Evolution of the H2O maser emission in G10.6-0.4 |
| |
| Authors: | E E Lekht N A Silant’ev V V Krasnov V A Munitsyn |
| |
| Institution: | (1) Instituto Nacional de Astrofísica, óptica y Electrónica, Luis Enrique Erro No. 1 Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla, México;(2) Sternberg Astronomical Institute, Universitetskiĭ pr. 13, Moscow, 119992, Russia;(3) Main Astronomical Observatory, Russian Academy of Sciences, Pulkovo, St. Petersburg, 196140, Russia;(4) Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997, Russia;(5) Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117810, Russia |
| |
| Abstract: | The water-vapor maser emission in the source G10.6-0.4 associated with an active starforming region (OB star cluster) is analyzed. The maser was monitored from 1981–2004 using the 22-meter radio telescope of the Pushchino Radio Astronomy Observatory. Statistical processing of the results revealed the presence of structural formations on various scales. The individual H2O maser features may form ordered structures with velocity (V LSR) gradients, localized in separate clusters of maser features. The statistical variations of the V LSR values for the maser components may be due to the accretion of material onto the OB star cluster in G10.6-0.4 together with the rotation of the molecular cloud core. A model with a rotating, nonuniform condensation of accreted material in the vicinity of the stellar cluster is proposed to explain the variations of the velocity centroid of the H2O spectra. The integrated flux variations are explained well by a model in which the central source is an OB star cluster, possibly containing five to six stars. An important role in the evolution of the maser emission, as well as of the source as a whole, may be played by turbulent motions of the gas. |
| |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ |
|
