Educação Humanizadora E O Uso Das Tecnologias

Tedesco, Anderson Luiz; Strieder, Roque; Lacerda, Tiago Eurico de

doi:10.22481/folio.v11i2.5519

Cited by 1 publication

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“…The values obtained here for diameter are "scaling values" of the given spin and shape solutions listed in Table 1 that would otherwise be scale-free. For comparison we also refer there to the diameters obtained previously from the AKARI (Usui et al 2011), IRAS (Tedesco et al 2005), and WISE Masiero et al 2011) surveys. We also added their taxonomic class following Bus & Binzel (2002a,b) and Tholen (1989), so that the albedos could be verified for agreement with taxonomy.…”

Section: Resultsmentioning

confidence: 99%

“…For practical reasons, the projections of the shape models and the fit to all the visible lightcurves are not presented here, but will be available from the DAMIT (Database of Astroid Models (Tedesco et al 2005;Usui et al 2011;Mainzer et al 2016), compared to our values from TPM (sixth column). We also provide the corresponding visible geometric albedo (p V ) as described in Sect.…”

Section: Resultsmentioning

confidence: 99%

“…The Bond albedo that would be derived from these values is sometimes different from the Bond albedo value used as input for the TPM (A i ). This value was obtained by first averaging the tabulated diameter from IRAS, AKARI, and WISE (Tedesco et al 2005;Usui et al 2011;Alí-Lagoa et al 2018;Mainzer et al 2016) and occultations (compiled by Dunham et al 2016). Then, we used this size to compute the Bond albedo from all available H-G, H-G 12 , and/or H-G 1 -G 2 values from the Minor Planet Center (Oszkiewicz et al (2011) or Vereš et al (2015), and took again the average value.…”

Section: Lightcurve Inversion and Thermophysical Modellingmentioning

confidence: 99%

“…We compiled archival lightcurves from four apparitions, published by Tedesco (1979), Gil-Hutton (1990), 2 http://astro.troja.mff.cuni.cz/projects/asteroids3D. Hainaut-Rouelle et al (1995), and Galad et al (2009), and complemented them with data from the SuperWASP survey (Wide Angle Search for Planets, Grice et al 2017), and our own data from three more apparitions (see Figs.…”

Section: (100) Hekatementioning

confidence: 99%

“…Lightcurves from two previous apparitions of Lina have been published by Tedesco (1979) and Buchheim (2007). Our visual observations of this target spanned six apparitions, and we found it displaying complex lightcurves, with wide, wavy maxima and narrow minima (Figs.…”

Section: (468) Linamentioning

confidence: 99%

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

Marciniak

Alí-Lagoa

Müller

et al. 2019

A&A

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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.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%