http://arxiv.org/abs/2012.15289
We used Gaia DR2 data in order to estimate parameters of the Pleiades. With the data on stars with m_G<=18 mag, we constructed the density maps and profile, luminosity and mass functions, determined the cluster radius, 10.9+/-0.3 deg (26.3+/-0.7 pc), and the radius of its core, 2.62 deg (6.24 pc), and obtained estimates for the number of stars in the cluster, 1542+/-121, and their mass, 855+/-104 solar mass. Distribution of stars with m_G<16 mag at distances r_s from the cluster center in three-dimensional space of r_s<1 pc and at r_s~1.4-5 pc contains radial density waves. We determined the average
prograde' rotation velocity of the core of the cluster v_c=0.56+/-0.07 km/s at distances d in the sky plane d<=4.6 pc from its center. The rotation velocity of the cluster core at a distance of d~5.5 pc from its center is close to zero: v_c=0.1+/-0.3 km/s. The velocity of theretrograde’ rotation of the cluster at a distance of d~7.1 pc from its center is v_c=0.48+/-0.20 km/s. The dependences of moduli of the tangential and radial components of the cluster core star velocities in the sky plane on the distance d to the cluster center contain the periodic oscillations. The velocity dispersions of the cluster core stars increase on average with an increase in r_s, which, like the radial density waves and the waves of oscillations of the velocity field in the sky plane, indicates the non-stationarity of the cluster in the regular field. The Jeans wavelength in the cluster core decreases, and the velocity dispersion of the core stars under the Jeans instability increases after taking into account the Galactic gravitational field. The region of gravitational instability in the Pleiades cluster is located in the interval r_s=2.2-5.7 pc and contains 39.4-60.5% of the total number of stars in the considered samples.
V. Danilov and A. Seleznev
Fri, 1 Jan 21
63/103
Comments: 18 pages, 10 figures, 1 table
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