Resonant Trapping of the Moving Groups G18-39 and G21-22 in the Galactic Halo. (arXiv:1811.09827v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Schuster_W/0/1/0/all/0/1">W. J. Schuster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Trincado_J/0/1/0/all/0/1">J. G. Fernández-Trincado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moreno_E/0/1/0/all/0/1">E. Moreno</a>
The 3D Galactic orbits of stars in the two groups G18-39 and G21-22
pertaining to the Galactic halo have been computed in a Galactic potential
including a Galactic bar. The orbits have been related with the orbital
structure of resonant orbits on the Galactic plane created by the bar
component. We find that the majority of stars in both groups are trapped mainly
by two resonant families already studied in a previous analysis. We show that
the observed U–V velocity field of the stars in both groups can be naturally
explained as a result of their trapping by these two resonant families, taking
the angular rotation speed of the bar approximately in the interval 45–60
$mathrm{km,s^{-1},kpc^{-1}}$. This analysis may help to understand the
identification of other known star groups as the possible result of the
interactions produced by resonances on stars close to resonant families. For
the two groups G18-39 and G21-22 we conclude that the majority of their stars
are members of the supergroups of stars in the Galaxy trapped by two resonant
families generated by the Galactic bar.
The 3D Galactic orbits of stars in the two groups G18-39 and G21-22
pertaining to the Galactic halo have been computed in a Galactic potential
including a Galactic bar. The orbits have been related with the orbital
structure of resonant orbits on the Galactic plane created by the bar
component. We find that the majority of stars in both groups are trapped mainly
by two resonant families already studied in a previous analysis. We show that
the observed U–V velocity field of the stars in both groups can be naturally
explained as a result of their trapping by these two resonant families, taking
the angular rotation speed of the bar approximately in the interval 45–60
$mathrm{km,s^{-1},kpc^{-1}}$. This analysis may help to understand the
identification of other known star groups as the possible result of the
interactions produced by resonances on stars close to resonant families. For
the two groups G18-39 and G21-22 we conclude that the majority of their stars
are members of the supergroups of stars in the Galaxy trapped by two resonant
families generated by the Galactic bar.
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