Results of Long-Term Monitoring of Maser Emission in the Star-forming Region G 10.623–0.383

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: 61
Номер: 12
Год издания: 2017
Издательство: Maik Nauka/Interperiodica Publishing
Местоположение издательства: Russian Federation
Первая страница: 1061
Последняя страница: 1072
DOI: 10.1134/S1063772917120046
Аннотация: The results of a study of the maser source G 10.623-0.383 in the λ = 1.35 cm H2O line using the 22-m radio telescope of the Pushchino Radio AstronomyObservatory (Russia) and in the main hydroxyl lines (λ = 18 cm) using the Nancay Tadio Telescope (France) are presented. Uncorrelated long-term variations of the integrated intensities and the velocity centroids with characteristic times of 11 yrs (mean value) and 32 yrs, respectively, are studied. The drift of the velocity centroid may be associated with maser condensations whose material is collapsing onto the OB cluster. It is shown that the H2O maser source contains maser condensation configurations on various scales over a long time, which evolve with time. OH maser emission was only detected in the main lines at 1665 and 1667 MHz. The flux densities of the strongest emission components were variable, but their radial velocities did not change. A Zeeman pair was found at 1667 MHz with a splitting of about 1.44 km/s, corresponding to a line-of-sight magnetic field of 4.1 mG, which was preserved over at least 25 years. The characteristics of the H2O andOHmaser variability suggests that the masers are located in different parts of G 10.623–0.383.
Добавил в систему: Рудницкий Георгий Михайлович

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Results of Long-Term Monitoring of Maser Emission in the Star-forming Region G 10.623–0.383статья Исследовательская статья

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