Pole and shape determinaton of asteroids. II

Blanco, C.; Cigna, M.; Riccioli, D.

doi:10.1016/s0032-0633(00)00065-9

Cited by 8 publications

(8 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In Table 4 we cite their spin axis coordinates and sidereal periods, if available, together with their reference. Comparison with our results in Table 2 shows a general agreement, with the exception of (108) Hecuba modelled by Blanco & Riccioli (1998), (362) Havnia modelled by Wang et al (2015), and (537) Pauly modelled by Blanco et al (2000) based on different shape approximations. Parameters strongly differing from the solutions obtained in this work are marked in italics in Table 4.…”

Section: Resultssupporting

confidence: 83%

Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Marciniak

Ďurech

Alí-Lagoa

et al. 2021

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Resultssupporting

confidence: 83%

Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Marciniak

Ďurech

Alí-Lagoa

et al. 2021

A&A

View full text Add to dashboard Cite

show abstract

“…Its rotation period, 12.027 hours, commensurate with an Earth day, required observations from sites well spaced in longitude for full coverage. Thanks to such an extensive dataset both spin and shape solutions are well constrained (Table 1), however different from those found by Blanco et al (2000), who reported four pole solutions, all much lower in |β| than ours, and a sidereal period longer by 0.027 hours, which is a substantial difference.…”

Section: (335) Robertacontrasting

confidence: 94%

Thermal properties of slowly rotating asteroids: results from a targeted survey

Marciniak

Alí-Lagoa

Müller

et al. 2019

A&A

View full text Add to dashboard Cite

Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the sub-surface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 hours, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3 +33 −3 and 45 +60 −30 J m −2 s −1/2 K −1 . Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.

show abstract

“…Asteroid (176) Iduna's rotation period had been analyzed widely in many studies (Alton ; Hansen & Arentoft ; Krajewski ; Oey et al ; Riccioli et al ). Iduna's orientation of pole ( λ p = 85° ± 1°, β p = 36° ± 1°) was determined first by Blanco et al (), based on the Amplitude‐Magnitude (AM) method. Combining the sparse photometric data derived from the Lowell database, Ďurech et al () obtained its orientation of pole ( λ p = 83° ± 5°, β p = 24° ± 5°) or ( λ p = 219° ± 5°, β p = 68° ± 5°) with a rotation period P = 11.28784 hr.…”

Section: Resultsmentioning

confidence: 99%

“…Iduna's orientation of pole ( p = 85 • ± 1 • , p = 36 • ± 1 • ) was determined first by Blanco et al (2000), based on the Amplitude-Magnitude (AM) method. Combining the sparse photometric data derived from the Lowell database,Ďurech et al (2016) obtained its orientation of pole ( p = 83 • ± 5 • , p = 24 • ± 5 • ) or ( p = 219 • ± 5 • , p = 68 • ± 5 • ) with a rotation period P = 11.28784 hr.…”

Section: (176) Idunamentioning

confidence: 99%

Study on the spin states of asteroids using a simplistic shape model

Wang

Fan

et al. 2018

Astron Nachr

View full text Add to dashboard Cite

Photometric observation is one of the most important means to understand the fundamental properties of asteroids. As more and more photometric data are obtained, expanding effectively the number of samples on the spin states of asteroids has become an important research topic. To obtain a preliminary solution of the spin state without statistical discrepancy by the photometric observations derived from a handful of apparitions, a moderate‐complexity shape model consisting of eight adjacent octants with different semiaxes, namely cellinoid ellipsoid, can be adopted. Using this model and employing a Markov chain Monte Carlo (MCMC) method, the spin states of four asteroids are discussed based on the existing photometric data.

show abstract

Pole and shape determinaton of asteroids. II

Cited by 8 publications

References 29 publications

Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

Thermal properties of slowly rotating asteroids: results from a targeted survey

Study on the spin states of asteroids using a simplistic shape model

Contact Info

Product

Resources

About