Classical Cepheids in the Galactic outer ring <i>R</i><sub>1</sub><i>R</i> ′<sub>2</sub>

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<jats:title>Abstract</jats:title><jats:p>The kinematics and distribution of classical Cepheids within ∼3 kpc from the Sun suggest the existence of the outer ring <jats:italic>R</jats:italic><jats:sub>1</jats:sub><jats:italic>R</jats:italic> ′<jats:sub>2</jats:sub> in the Galaxy. The optimum value of the solar position angle with respect to the major axis of the bar, <jats:italic>θ</jats:italic><jats:sub>b</jats:sub>, providing the best agreement between the distribution of Cepheids and model particles, is <jats:italic>θ</jats:italic><jats:sub>b</jats:sub> = 37° ±13°. The kinematical features obtained for Cepheids with negative galactocentric radial velocity <jats:italic>V</jats:italic><jats:sub>R</jats:sub> are consistent with the solar location near the descending segment of the outer ring <jats:italic>R</jats:italic><jats:sub>2</jats:sub>. The sharp rise of extinction toward of the Galactic center can be explained by the presence of the outer ring <jats:italic>R</jats:italic><jats:sub>1</jats:sub> near the Sun. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)</jats:p>

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