Spin vectors of 22 large asteroids

Magnusson, P.

doi:10.1016/0019-1035(90)90113-n

Cited by 31 publications

(17 citation statements)

References 18 publications

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“…Only eight objects (2,Pallas,7 Iris,8 Flora,16 Psyche,22 Kalliope,28 Bellona,433 Eros,and 704 Interamnia) are found in the range 80 • < ε < 100 • . This conforms the remark made by Michalowski (1993) and also agrees with Magnusson (1986Magnusson ( , 1990 who analyzes the spin vectors of 20 to 30 asteroids respectively. When quoting the apparent lack of poles with axes close to the ecliptic, this last author attributed this deficiency to an observational selection effect: an asteroid with a pole at a low ecliptic latitude is naturally less suitable to present a significant amplitude of the lightcurve variation.…”

Section: Results and Statisticssupporting

confidence: 92%

“…Thanks to our relatively large sample of 100 asteroids, we were able to analyze the asteroid data and to derive some statistical properties of the rotational characteristics. Concerning the distribution of obliquities, main features are revealed, which agree with previous authors (Drummond et al (1988(Drummond et al ( , 1991; Magnusson (1986Magnusson ( , 1990; Michalowski (1993); Pravec et al (2002)). However, the results in these studies are affected, because they aproximated the orbital plane by the ecliptic for the calculation of the obliquity, while we used the true orbital plane that enabled us to calculate the more accurate value of the obliquity.…”

Section: Resultssupporting

confidence: 91%

“…Drummond et al (1988Drummond et al ( , 1991 confirmed the bimodality of the observed pole distribution using results for 26 asteroids. If they used the same explanation as Magnusson (1986Magnusson ( , 1990 for this distribution, they did not exclude the possibility that the bimodality may be real and may reflect a primordial distribution of spin rates. Another confirmation of the non-uniform distribution of spin axes comes from Pravec et al (2002), who use a larger sample of asteroid-pole estimates than the authors above.…”

Section: Results and Statisticsmentioning

confidence: 99%

See 2 more Smart Citations

Obliquity, precession rate, and nutation coefficients for a set of 100 asteroids

Lhotka¹,

Souchay²,

Shahsavari³

2013

A&A

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Context. Thanks to various space missions and the progress of ground-based observational techniques, the knowledge of asteroids has considerably increased in the recent years. Aims. Due to this increasing database that accompanies this evolution, we compute for a set of 100 asteroids their rotational parameters: the moments of inertia along the principal axes of the object, the obliquity of the axis of rotation with respect to the orbital plane, the precession rates, and the nutation coefficients. Methods. We select 100 asteroids for which the parameters for the study are well-known from observations or space missions. For each asteroid, we determine the moments of inertia, assuming an ellipsoidal shape. We calculate their obliquity from their orbit (instead of the ecliptic) and the orientation of the spin-pole. Finally, we calculate the precession rates and the largest nutation components. The number of asteroids concerned leads to some statistical studies of the output. Results. We provide a table of rotational parameters for our set of asteroids. The table includes the obliquity, their axes ratio, their dynamical ellipticity H d , and the scaling factor K. We compute the precession rateψ and the leading nutation coefficients Δψ and Δε. We observe similar characteristics, as observed by previous authors that is, a significantly larger number of asteroids rotates in the prograde mode (≈60%) than in the retrograde one with a bimodal distribution. In particular, there is a deficiency of objects with a polar axis close to the orbit. The precession rates have a mean absolute value of 18 /y, and the leading nutation coefficients have an average absolute amplitude of 5.7 for Δψ and 5.2 for Δε. At last, we identify and characterize some cases with large precession rates, as seen in 25143 Itokawa, with has a precession rate of about −475 /y.

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Section: Results and Statisticssupporting

confidence: 92%

Section: Resultssupporting

confidence: 91%

Section: Results and Statisticsmentioning

confidence: 99%

See 1 more Smart Citation

Obliquity, precession rate, and nutation coefficients for a set of 100 asteroids

Lhotka¹,

Souchay²,

Shahsavari³

2013

A&A

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show abstract

“…Using all available data for this asteroid from four oppositions we were able to put constraints on its spin state using the method described by Magnusson (1990). Two possible pole solutions were found: λ 1 = 97…”

Section: Phaethonmentioning

confidence: 99%

The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

Krugly

Belskaya²,

Shevchenko³

et al. 2002

Icarus

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“…This spin-orbit coupling might have played a role in the regular or chaotic evolution of the asteroids' spin properties. The present spin vector distribution (SVD) is known for a substantial number of the larger main belt asteroids (e.g., Magnusson et al 1989;Magnusson 1990;Michal owski1993;De Angelis 1995;Erikson 1999Erikson , 2000. In the most recent of these studies (Erikson 1999(Erikson , 2000, based on well-determined spin vectors for 73 main belt asteroids, it was possible to derive some general characteristics of the SVD (see Fig.…”

Section: Introductionmentioning

confidence: 99%

The Influence of the Orbital Evolution of Main Belt Asteroids on Their Spin Vectors

Skoglöv¹

2002

Icarus

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Spin vectors of 22 large asteroids

Cited by 31 publications

References 18 publications

Obliquity, precession rate, and nutation coefficients for a set of 100 asteroids

Obliquity, precession rate, and nutation coefficients for a set of 100 asteroids

The Near-Earth Objects Follow-up Program IV. CCD Photometry in 1996–1999

The Influence of the Orbital Evolution of Main Belt Asteroids on Their Spin Vectors

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