Sizes of Masing Parts of Massive Star Forming Regions

It is shown that the images, line profiles, and time evolution of different interstellar masing transitions can be explained by the hypothesis that the population inversions giving birth to masers take place in turbulent regions with extents that are orders of magnitude greater than the sizes of the...

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Дата:2012
Автори: Sobolev, A. M., Sutton, E. C., Watson, W. D., Ostrovskii, A. B., Shelemei, O. V.
Формат: Стаття
Мова:Російська
Опубліковано: Видавничий дім «Академперіодика» 2012
Онлайн доступ:http://rpra-journal.org.ua/index.php/ra/article/view/550
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Назва журналу:Radio physics and radio astronomy

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Radio physics and radio astronomy
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author Sobolev, A. M.
Sutton, E. C.
Watson, W. D.
Ostrovskii, A. B.
Shelemei, O. V.
author_facet Sobolev, A. M.
Sutton, E. C.
Watson, W. D.
Ostrovskii, A. B.
Shelemei, O. V.
author_sort Sobolev, A. M.
baseUrl_str
collection OJS
datestamp_date 2012-12-09T20:56:27Z
description It is shown that the images, line profiles, and time evolution of different interstellar masing transitions can be explained by the hypothesis that the population inversions giving birth to masers take place in turbulent regions with extents that are orders of magnitude greater than the sizes of the maser spots. It is shown that the images of methanol masers in the turbulent model persist within considerable time and do not prevent measurement of the annual parallaxes using data on the 12 GHz methanol maser positions.
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spelling rpra-journalorgua-article-5502012-12-09T20:56:27Z Sizes of Masing Parts of Massive Star Forming Regions Sizes of Masing Parts of Massive Star Forming Regions Sobolev, A. M. Sutton, E. C. Watson, W. D. Ostrovskii, A. B. Shelemei, O. V. It is shown that the images, line profiles, and time evolution of different interstellar masing transitions can be explained by the hypothesis that the population inversions giving birth to masers take place in turbulent regions with extents that are orders of magnitude greater than the sizes of the maser spots. It is shown that the images of methanol masers in the turbulent model persist within considerable time and do not prevent measurement of the annual parallaxes using data on the 12 GHz methanol maser positions. It is shown that the images, line profiles, and time evolution of different interstellar masing transitions can be explained by the hypothesis that the population inversions giving birth to masers take place in turbulent regions with extents that are orders of magnitude greater than the sizes of the maser spots. It is shown that the images of methanol masers in the turbulent model persist within considerable time and do not prevent measurement of the annual parallaxes using data on the 12 GHz methanol maser positions. Видавничий дім «Академперіодика» 2012-12-09 Article Article application/pdf http://rpra-journal.org.ua/index.php/ra/article/view/550 РАДИОФИЗИКА И РАДИОАСТРОНОМИЯ; Vol 13, No 3 (2008); 76 RADIO PHYSICS AND RADIO ASTRONOMY; Vol 13, No 3 (2008); 76 РАДІОФІЗИКА І РАДІОАСТРОНОМІЯ; Vol 13, No 3 (2008); 76 2415-7007 1027-9636 ru http://rpra-journal.org.ua/index.php/ra/article/view/550/124
spellingShingle Sobolev, A. M.
Sutton, E. C.
Watson, W. D.
Ostrovskii, A. B.
Shelemei, O. V.
Sizes of Masing Parts of Massive Star Forming Regions
title Sizes of Masing Parts of Massive Star Forming Regions
title_alt Sizes of Masing Parts of Massive Star Forming Regions
title_full Sizes of Masing Parts of Massive Star Forming Regions
title_fullStr Sizes of Masing Parts of Massive Star Forming Regions
title_full_unstemmed Sizes of Masing Parts of Massive Star Forming Regions
title_short Sizes of Masing Parts of Massive Star Forming Regions
title_sort sizes of masing parts of massive star forming regions
url http://rpra-journal.org.ua/index.php/ra/article/view/550
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