VizieR Online Data Catalog: 100 asteroids rotational parameters (Lhotka+, 2013)
Abstract
We provide our target list in which one data point entry consists of four lines in table1.ori. Each line starts with the IAU designation number of the asteroid:
1:id., name, 2:id., m[1],[4], R[4] [km], a/b[1], b/c[1], no., c[2] [km], a/b[2], b/c[2], 3:id., Trot[2],[4] [h], λ[2], β[2], {epsilon}[2],[3], no., λ[1], β[1],{epsilon}[1],[3], 4:id., Trev[4] [y], T0[3], a[3] [AU], e[3], i[3], ω[3], Ω[3], M[3], n[3] [°/d]. In line1 id. stands for the designation number, and name is the official IAU name of the object, as published in [3]. In line2: m, taken from [1] or [4], is the mass of the object given in the mass unit of Ceres; the equatorial radius R is given in [km]; the first two ratios, a/b and b/c, are the ratios of the semi axes published in [1]; no. defines the number of shape models that exist for one asteroid in [2] from which a,b,c and the respective ratios are calculated (see below). In line3, Trot is the rotation period (in hours) of the asteroid as published in [2]. The first three parameters (λ,β,{epsilon}) denote the ecliptic longitude λ and latitude β as they are published in [2]; the resulting obliquity {epsilon} has been calculated on the basis of the orbital parameters (line 4). The integer no. gives the number of spin-vector solutions, which are published for one object in [1] (the number of triplets of the form (λ,β,{epsilon}) that could be calculated using the different (λ,β) that are published in [1] on the basis of the orbital parameters given in line4). The first entry in line4 is the orbital period in [y] published in [4], T0 defines the epoch for which the elements are given; a is the semi-major axis in [AU]; e is the eccentricity, i is the inclination, ω is the argument of perihelium; Ω is the longitude of the ascending node; M is the mean anomaly at T0, and n is the mean motion in [°] and [°/d]. We note that all values are taken as they are published in [1]-[4] with the exception of the second set of shape parameters a/b,b/c, and c in line2, which were calculated from shape models published in [2] and the obliquities of the asteroids {epsilon} in line3. The obliquities are obtained by combining the spin-vector solutions, which are published in [1] or [2] with the orbital parameters (published for the object in [3] and [4]) according to a method fully described in Sect. 5. (3 data files).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- July 2013
- DOI:
- 10.26093/cds/vizier.35560008
- Bibcode:
- 2013yCat..35560008L
- Keywords:
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- Minor planets