Colour variations of asteroid 243 Ida

Mottola, S.; Gonano-Beurer, M.; Green, S.F.; McBride, Neil; Brinjes, J.C.; Martino, M. Di

doi:10.1016/0032-0633(94)90137-6

Cited by 9 publications

(5 citation statements)

References 7 publications

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“…The measurements were made in the V band of the standard JohnsonCousins photometric system. The photometric reduction of the CCD frames was performed by using the ASTPHOT package developed at DLR by S. Mottola (Mottola et al, 1994(Mottola et al, , 1995. The absolute calibration was done using standard stars with colors close to the solar ones from Landolt (1983Landolt ( , 1992 and Lasker et al (1988).…”

Section: Observations and Resultsmentioning

confidence: 99%

Opposition polarimetry and photometry of S- and E-type asteroids

Belskaya¹,

Shevchenko²,

Kiselev³

et al. 2003

Icarus

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Section: Observations and Resultsmentioning

confidence: 99%

Opposition polarimetry and photometry of S- and E-type asteroids

Belskaya¹,

Shevchenko²,

Kiselev³

et al. 2003

Icarus

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“…The flat-field images were obtained during evening or morning twilight. Aperture photometry of Makemake was performed using the astphot package developed at DLR (German Aerospace Center) by S. Mottola (Mottola et al 1994). We used from three to five comparison stars in the object's field, which were inspected for possible variability.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Long-term photometric monitoring of the dwarf planet (136472) Makemake

Hromakina

Belskaya

Krugly

et al. 2019

A&A

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Aims. We studied the rotational properties of the dwarf planet Makemake. Methods. The photometric observations were carried out at different telescopes between 2006 and 2017. Most of the measurements were acquired in BVRI broad-band filters of a standard Johnson-Cousins photometric system. Results. We found that Makemake rotates more slowly than was previously reported. A possible lightcurve asymmetry suggests a double-peaked period of P = 22.8266±0.0001 h. A small peak-to-peak lightcurve amplitude in R-filter A = 0.032±0.005 mag implies an almost spherical shape or near pole-on orientation. We also measured BVRI colours and the R-filter phase-angle slope and revised the absolute magnitudes. The absolute magnitude of Makemake has remained unchanged since its discovery in 2005. No direct evidence of a newly discovered satellite was found in our photometric data; however, we discuss the possible existence of another larger satellite.

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“…In Simeiz, we used a SBIG ST-6 camera placed on the 1-m Ritchey-Chretien telescope equipped with a focal reducer ( f /5 system). The photometric reduction of the CCD frames was performed using the ASTPHOT package developed at DLR by Mottola (Mottola et al 1994). The absolute calibration was performed using standard stars of colors close to those of the Sun taken from Landolt (1983Landolt ( , 1992 and Lasker et al (1988).…”

Section: Photometrymentioning

confidence: 99%

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Belskaya

Fornasier

Krugly

et al. 2010

A&A

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Aims. A wide observational campaign was carried out in [2004][2005][2006][2007][2008][2009] that aimed to complete the ground-based investigation of Lutetia prior to the Rosetta fly-by in July 2010. Methods. We obtained BVRI photometric and V-band polarimetric measurements over a wide range of phase angles, and visible and infrared spectra in the 0.4-2.4 μm range. We analyze them with previously published data to retrieve information about Lutetia's surface properties.Results. Values of lightcurve amplitudes, absolute magnitude, opposition effect, phase coefficient, and BVRI colors of Lutetia surface seen at near pole-on aspect are determined. We define more precisely parameters of polarization phase curve and show their distinct deviation from any other moderate-albedo asteroid. An indication of possible variations in both polarization and spectral data across the asteroid surface are found. To explain features found by different techniques, we propose that (i) Lutetia has a non-convex shape, probably due to a large crater, and heterogeneous surface properties probably related to surface morphology; (ii) at least part of the surface is covered by a fine-grained regolith of particle size smaller than 20 μm; (iii) the closest meteorite analogues of Lutetia's surface composition are particular types of carbonaceous chondrites, or Lutetia has specific surface composition that is not representative among studied meteorites.

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Colour variations of asteroid 243 Ida

Cited by 9 publications

References 7 publications

Opposition polarimetry and photometry of S- and E-type asteroids

Opposition polarimetry and photometry of S- and E-type asteroids

Long-term photometric monitoring of the dwarf planet (136472) Makemake

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

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