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How do methanol masers manage to appear in the youngest star vicinities
and isolated molecular clumps? | | A.M. Sobolev
; D.M. Cragg
; S.P. Ellingsen
; M.J. Gaylard
; S. Goedhart
; C. Henkel
; M.S. Kirsanova
; A.B. Ostrovskii
; N.V. Pankratova
; O.V. Shelemei
; D.J. van der Walt
; T.S. Vasyunina
; M.A. Voronkov
; | | Date: |
21 Jun 2007 | | Abstract: | General characteristics of methanol (CH3OH) maser emission are summarized. It
is shown that methanol maser sources are concentrated in the spiral arms. Most
of the methanol maser sources from the Perseus arm are associated with embedded
stellar clusters and a considerable portion is situated close to compact HII
regions. Almost 1/3 of the Perseus Arm sources lie at the edges of optically
identified HII regions which means that massive star formation in the Perseus
Arm is to a great extent triggered by local phenomena. A multiline analysis of
the methanol masers allows us to determine the physical parameters in the
regions of maser formation. Maser modelling shows that class II methanol masers
can be pumped by the radiation of the warm dust as well as by free-free
emission of a hypercompact region hcHII with a turnover frequency exceeding 100
GHz. Methanol masers of both classes can reside in the vicinity of hcHIIs.
Modelling shows that periodic changes of maser fluxes can be reproduced by
variations of the dust temperature by a few percent which may be caused by
variations in the brightness of the central young stellar object reflecting the
character of the accretion process. Sensitive observations have shown that the
masers with low flux densities can still have considerable amplification
factors. The analysis of class I maser surveys allows us to identify four
distinct regimes that differ by the series of their brightest lines. | | Source: | arXiv, arxiv.0706.3117 | | Services: | Forum | Review | PDF | Favorites | |
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