Interpretation of (596) Scheila's Triple Dust Tails

Ishiguro, Masateru; Hanayama, H.; Hasegawa, Susumu; Sarugaku, Yuki; Watanabe, J.; Fujiwara, Hideaki; Terada, Hiroshi; Hsieh, Henry H.; Vaubaillon, Jérémie; Kawai, N.; Yanagisawa, K.; Kuroda, D.; Miyaji, Takeshi; Fukushima, Hideo; Ohta, Kouji; Hamanowa, Hiromi; Kim, Junhan; Pyo, Jeonghyun; Nakamura, Akiko

doi:10.1088/2041-8205/741/1/l24

Cited by 48 publications

(50 citation statements)

References 20 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The comet also exhibits a diffuse coma and a featureless fan-like tail that remains aligned with the antisolar direction, distinctly different from the crossed filamentary structure of P/2010 A2's tail, the three-plumed morphology of (596) Scheila's dust tail, and the orbit-plane-aligned dust trail of P/2012 F5 Ishiguro et al 2011;Stevenson et al 2012;Moreno et al 2012). The post-perihelion peaking of P/2012 T1's activity is also consistent with the post-perihelion peaking of activity for other MBCs (Hsieh et al 2012c).…”

Section: Discussionmentioning

confidence: 90%

Main-Belt Comet P/2012 T1 (Panstarrs)

Hsieh

Kaluna

Novaković

et al. 2013

ApJ

Self Cite

View full text Add to dashboard Cite

We present initial results from observations and numerical analyses aimed at characterizing the main-belt comet P/2012 T1 (PANSTARRS). Optical monitoring observations were made between 2012 October and 2013 February using the University of Hawaii 2.2 m telescope, the Keck I telescope, the Baade and Clay Magellan telescopes, Faulkes Telescope South, the Perkins Telescope at Lowell Observatory, and the Southern Astrophysical Research Telescope. The object's intrinsic brightness approximately doubles from the time of its discovery in early October until mid-November and then decreases by ∼60% between late December and early February, similar to photometric behavior exhibited by several other main-belt comets and unlike that exhibited by disrupted asteroid (596) Scheila. We also used Keck to conduct spectroscopic searches for CN emission as well as absorption at 0.7 μm that could indicate the presence of hydrated minerals, finding an upper limit CN production rate of Q CN < 1.5 × 10 23 mol s −1 , from which we infer a water production rate of Q H 2 O < 5 × 10 25 mol s −1 , and no evidence of the presence of hydrated minerals. Numerical simulations indicate that P/2012 T1 is largely dynamically stable for >100 Myr and is unlikely to be a recently implanted interloper from the outer solar system, while a search for potential asteroid family associations reveals that it is dynamically linked to the ∼155 Myr old Lixiaohua asteroid family.

show abstract

Section: Discussionmentioning

confidence: 90%

Main-Belt Comet P/2012 T1 (Panstarrs)

Hsieh

Kaluna

Novaković

et al. 2013

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…Many different physical mechanisms operate to account for mass loss from the active asteroids (Jewitt 2012). For example, 100 km -sized (596) Scheila ejected dust following the impact of a ∼30 meter sized projectile (Bodewits et al 2011, Jewitt et al 2011, Ishiguro et al 2011, Bodewits et al 2014. The tiny (∼100 meter diameter) active asteroid P/2010 A2 is either impact-produced or the result of rotational breakup, perhaps driven by radiation torques (Jewitt et al 2010, Agarwal et al 2013.…”

Section: Introductionmentioning

confidence: 99%

Hubble and Keck Telescope Observations of Active Asteroid 288p/300163 (2006 Vw139)

Agarwal

Jewitt

Weaver

et al. 2015

View full text Add to dashboard Cite

We present Hubble Space Telescope (HST) and Keck 10 m telescope observations of active asteroid 288P/300163 (2006 VW139) taken to examine ejected dust. The nucleus is a C-type object with absolute magnitude H V = 17.0 ± 0.1 and estimated diameter ∼2.6 km (for assumed visual geometric albedo p V = 0.04). Variations in the brightness of the nucleus at the 10%-15% level are significant in both 2011 December and 2012 October but we possess too few data to distinguish variations caused by activity from those caused by rotation. The dust scattering cross-section in 2011 December is ∼40 km 2 , corresponding to a dust mass ∼9 × 10 6 kg (88 μm mean particle radius assumed). The FWHM of the debris sheet varies from ∼100 km near the nucleus to ∼1000 km 30″ (40,000 km) east of it. Dust dynamical models indicate ejection speeds between 0.06 and 0.3 m s −1 , particle sizes between 10 and 300 μm and an inverse square-root relation between particle size and velocity. Overall, the data are most simply explained by prolonged, low velocity ejection of dust, starting in or before 2011 July and continuing until at least 2011 October. These properties are consistent with the sublimation of near-surface ice aided by centrifugal forces. The high spatial resolution of our HST images (52 km pixel −1 ) reveals details that remained hidden in previous ground-based observations, such as the extraordinarily small vertical extent of the dust sheet, ejection speeds well below the nucleus escape speed, and the possibility of a binary nucleus.

show abstract

“…Active asteroids have orbits typical of asteroids (with a Tisserand parameter relative to Jupiter >3, Kresák 1972), but temporarily display dust activity similar to comets (Hsieh & Jewitt 2006;Jewitt 2012;Jewitt et al 2015b). While cometary activity is generally thought to be driven by the sublimation of embedded volatiles (Whipple 1950), the situation is likely more diverse in asteroids.…”

Section: Introductionmentioning

confidence: 99%

Nucleus of active asteroid 358P/Pan-STARRS (P/2012 T1)

Agarwal

Mommert

2018

A&A

View full text Add to dashboard Cite

Context. The dust emission from active asteroids is likely driven by collisions, fast rotation, sublimation of embedded ice, and combinations of these. Characterising these processes leads to a better understanding of their respective influence on the evolution of the asteroid population. Aims. We study the role of fast rotation in the active asteroid 358P (P 2012/T1). Methods. We obtained two nights of deep imaging of 358P with SOAR/Goodman and VLT/FORS2. We derived the rotational light curve from time-resolved photometry and searched for large fragments and debris >8 mm in a stacked, ultra-deep image. Results. The nucleus has an absolute magnitude of m R =19.68, corresponding to a diameter of 530 m for standard assumptions on the albedo and phase function of a C-type asteroid. We do not detect fragments or debris that would require fast rotation to reduce surface gravity to facilitate their escape. The 10-hour light curve does not show an unambiguous periodicity.

show abstract

Interpretation of (596) Scheila's Triple Dust Tails

Cited by 48 publications

References 20 publications

Main-Belt Comet P/2012 T1 (Panstarrs)

Main-Belt Comet P/2012 T1 (Panstarrs)

Hubble and Keck Telescope Observations of Active Asteroid 288p/300163 (2006 Vw139)

Nucleus of active asteroid 358P/Pan-STARRS (P/2012 T1)

Contact Info

Product

Resources

About