −1 speeds), with mass-loss rates of 2 kg s −1 . The orbit of P3 is unstable on timescales ∼10 Myr. Conclusions. We speculate that P3 has recently arrived from a more stable source (either the Kuiper Belt or elsewhere in the main belt) and has been physically aged at its current location, finally becoming indistinguishable from a weakly sublimating asteroid in terms of its dust properties. Whatever the source of P3, given the dynamical instability of its current orbit, P3 should not be used to trace the native distribution of asteroid ice.

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“…The 427P (P/2017 S5) is interesting from another point of view. Its time-series photometry lightcurve indicates possibly rapid rotation with a period of 1.4 h. Though this period is yet to be confirmed, Jewitt et al (2019) suggested that, if real, it may also play a role in the mass loss. The authors further suggested that such a rapid rotation could be a consequence of spin-up by sublimation torques.…”

Section: Main Properties Of Three Families Associated With the Most Mbcsmentioning

confidence: 98%

Asteroid families: properties, recent advances, and future opportunities

Novaković

¹

,

Vokrouhlický

²

,

Spoto

³

et al. 2022

Celest Mech Dyn Astron

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Collisions are one of the key processes shaping planetary systems. Asteroid families are outcomes of such collision still identifiable across our solar system. The families provide a unique view of catastrophic disruption phenomena and have been in the focus of planetary scientists for more than a century. Most of them are located in the main belt, a ring of asteroids between Mars and Jupiter. Here we review the basic properties of the families, discuss some recent advances, and anticipate future challenges. This review pays more attention to dynamic aspects such as family identification, age determination, and long-term evolution. The text, however, goes beyond that. Especially, we cover the details of young families that see the major advances in the last years, and we anticipate it will develop even faster in the future. We also discuss the relevance of asteroid families for water-ice content in the asteroid belt and our current knowledge on links between families and main-belt comets. query Please check the edit made in the article title.

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“…Comet 427P/ATLAS (hereafter 427P), previously designated P/2017 S5, was discovered on 2017 September 27 by the Asteroid Terrestrial-impact Last Alert System (ATLAS) survey telescope (Heinze et al 2017) when the object was at ν = 21.3°, r h = 2.214 au, and Δ = 1.267 au. Jewitt et al (2019) conducted an observational analysis shortly after its discovery, finding that the comet's activity was due to a prolonged dust-emission event occurring over ∼150 days, consistent with sublimation-driven emission. Using follow-up observations obtained using HST the following year when the object was apparently inactive, Jewitt et al (2019) also estimated 427P's nucleus to have an effective radius of 450 60 100 -+ m, assuming an albedo of p = 0.06 ± 0.02.…”

Section: P/atlasmentioning

confidence: 99%

Observational Characterization of Main-belt Comet and Candidate Main-belt Comet Nuclei

Hsieh¹,

Micheli²,

Kelley³

et al. 2023

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We report observations of nine main-belt comets (MBCs) or candidate MBCs, most of which were obtained when the targets were apparently inactive. We find effective nucleus radii (assuming albedos of p V = 0.05 ± 0.02) of r n = (0.24 ± 0.05) km for 238P/Read, r n = (0.9 ± 0.2) km for 313P/Gibbs, r n = (0.6 ± 0.1) km for 324P/La Sagra, r n = (1.0 ± 0.2) km for 426P/PANSTARRS, r n = (0.5 ± 0.1) km for 427P/ATLAS, r n < (0.3 ± 0.1) km for P/2016 J1-A (PANSTARRS), r n < (0.17 ± 0.04) km for P/2016 J1-B (PANSTARRS), r n ≤ (0.5 ± 0.2) km for P/2017 S9 (PANSTARRS), recently redesignated 455P/PANSTARRS, and r n = (0.4 ± 0.1) km for P/2019 A3 (PANSTARRS). We identify evidence of activity in observations of 238P in 2021, and find similar inferred activity onset times and net initial mass-loss rates for 238P during perihelion approaches in 2010, 2016, and 2021. P/2016 J1-A and P/2016 J1-B are also found to be active in 2021 and 2022, making them collectively the tenth MBC confirmed to be recurrently active near perihelion and therefore likely to be exhibiting sublimation-driven activity. The nucleus of 313P is found to have colors of g ′ − r ′ = 0.52 ± 0.05 and r ′ − i ′ = 0.22 ± 0.07 , consistent with 313P being a Lixiaohua family member. We also report nondetections of P/2015 X6 (PANSTARRS), where we conclude that its current nucleus size is likely below our detection limits (r n ≲ 0.3 km). Lastly, we find that of 17 MBCs or candidate MBCs for which nucleus sizes (or inferred parent body sizes) have been estimated, >80% have r n ≤ 1.0 km, pointing to an apparent physical preference toward small MBCs, where we suggest that Yarkovsky–O’Keefe–Radzievskii–Paddack spin-up may play a significant role in triggering and/or facilitating MBC activity.

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Active Asteroid P/2017 S5 (ATLAS)

Cited by 10 publications

References 23 publications

Sublimation origin of active asteroid P/2018 P3

Sublimation origin of active asteroid P/2018 P3

Asteroid families: properties, recent advances, and future opportunities

Observational Characterization of Main-belt Comet and Candidate Main-belt Comet Nuclei

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