Shapes and rotational properties of thirty asteroids from photometric data

Torppa, Johanna; Kaasalainen, M.; Michałowski, Tadeusz; Kwiatkowski, T.; Kryszczyńska, A.; Denchev, P.; Kowalski, R. A.

doi:10.1016/s0019-1035(03)00146-5

Cited by 124 publications

(144 citation statements)

References 17 publications

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“…Note that even large asteroids typically have strong local irregularities even if their global shapes were "pseudoellipsoidal" (Kaasalainen et al 2002b;Torppa et al 2003). Simulations with such shapes produce results similar to those above.…”

Section: Photocentres Of Irregular Bodiessupporting

confidence: 66%

Photocentre offset in ultraprecise astrometry: Implications for barycentre determination and asteroid modelling

Kaasalainen

Tanga

2004

A&A

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Section: Photocentres Of Irregular Bodiessupporting

confidence: 66%

Photocentre offset in ultraprecise astrometry: Implications for barycentre determination and asteroid modelling

Kaasalainen

Tanga

2004

A&A

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“…Using the inversion method for 32 lightcurves from 1962−1998 time interval, Torppa et al (2003) constructed a shape model of Lutetia with some sharp and irregular features and rough global dimensions of a/b = 1.2 and b/c = 1.2 (where a, b, and c are the semi-major axis of the ellipsoid figure, the closest to the shape model). The J2000.0 ecliptic coordinates of the adopted pole solutions for physical model are…”

Section: Photometrymentioning

confidence: 99%

“…The rotational period inferred from the 36-year baseline was derived to be P = 8.165455 h (Torppa et al 2003).…”

Section: Photometrymentioning

confidence: 99%

“…Following Torppa et al (2003)'s pole solution, (21) Lutetia was in a near equatorial aspect during the 2006 opposition. Thus our expectation was to observe a lightcurve with a relatively large amplitude.…”

Section: Photometrymentioning

confidence: 99%

“…The second order largest contribution in the error arises from the estimation of the ellipsoid flatness from the asteroid shape model axis ratio (Torppa et al 2003) and affects mainly the sub-Earth latitudes. However, we note that these two types of errors do not change the relative positions of the sub-Earth points for different instances.…”

Section: Photometrymentioning

confidence: 99%

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Near infra-red spectroscopy of the asteroid 21 Lutetia

Nedelcu

Birlan²,

Vernazza³

et al. 2007

A&A

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Aims. In the framework of the ground-based science campaign dedicated to the encounter with the Rosetta spacecraft, the mineralogy of the asteroid (21) Lutetia was investigated. Methods. Near-infrared (NIR) spectra of the asteroid in the 0.8−2.5 µm spectral range were obtained with SpeX/IRTF in remote observing mode from Meudon, France in March and April 2006. We analysed these data together with previously acquired spectra -March 2003, August 2004. I-band relative photometric data obtained on 20 January 2006 using the 105 cm telescope from Pic du Midi, France has been used to build the ephemeris for physical observations. A χ 2 test using meteorite spectra from the RELAB database was performed in order to find the best fit of complete visible + infrared (VNIR) spectra of Lutetia. Results. The new spectra reveal no absorption features. We find a clear spectral variation (slope), and a good correspondence between spectral variations and rotational phase. Two of the most different spectra correspond to two opposite sides of the asteroid (sub-Earth longitude difference around 180 • ). For the neutral spectra a carbonaceous chondrite spectrum yields the best fit, while for those with a slightly positive slope the enstatitic chondrite spectra are the best analog. Based on the chosen subset of the meteorite samples, our analysis suggests a primitive, chondritic nature for (21) Lutetia. Differences in spectra are interpreted in terms of the coexistence of several lithologies on the surface where the aqueous alteration played an important role.

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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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Shapes and rotational properties of thirty asteroids from photometric data

Cited by 124 publications

References 17 publications

Photocentre offset in ultraprecise astrometry: Implications for barycentre determination and asteroid modelling

Photocentre offset in ultraprecise astrometry: Implications for barycentre determination and asteroid modelling

Near infra-red spectroscopy of the asteroid 21 Lutetia

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

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