Evolution of the H2O and OH Maser Emission in W75N

Colom, P.; Lekht, E.E.; Pashchenko, M.I.; Rudnitskii, G.M.; Tolmachev, A.M.

Авторы: Colom P., Lekht E.E., Pashchenko M.I., Rudnitskii G.M., Tolmachev A.M.
Журнал: Astronomy Reports
Том: 62
Номер: 7
Год издания: 2018
Издательство: Maik Nauka/Interperiodica Publishing
Местоположение издательства: Russian Federation
Первая страница: 440
Последняя страница: 454
DOI: 10.1134/S1063772918060045
Аннотация: The results of a study of H2O and OH maser emission in the complex region of active star formation W75N are presented. Observations were obtained using the 22-m radio telescope of the Pushchino Radio Astronomy Observatory (Russia) and the Nançay radio telescope (France). Flaring H2O maser featuresmay be identified with maser spots associated with the sources VLA 1 and VLA 2. The main H2O flares occurred in VLA 1. The flare emission was associated with either maser clusters having closely spaced radial velocities and sizes up to ∼2 AU or individual features. The maser emission is generated in a medium where turbulence on various scales is present. Analysis of the line shapes during flare maxima does not indicate the presence of the simplest structures — homogeneous maser condensations. Strong variability of the OH maser emission was observed. Zeeman splitting of the 1665-MHz line was detected for several features of the same cluster at a radial velocity of +5.5 km/s. The mean line-of-sight magnetic field in this cluster is ∼0.5 mG, directed away from the observer. Flares of the OH masers may be due to gas compression at a shock or MHD wave front.
Добавил в систему: Рудницкий Георгий Михайлович

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