Evidence of surface heterogeneity on active asteroid (3200) Phaethon

MacLennan, Eric; Marshall, Sean; Granvik, Mikael

doi:10.1016/j.icarus.2022.115226

Cited by 9 publications

(9 citation statements)

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“…Photometric modeling of such a spotted surface could provide insight on whether this interpretation is physically plausible, but this is beyond the scope of this work. Notably, a recent study by MacLennan et al (2022) found evidence that Phaethon's surface is heterogeneous as a function of latitude, which adds merit to the above hypothesis. Future multicolor photometric observations could provide further insight into 2005 UDʼs surface properties.…”

Section: Surface Colorsmentioning

confidence: 90%

Implications for the Formation of (155140) 2005 UD from a New Convex Shape Model

et al. 2023

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(155140) 2005 UD has a similar orbit to (3200) Phaethon, an active asteroid in a highly eccentric orbit thought to be the source of the Geminid meteor shower. Evidence points to a genetic relationship between these two objects, but we have yet to fully understand how 2005 UD and Phaethon could have separated into this associated pair. Presented herein are new observations of 2005 UD from five observatories that were carried out during the 2018, 2019, and 2021 apparitions. We implemented light curve inversion using our new data, as well as dense and sparse archival data from epochs in 2005–2021, to better constrain the rotational period and derive a convex shape model of 2005 UD. We discuss two equally well-fitting pole solutions (λ = 116.°6, β = −53.°6) and (λ = 300.°3, β = −55.°4), the former largely in agreement with previous thermophysical analyses and the latter interesting due to its proximity to Phaethon’s pole orientation. We also present a refined sidereal period of P sid = 5.234246 ± 0.000097 hr. A search for surface color heterogeneity showed no significant rotational variation. An activity search using the deepest stacked image available of 2005 UD near aphelion did not reveal a coma or tail but allowed modeling of an upper limit of 0.04–0.37 kg s−1 for dust production. We then leveraged our spin solutions to help limit the range of formation scenarios and the link to Phaethon in the context of nongravitational forces and timescales associated with the physical evolution of the system.

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Section: Surface Colorsmentioning

confidence: 90%

Implications for the Formation of (155140) 2005 UD from a New Convex Shape Model

et al. 2023

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“…The size is consistent within 2σ of the other TPM result D e = 5.1 ± 0.2 km (Hanuš et al 2016(Hanuš et al , 2018, while not consistent with D e ∼ 5.5 km showing a muffin-top shape (equatorial bulge of 6.3 km) as observed by Arecibo radar during the apparition in 2017 December (Taylor et al 2019). The shape model or observed orbital positions (preor post-q) may require some offsets in size estimations and thermophysical behavior (MacLennan & Emery 2021;MacLennan et al 2022). Here, we describe the justification for applying the WISE/NEOWISE-derived size with its spherical assumption.…”

Section: Wise/neowise Datamentioning

confidence: 99%

“…The infrared data do not resolve a 5-6 km asteroidal shape, indicating that the assumption of spherical body is reasonable for the usage of WISE/NEOWISE alone. The post-q data tend to estimate larger sizes than those of pre-q data due to significant bias suffered from extreme heating at its perihelion passage (MacLennan et al 2022). In such a case, the pre-q data use a stable variation of surface temperature presumed to be plausible for obtaining the statistically best-fitted size D e = 4.8 ± 0.2 km (Table 4 in MacLennan et al 2022).…”

Section: Wise/neowise Datamentioning

confidence: 99%

“…The post-q data tend to estimate larger sizes than those of pre-q data due to significant bias suffered from extreme heating at its perihelion passage (MacLennan et al 2022). In such a case, the pre-q data use a stable variation of surface temperature presumed to be plausible for obtaining the statistically best-fitted size D e = 4.8 ± 0.2 km (Table 4 in MacLennan et al 2022). This is consistent within 1σ of our WISE/NEOWISE-derived size.…”

Section: Wise/neowise Datamentioning

confidence: 99%

“…This produced fragmental kilometersized NEAs: (155140) 2005 UD and (225416) 1999 YC (hereafter 2005 UD and 1999 YC, respectively), named as "Phaethon-Geminid Complex" (PGC; Ohtsuka et al 2006Ohtsuka et al , 2008. The optical color of 2005 UD is blue (B-type), consistent with Phaethon (Jewitt & Hsieh 2006), but the dissimilarity in the concave-shaped near-infrared spectrum makes a direct association debatable (Kareta et al 2021;MacLennan et al 2022). The color of 1999 YC in the visual band distinctly exhibits a neutral (C-type) slope (Kasuga & Jewitt 2008).…”

Section: Introductionmentioning

confidence: 99%

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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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Dual broadband phase curves of asteroid (3200) Phaethon

Betzler,

de Sousa

2024

Astrophys Space Sci

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Evidence of surface heterogeneity on active asteroid (3200) Phaethon

Cited by 9 publications

References 91 publications

Implications for the Formation of (155140) 2005 UD from a New Convex Shape Model

Implications for the Formation of (155140) 2005 UD from a New Convex Shape Model

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

Dual broadband phase curves of asteroid (3200) Phaethon

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