The orbit of (1011) Laodamia and the mass of Mars.
1959; Institute of Physics; Volume: 64; Linguagem: Inglês
10.1086/108005
ISSN1538-3881
Autores Tópico(s)Planetary Science and Exploration
ResumoThe recently improved orbit of the minor planet (loll) Laodamia (Rabe 1956) reveals a remarkable relationship to the orbit of Mars. The trajectories interlock near to the ascending node of Laodamia on Mars, and to the aphelion of Mars. The orbits approach to 0.04 a.u., yet the approach is so asymptotic that the distance between the two curves is of the order of 0.1 a.u. for orbital arcs of nearly 900, between the approximate heliocentric longitudes of 960 and 1810. The orbits deviate by less than 0.05 a.u. between the longitudes 1580 and 1690. The closeness of actual approaches depends on the difference of the longitudes. In consequence of the near commensurability of the mean motions of Mars and Laodamia in the ratio 1.97: 1, any close approaches occur in series of successive passages. The subsequent approaches of September 1957 and March 1961 amount to 0.10 a.u. each. They are preceded by an approach to 0.36 a.u. in January 1954, and followed by approaches to 0.14 and 0.36 a.u. in September 1964 and June 1968, respectively. If the Mars perturbations of Lao ciamia are integrated from a zero epoch in 1959, between the two closest approaches to 0.10 a.u., then in the backward integration the longitude perturbations exceed -1000" already in 1941 (the discovery opposition is 1924). The perturbations will increase even more rapidly in the forward integration, through the three approaches to 0.10, 0.14 and 0.36 a.u. In perihelion oppositions these perturbations can be observed at geocentric distances of roughly 0.6 a.u. The planet has been observed in 5 oppositions 1924- 57, mostly near perihelion. Observers with powerful instruments are urged especially to observe this relatively faint object as extensively as possible, because undoubtedly the mass of Mars can be determined from the motion of (101 i) Laodamia to a very considerable degree of accuracy. REFERENCE Rabe, E. 1956, Minor Planet Circ. `474. University of Cincinnati Observatory Cincinnati, Ohio
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