Thermal properties of large main-belt asteroids observed by<i>Herschel</i>PACS

Alí-Lagoa, V.; Müller, Thomas; Kiss, Csaba; Szakáts, R.; Márton, G.; Farkas-Takács, Anikó; Bartczak, P.; Butkiewicz-Bąk, M.; Dudziński, G.; Marciniak, A.; Podlewska-Gaca, E.; Duffárd, R.; Santos-Sanz, P.; Ortiz, J. L.

doi:10.1051/0004-6361/202037718

Cited by 17 publications

(15 citation statements)

References 71 publications

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“…Our larger α and steeper β terms with our sample's data compared to the literature-only data set can be accounted for by the lack of large asteroids in our sample, having only one data point with a diameter larger than 100 km. Though many of the literature estimates we fit use several different thermophysical models and thermal data sources, such as observations from the Spitzer Space Telescope (e.g., Lamy et al 2008;Marchis et al 2012) and the Herschel Space Observatory (e.g., O'Rourke et al 2012;Fornasier et al 2013;Alí-Lagoa et al 2020), we see an overall strong consistency with our Γ-D relation compared to the literature as a whole. Because our thermal inertia error bars are so large, however, it is difficult to draw any more definitive conclusions about its relationship with size.…”

Section: Relationship With Sizesupporting

confidence: 68%

“…It is difficult to comment on the average thermal inertia representative of various asteroid subpopulations as existing thermal inertia estimates only number in the few hundreds and cover a wide range in values, from 0 to nearly 1500 J m −2 s −0.5 K −1 (see Table 3). Previous studies have attempted to identify how thermal inertia might correlate with other physical properties such as spectral type, rotation period, and size (e.g., Delbo' et al 2015;Hanuš et al 2018a;Alí-Lagoa et al 2020). Due to the inverse dependency of skin depth with rotation speed, the heat from solar radiation can penetrate the thin topmost regolith layers of slowly rotating asteroids and reach the denser, more highly thermally conductive subsurface material.…”

Section: Introductionmentioning

confidence: 99%

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Thermal Properties of 1847 WISE-observed Asteroids

Hung¹,

Hanuš²,

Masiero³

et al. 2022

Preprint

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We present new thermophysical model (TPM) fits of 1,847 asteroids, deriving thermal inertia, diameter, and Bond and visible geometric albedo. We use thermal flux measurements obtained by the Wide-field Infrared Survey Explorer (WISE;Wright et al. 2010;Mainzer et al. 2011) during its fully cryogenic phase, when both the 12µm (W3) and 22µm (W4) bands were available. We take shape models and spin information from the Database of Asteroid Models from Inversion Techniques (DAMIT; Ďurech et al. 2010) and derive new shape models through lightcurve inversion and combining WISE photometry with existing DAMIT lightcurves. When we limit our sample to the asteroids with the most reliable shape models and thermal flux measurements, we find broadly consistent thermal inertia relations with recent studies. We apply fits to the diameters D (km) and thermal inertia Γ (J m −2 s −0.5 K −1 ) normalized to 1 au with a linear relation of the form log[Γ] = α + β log[D], where we find α = 2.667 ± 0.059 and β = −0.467 ± 0.044 for our sample alone and α = 2.509 ± 0.017 and β = −0.352 ± 0.012 when combined with other literature estimates. We find little evidence of any correlation between rotation period and thermal inertia, owing to the small number of slow rotators to consider in our sample. While the large uncertainties on the majority of our derived thermal inertia only allow us to identify broad trends between thermal inertia and other physical parameters, we can expect a significant increase in high-quality thermal flux measurements and asteroid shape models with upcoming infrared and wide-field surveys, enabling even more thermophysical modeling of higher precision in the future.

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Section: Relationship With Sizesupporting

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Thermal Properties of 1847 WISE-observed Asteroids

Hung¹,

Hanuš²,

Masiero³

et al. 2022

Preprint

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“…It was thus hypothesized that slow rotators (i.e., rotation periods longer than 12 hours) should on average present higher thermal inertia than those of fast rotators. While early studies such as Harris & Drube (2016) and Marciniak et al (2018) appeared to confirm this trend, later studies with larger samples of slow rotators (e.g., Marciniak et al 2019;Alí-Lagoa et al 2020;Marciniak et al 2021) found no such relation.…”

Section: Introductionmentioning

confidence: 95%

Thermal Properties of 1847 WISE-observed Asteroids

Hung¹,

Hanuš²,

Masiero³

et al. 2022

Planet. Sci. J.

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We present new thermophysical model fits of 1847 asteroids, deriving thermal inertia, diameter, and Bond and visible geometric albedo. We use thermal flux measurements obtained by the Wide-field Infrared Survey Explorer (WISE) during its fully cryogenic phase, when both the 12 μm (W3) and 22 μm (W4) bands were available. We take shape models and spin information from the Database of Asteroid Models from Inversion Techniques (DAMIT) and derive new shape models through lightcurve inversion and combining WISE photometry with existing DAMIT lightcurves. When we limit our sample to the asteroids with the most reliable shape models and thermal flux measurements, we find broadly consistent thermal inertia relations with recent studies. We apply fits to the diameters D (km) and thermal inertia Γ (J m−2 s−0.5 K−1) normalized to 1 au with a linear relation of the form log [ Γ ] = α + β log [ D ] , where we find α = 2.667 ± 0.059 and β = −0.467 ± 0.044 for our sample alone and α = 2.509 ± 0.017 and β = −0.352 ± 0.012 when combined with other literature estimates. We find little evidence of any correlation between rotation period and thermal inertia, owing to the small number of slow rotators to consider in our sample. While the large uncertainties on the majority of our derived thermal inertia only allow us to identify broad trends between thermal inertia and other physical parameters, we can expect a significant increase in high-quality thermal flux measurements and asteroid shape models with upcoming infrared and wide-field surveys, enabling even more thermophysical modeling of higher precision in the future.

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“…Numbers in italics mark the pole solution of ( 667 where the α exponent is equal to 0.75, which takes into account a radiative conduction term in thermal conductivity. Different exponents are also possible (Rozitis et al 2018), but here we opted for the most widely used value to facilitate comparison with previous works (see the discussion in Alí-Lagoa et al 2020;Szakáts et al 2020).…”

Section: Resultsmentioning

confidence: 99%

Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Marciniak

Ďurech

Alí-Lagoa

et al. 2021

A&A

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Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to <400 J m−2 s−1∕2 K−1, not showing any correlation with the period. Conclusions. With this work we increase the sample of slow rotators with reliable spin and shape models and known thermal inertia by 40%. The thermal inertia values of our sample do not display a previously suggested increasing trend with rotation period, which mightbe due to their small skin depth.

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Thermal properties of large main-belt asteroids observed byHerschelPACS

Cited by 17 publications

References 71 publications

Thermal Properties of 1847 WISE-observed Asteroids

Thermal Properties of 1847 WISE-observed Asteroids

Thermal Properties of 1847 WISE-observed Asteroids

Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

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