J/A+A/654/A87 Properties of slowly rotating asteroids. (Marciniak+ 2021)
Properties of slowly rotating asteroids from Convex Inversion Thermophysical
Model.
Marciniak A., Durech J., Ali-Lagoa V., Ogloza W., Szakats R., Mueller T.G.,
Molnar L., Pal A., Monteiro F., Arcoverde P., Behrend R., Benkhaldoun Z.,
Bernasconi L., Bosch J., Brincat S., Brunetto L., Butkiewicz-Bak M.,
Del Freo F., Duffard R., Evangelista-Santana M., Farroni G., Fauvaud S.,
Fauvaud M., Ferrais M., Geier S., Golonka J., Grice J., Hirsch R.,
Horbowicz J., Jehin E., Julien P., Kalup Cs., Kaminski K., Kaminska M.K.,
Kankiewicz P., Kecskemethy V., Kim D.-H., Kim M.-J., Konstanciak I.,
Krajewski J., Kudak V., Kulczak P., Kundera T., Lazzaro D., Manzini F.,
Medeiros H., Michimani-Garcia J., Morales N., Nadolny J., Oszkiewicz D.,
Pakstiene E., Pawlowski M., Perig V., Pilcher F., Pinel P.,
Podlewska-Gaca E., Polakis T., Richard F., Rodrigues T., Rondon E., Roy R.,
Sanabria J.J., Santana-Ros T., Skiff B., Skrzypek J., Sobkowiak K.,
Sonbas E., Stachowski G., Strajnic J., Trela P., Tychoniec L., Urakawa S.,
Verebelyi E., Wagrez K., Zejmo M., Zukowski K.
<Astron. Astrophys. 654, A87 (2021)>
=2021A&A...654A..87M 2021A&A...654A..87M (SIMBAD/NED BibCode)
ADC_Keywords: Minor planets ; Photometry
Keywords: minor planets: asteroids: general - techniques: photometric -
radiation mechanisms: thermal
Abstract:
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>12h), 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.
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.
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.
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 145km. The rotation
periods of our targets range from 11 to 59h, and the thermal inertia
covers a wide range of values, from 2 to <400J/m2/s1/2/K,
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.
Description:
The files contain asteroid brightness and geometry for corresponding
epochs. The "*lcs.dat" files were used for obtaining shape models and
spin states of the asteroids using multi-apparition data. Individual
lightcurves within a file are separated by an empty line, all
lightcurves are relative.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 55 16 Ancillary information on the data and
physical properties of our targets
108lcs.dat 112 3029 Asteroid 108 Hecuba individual lightcurves
202lcs.dat 112 3135 Asteroid 202 Chryseis individual lightcurves
219lcs.dat 112 2408 Asteroid 219 Thusnelda individual lightcurves
223lcs.dat 112 2471 Asteroid 223 Rosa individual lightcurves
362lcs.dat 112 1750 Asteroid 362 Havnia individual lightcurves
478lcs.dat 112 1364 Asteroid 478 Tergeste individual lightcurves
483lcs.dat 112 1630 Asteroid 483 Seppina individual lightcurves
501lcs.dat 112 2224 Asteroid 501 Urhixidur individual lightcurves
537lcs.dat 112 1714 Asteroid 537 Pauly individual lightcurves
552lcs.dat 112 2445 Asteroid 552 Sigelinde individual lightcurves
618lcs.dat 112 2739 Asteroid 618 Elfriede individual lightcurves
666lcs.dat 112 1519 Asteroid 666 Desdemona individual lightcurves
667lcs.dat 112 835 Asteroid 667 Denise individual lightcurves
780lcs.dat 112 2567 Asteroid 780 Armenia individual lightcurves
923lcs.dat 112 1095 Asteroid 923 Herluga individual lightcurves
995lcs.dat 112 2828 Asteroid 995 Sternberga individual lightcurves
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See also:
B/astorb : Orbits of Minor Planets (Bowell+ 2014)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Num Asteroid number
5- 14 A10 --- Name Asteroid name
16 I1 --- Napp Number of apparition during which the Nlc of
visible light curves were obtained
18- 20 I3 --- Nlc Number of visible light curves
22- 23 I2 --- NI ? Number of points provided by space
observatories IRAS NI
25- 26 I2 --- NA Number of points provided by space
observatories Akari NA
28- 29 I2 --- NW3 ? Number of points provided by space
observatories WISE in W3 band
31- 32 I2 --- NW4 ? Number of points provided by space
observatorie WISE in W4 bands
34- 40 F7.3 km DWISE Diameter from WISE spacecraft (1)
41 A1 --- n_DWISE [)] Uncertainty flag on DWISE (2)
43- 44 A2 --- Type Taxonomic type (3)
46- 55 A10 --- FileName name of the table with light curve data
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Note (1): Diameters DWISE from WISE spacecraft (Mainzer et al.,
2011ApJ...741...90M 2011ApJ...741...90M; Masiero et al. 2011ApJ...741...68M 2011ApJ...741...68M, Cat. J/ApJ/741/68).
Note (2): ")" for a lack of size determination from WISE, comes from IRAS survey
results (Tedesco et al. 2004, NASA Planetary Data System, IRAS).
Note (3): taxonomic types (Bus & Binzel, 2002Icar..158..146B 2002Icar..158..146B,
2002Icar..158..106B 2002Icar..158..106B, and Tholen 1989, in Asteroids II, eds. R.P. Binzel,
T. Gehrels, & M. S. Matthews (Tucson: University of Arizona Press), 1139).
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Byte-by-byte Description of file: *lcs.dat
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Bytes Format Units Label Explanations
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2- 15 F14.6 d JD JD epoch corrected for the light-time
corresponding to the Earth-asteroid distance
17- 28 E12.6 --- br Relative brightness in intensity units,
mean brightness of each lightcurve is unity
30- 42 E13.6 AU Sx x component of the vector from the asteroid to
the Sun in J2000 ecliptic Cartesian coordinates
44- 56 E13.6 AU Sy y component of the vector from the asteroid to
the Sun in J2000 ecliptic Cartesian coordinates
58- 70 E13.6 AU Sz z component of the vector from the asteroid to
the Sun in J2000 ecliptic Cartesian coordinates
72- 84 E13.6 AU Ex x component of the vector from the asteroid to
the Earth in J2000 ecliptic Cartesian coordinates
86- 98 E13.6 AU Ey y component of the vector from the asteroid to
the Earth in J2000 ecliptic Cartesian coordinates
100-112 E13.6 AU Ez z component of the vector from the asteroid to
the Earth in J2000 ecliptic Cartesian coordinates
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Acknowledgements:
Anna Marciniak, am(at)amu.edu.pl
(End) Patricia Vannier [CDS] 30-Jun-2021