Rotational periods of asteroids II

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

doi:10.1016/s0032-0633(01)00014-9

Cited by 10 publications

(7 citation statements)

References 31 publications

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“…Additional observations were performed by two of the present authors (Riccioli et al, 2001) who obtained a synodic period of 5.560 ± 0.018 h, i.e. about two hundredth shorter than the one previously published by Di and Piironen et al (1994).…”

Section: Gretiasupporting

confidence: 48%

“…The results reported in this paper are part of the large photometric observational programme of asteroids undertaken since 1979 at the Physics and Astronomy Department of Catania University (Blanco & Catalano, 1979;Di Martino et al, 1994;Blanco & Riccioli, 1998;Riccioli et al, 2001). The aim of this long-term programme is to increase the number of asteroids with well-known rotational parameters and consequently improve the database necessary for the investigation of the minor planet evolutionary history.…”

Section: Introductionmentioning

confidence: 99%

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CCD and photon-counting photometric observations of asteroids carried out at Padova and Catania observatories

Cigna

Fulvio

Blanco

2009

Planetary and Space Science

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Section: Gretiasupporting

confidence: 48%

Section: Introductionmentioning

confidence: 99%

CCD and photon-counting photometric observations of asteroids carried out at Padova and Catania observatories

Cigna

Fulvio

Blanco

2009

Planetary and Space Science

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“…This low-albedo asteroid is classified as G-type (DeMeo et al, 2009;DeMeo and Carry, 2013). The rotational period was determined by Hansen and Arentoft (1997) and Riccioli et al (2001). The detailed magnitude-phase relation including low phase angles was not previously obtained.…”

Section: (176) Idunamentioning

confidence: 99%

Asteroid observations at low phase angles. IV. Average parameters for the new H , G 1 , G 2 magnitude system

Shevchenko

Belskaya

Muinonen

et al. 2016

Planetary and Space Science

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a b s t r a c tWe present new observational data for selected main-belt asteroids of different compositional types. The detailed magnitude-phase dependences including small phase angles ( o1°) were obtained for these asteroids, namely: (10) Hygiea (down to the phase angle of 0.Flammario (0.6°, B-type), and (1279) Uganda (0.5°, E-type). For several asteroids, the dependences of brightness on the phase angle were investigated in the BVRI bands. We found a great diversity in the opposition-effect behavior both in the magnitude and the width of the opposition surges, especially for low-albedo asteroids. Some low-albedo asteroids (e.g., (10) Hygiea) display a broad opposition effect with an amplitude of 0.15-0.20 mag relative to the extrapolation of the linear part of the phase curve. Other asteroids (e.g., (596) Scheila, (1021) Flammario) show linear magnitude-phase dependences down to small phase angles (0.1-0.2°). Using numerous data sets on the magnitude-phase dependences with extensive phase-angle coverage, we examined in more detail the new threeparameter H, G 1 , G 2 magnitude system. We determined the values of the G 1 and G 2 parameters for magnitude phase dependences of individual asteroids and obtained the average parameters for main asteroid compositional types. The values obtained can be used for the estimation of the absolute magnitude of an asteroid from a single observed magnitude when the magnitude-phase dependency is unknown and/or to calculate a visible magnitude for the ephemerides.

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“…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.…”

Section: Resultsmentioning

confidence: 99%

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

Wang

Fan

et al. 2018

Astron Nachr

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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.

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Rotational periods of asteroids II

Cited by 10 publications

References 31 publications

CCD and photon-counting photometric observations of asteroids carried out at Padova and Catania observatories

CCD and photon-counting photometric observations of asteroids carried out at Padova and Catania observatories

Asteroid observations at low phase angles. IV. Average parameters for the new H , G 1 , G 2 magnitude system

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

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