Fragmented Comet 73P/Schwassmann–Wachmann 3

Graykowski, Ariel; Jewitt, and David

doi:10.3847/1538-3881/ab2f7a

Cited by 3 publications

(1 citation statement)

References 22 publications

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“…where C D ∼1 is a dimensionless drag coefficient which depends on the shape and nature of the grain and v gas is the thermal speed of gas molecules. We set a c =1 mm-1 cm using v gas =490 m s −1 (Equation (10) of Graykowski & Jewitt 2019) and (dm/dt) ice = 8×10 −4 kg m −2 s −1 and again take the same values of G, ρ and D p . We then find r ice > 3-25 m corresponding to the fractional area of (sub)surface ice ∼ 0.001-0.05 %.…”

Section: Sublimation Of Water Icementioning

confidence: 99%

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT₁

Kasuga

Sato

Ueda

et al. 2020

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We present a fireball detected in the night sky over Kyoto, Japan on UT 2017 April 28 at 15 h 58 m 19 s by the SonotaCo Network. The absolute visual magnitude is M v =−4.10±0.42 mag. Luminous light curves obtain a meteoroid mass m=29±1 g, corresponding to the size a s =2.7±0.1 cm. Orbital similarity assessed by D-criterions (cf. D SH =0.0079) has identified a likely parent, the binary near-Earth asteroid (164121) 2003 YT 1 . The suggested binary formation process is a YORP-driven rotational disintegration (Pravec & Harris 2007). The asynchronous state indicates the age of < 10 4 yr, near or shorter than the upper limit to meteoroid stream lifetime. We examine potential dust production mechanisms for the asteroid, including rotational instability, resurfacing, impact, photoionization, radiation pressure sweeping, thermal fracture and sublimation of ice. We find some of them capable of producing the meteoroid-scale particles. Rotational instability is presumed to cause mass shedding, in consideration of the recent precedents (e.g. asteroid (6478) Gault), possibly releasing mm-cm scale dust particles. Impacts by micrometeorites with size ≃ 1 mm could be a trigger for ejecting the cm-sized particles. Radiation pressure can sweep out the mm-sized dust particles, while not sufficient for the cm-sized. For the other mechanisms, unprovable or unidentified. The feasibility in the parental aspect of 2003 YT 1 is somewhat reconciled with the fireball observation, yielding an insight into how we approach potentially hazardous objects.

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Section: Sublimation Of Water Icementioning

confidence: 99%

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT₁

Kasuga

Sato

Ueda

et al. 2020

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Comparing the dynamics of Jupiter-family Comets and comet-like fireballs

Shober,

Tancredi,

Vaubaillon

et al. 2024

A&A

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Jupiter-family comets (JFCs), which originate from the Kuiper belt and scattered disk, exhibit low-inclination and chaotic trajectories due to close encounters with Jupiter. Despite their typically short incursions into the inner solar system, a notable number of them are on Earth-crossing orbits, with fireball networks detecting many objects on ``JFC-like'' ($2<T_ J <3$) orbits. This investigation aims to examine the orbital dynamics of JFCs and comet-like fireballs over $10^ $\,yr timescales, focusing on the trajectories and stability of these objects in the context of gravitational interactions within the solar system. We employed an extensive fireball dataset from Desert Fireball Network (DFN), European Fireball Network (EFN), Fireball Recovery and InterPlanetary Observation Network (FRIPON), and Meteorite Observation and Recovery Project (MORP), alongside telescopically observed cometary ephemeris from the NASA HORIZONS database. The study integrates 646 fireball orbits with 661 JFC orbits for a comparative analysis of their orbital stability and evolution. The analysis confirms frequent Jupiter encounters among most JFCs, inducing chaotic orbital behavior with limited predictability and short Lyapunov lifetimes (sim 120 years), underscoring Jupiter's significant dynamical influence. In contrast, "JFC-like" meteoroids detected by fireball networks largely exhibit dynamics divergent from genuine JFCs, with 79-92<!PCT!> on ``JFC-like'' orbits shown not to be prone to frequent Jupiter encounters; in particular, only 1-5<!PCT!> of all fireballs detected by the four networks exhibit dynamics similar to that of actual JFCs. In addition, 22<!PCT!> (16 of 72) of near-Earth JFCs are on highly stable orbits, suggesting a potential main belt origin for some of the bodies. This extensive study delineates the stark dynamical contrast between JFCs and JFC-like meteoroids detected by global fireball networks. The majority of centimeter- and meter-scale meteoroids on JFC-like orbits exhibit remarkably stable trajectories, which starkly differ from the chaotic paths of their km-scale counterparts. Our findings suggest that the JFC-like objects observed by fireball networks predominantly originate from the outer main belt, with only a minor fraction being directly attributable to traditional JFCs.

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WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC

Kasuga

Masiero

2022

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We present space-based thermal infrared observations of the presumably Geminid-associated asteroids: (3200) Phaethon, 2005 UD, and 1999 YC using Wide-field Infrared Survey Explorer/Near-Earth Object WISE. The images were taken at the four wavelength bands 3.4 μm (W1), 4.6 μm (W2), 12 μm (W3), and 22 μm (W4). We find no evidence of lasting mass loss in the asteroids over the decadal multiepoch data sets. We set an upper limit to the mass-loss rate in dust of Q dust ≲ 2 kg s−1 for Phaethon and ≲0.1 kg s−1 for both 2005 UD and 1999 YC, respectively, with little dependency over the observed heliocentric distances of R h = 1.0–2.3 au. For Phaethon, even if the maximum mass loss was sustained over the 1000(s) yr dynamical age of the Geminid stream, it is more than two orders of magnitude too small to supply the reported stream mass (1013–14 kg). The Phaethon-associated dust trail (Geminid stream) is not detected at R h = 2.3 au, corresponding to an upper limit on the optical depth of τ < 7 × 10−9. Additionally, no comoving asteroids with radii r e < 650 m were found. The DESTINY+ dust analyzer would be capable of detecting several of the 10 μm sized interplanetary dust particles when at far distances (≳50,000 km) from Phaethon. From 2005 UD, if the mass-loss rate lasted over the 10,000 yr dynamical age of the Daytime Sextantid meteoroid stream, the mass of the stream would be ∼1010 kg. The 1999 YC images showed neither the related dust trail (the optical depth τ < 2 × 10−8) nor comoving objects with radii r e < 170 m at R h = 1.6 au. Estimated physical parameters from these limits do not explain the production mechanism of the Geminid meteoroid stream. Lastly, to explore the origin of the Geminids, we discuss the implications for our data in relation to the possibly sodium-driven perihelion activity of Phaethon.

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Fragmented Comet 73P/Schwassmann–Wachmann 3

Cited by 3 publications

References 22 publications

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT₁

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT₁

Comparing the dynamics of Jupiter-family Comets and comet-like fireballs

WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC

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Fragmented Comet 73P/Schwassmann–Wachmann 3

Cited by 3 publications

References 22 publications

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT1

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT1

Comparing the dynamics of Jupiter-family Comets and comet-like fireballs

WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC

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A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT₁

A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT₁