The radial-velocity field in the southern part of the supershell around the Cyg OB1 association: the interstellar medium in the vicinity of the stars WR 141 and WR 142статья

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[1] Lozinskaya T. A., Pravdikova V. V., Sitnik T. G. The radial-velocity field in the southern part of the supershell around the cyg ob1 association: the interstellar medium in the vicinity of the stars wr 141 and wr 142 // Astronomy Reports. — 1994. — Vol. 38, no. 4. — P. 453–461. Interferometric observations of the emission nebulas near the stars WR 141 and WR 142, lying in the southern part of the supershell surrounding the Cyg OB1 association, have been conducted in the H(alpha) line. The radial-velocity field of a sky area about 1 degree2 in size was investigated using a folding optical system, which comprised a Fabry-Perot interferometer and an image intensifier, attached to the 125-cm and 60-cm reflectors. The ionized hydrogen in the filament surrounding the star WR 142 was shown to emit at about 10 km s-1, whereas its emission near the star WR 141 was found to occur in the velocity range 0 to 12 km s-1. A weaker H(alpha) emission was also detected at high negative (V(LSR) approximately 50 km s-1) and positive (V(LSR) approximately 20 - 45 km s-1) velocities. In the sky area under study, low-brightness regions around both stars were identified at velocities of 7.5 to 10 km s-1 (WR 141) and of 10 to 12.5 km s-1 (WR 142), which are close to the velocity of the main H(alpha)-line component, using the available distribution of CO emission. These velocities correspond to the far edge of the molecular-cloud complex. High-velocity motions in the H(alpha) line and cavities in the distribution of CO emission are likely to be caused by the ionizing radiation and wind arising from the stars WR 141 and WR 142.

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