Other
Scientific paper
Aug 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002acasn..43..302w&link_type=abstract
Acta Astronomica Sinica, vol.43, no.3, p. 299-326
Other
1
Globular Clusters, Space Distribution, Motional Orbits
Scientific paper
The 29 F globular clusters in the galaxy are selected as samples. According to the basic data, radial velocities and proper motions of sample clusters, the initial positions and velocities of the samples are reduced using the galactic coordinates, and their orbits are integrated by numerical method for three different Galactic gravitational potential models. The calculating results show: (1) most of samples are located in 5 kpc---10 kpc from Galactic center. All of the sample clusters present a spherical symmetrical distribution around the Galactic center, and their space velocities are presented a ellipsoidal distribution; (2) According to the metallicity and basic characters, the sample clusters are separated into HB subgroup and MP subgroup. The number of samples are changed with metallicity [Fe/H], and there is a peak at [Fe/H] =-1.6; (3) The orbits of sample clusters show mostly limited, periodic characteristics, but the orbits are not closed completely, their maximal galactocentric distance is less than 40 kpc. The differences in orbital morphologies due to different potentials is slighting, however, given a certain potential, for clusters that have perigalactic distance smaller than 1 kpc, some orbits may exhibit a chaotic behavior. The correlation between the metallicity of samples and the orbital morphologies is unclearly; (4) It is found that the semi-major axis, apogalactic distance and azimuth period of 29 example clusters are changed with their metallicity similarly, but a obvious correlation is seen between orbital eccentricity and metallicity. There is a fraction of 24% of the sample clusters with eccentricities lower than 0.4. The different Galactic gravitational potential have not clear influence upon the perigalactic distance, eccentricity and uncertainty of orbital parameters, but which is significant for other parameters, such as the apogalactic distance, semi-major axis, radial period and azimuth period and so on.
Wang Lanjuan
Zhou Hong-Nan
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