Reference : UBV photometry of the minor planets 86 Semele, 521 Brixia, 53 Kalypso and 113 Amalthea
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/22122
UBV photometry of the minor planets 86 Semele, 521 Brixia, 53 Kalypso and 113 Amalthea
English
Surdej, Jean mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Surdej, Anna [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Louis, B. [> > > >]
1-May-1983
Astronomy and Astrophysics. Supplement Series
EDP Sciences
52
203-211
Yes (verified by ORBi)
International
0365-0138
Les Ulis
France
[en] ASTEROIDS ; ASTEROIDS ; ASTRONOMICAL PHOTOMETRY ; LIGHT CURVE ; PLANETARY ROTATION ; UBV SPECTRA ; ELECTROPHOTOMETRY ; PHOTOMETRY ; ULTRAVIOLET ; WAVELENGTHS ; 86 SEMELE ; 521 BRIXIA ; 53 KALYPSO ; 113 AMALTHEA ; LIGHTCURVE ; AMPLITUDE ; ROTATION ; PERIODS ; COLOR ; COMPARISONS ; ASTRONOMY
[en] The asteroids were observed photometrically during the 1980 and 1981 oppositions, respectively. The V lightcurve of 86 Semele displays two asymmetric maxima and minima with a total amplitude DeltaV = 0.18 mag. Its synodic rotation period is P[SUB]s[/SUB] = 16h38m02" ± 16" and the color indices B-V = 0.690 ± 0.011 and U-B = 0.320 ± 0.015 mag. 521 Brixia is a slow rotator (P[SUB]s[/SUB] > 24h) showing light variations greater than DeltaV â 0.09 mag and with color indices B-V = 0.714 ± 0.008 and U-B = 0.337 ± 0.011 mag. 53 Kalypso rotates with a period P[SUB]s[/SUB] = 26h33m ± 4m with a total light amplitude DeltaV > 0.10 mag and color indices B-V = 0.692 ± 0.015 and U-B = 0.341 ± 0.022 mag. The lightcurve of 113 Amalthea shows large amplitude variations (DeltaV > 0.26 mag) with a broad minimum and the rotation period is greater than 12h with color indices B-V = 0.888 ± 0.012 and U-B = 0.487 ± 0.019 mag.
Researchers ; Professionals
http://hdl.handle.net/2268/22122
http://esoads.eso.org/abs/1983A%26AS...52..203S
The authors thank SAO/NASA ADS Astronomy Abstract Service and EDP Sciences for their deposit authorization.

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