Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model
Abstract
Results from the TESS mission showed that previous studies strngly underestimated the number of slow rotators, revealing the importance of studying those asteroids. For most slowly rotating asteroids (P > 12), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. The goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS. In addition to data in the visible range, we also use thermal data from infrared space observatories (IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model (CITPM). This novel method has so far been applied to only a few targets, and in this work we further validate the method. We present the models of 16 slow rotators. All provide good fits to both thermal and visible data. The obtained sizes are on average accurate at the 5% precision, with diameters in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 hours, and the thermal inertia covers a wide range of values, from 2 to <400 SI units, not showing any correlation with the period. 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 might be due to their small skin depth.
Keywords
Cite
@article{arxiv.2109.00463,
title = {Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model},
author = {A. Marciniak and J. Ďurech and V. Alí-Lagoa and W. Ogłoza and R. Szakáts and T. G. Müller and L. Molnár and A. Pál and F. Monteiro and P. Arcoverde and R. Behrend and Z. Benkhaldoun and L. Bernasconi and J. Bosch and S. Brincat and L. Brunetto and M. Butkiewicz - Bąk and F. Del Freo and R. Duffard and M. Evangelista-Santana and G. Farroni and S. Fauvaud and M. Fauvaud and M. Ferrais and S. Geier and J. Golonka and J. Grice and R. Hirsch and J. Horbowicz and E. Jehin and P. Julien and Cs. Kalup and K. Kamiński and M. K. Kamińska and P. Kankiewicz and V. Kecskeméthy and D. -H. Kim and M. -J. Kim and I. Konstanciak and J. Krajewski and V. Kudak and P. Kulczak and T. Kundera and D. Lazzaro and F. Manzini and H. Medeiros and J. Michimani-Garcia and N. Morales and J. Nadolny and D. Oszkiewicz and E. Pakštienė and M. Pawłowski and V. Perig and F. Pilcher and P. Pinel and E. Podlewska-Gaca and T. Polakis and F. Richard and T. Rodrigues and E. Rondon and R. Roy and J. J. Sanabria and T. Santana-Ros and B. Skiff and J. Skrzypek and K. Sobkowiak and E. Sonbas and G. Stachowski and J. Strajnic and P. Trela and Ł. Tychoniec and S. Urakawa and E. Verebelyi and K. Wagrez and M. Żejmo and K. Żukowski},
journal= {arXiv preprint arXiv:2109.00463},
year = {2021}
}
Comments
Accepted to Astronomy & Astrophysics. 10 pages + appendices