Evolution of the H2O Maser Emission Zone in ON2 N

被引：0
|
作者：
Lekht, E. E. [1 ]
Slysh, V. I. [2 ]
Tolmachev, A. M. [3 ]
机构：
[1] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia
[2] Russian Acad Sci, Astrospace Ctr, PN Lebedev Phys Inst, Moscow 117997, Russia
[3] Russian Acad Sci, Pushchino Radio Astron Observ, Ctr Astro Space, PN Lebedev Phys Inst, Pushchino 142290, Moscow Oblast, Russia
来源：
ASTRONOMY REPORTS | 2010年 / 54卷 / 06期
基金：
俄罗斯基础研究基金会;
关键词：
H-II REGIONS; WATER MASER;
D O I：
10.1134/S1063772910060041
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Results of a multi-faceted study of the H2O maser emission in the region ON2 N carried out on the Very Large Array (VLA, NRAO) and 22-m radio telescope of the Pushchino Radio Astronomy Observatory are reported. The envelope around the ultracompact HII region is fairly extended and has a composite, strongly fragmented structure. The maser emission zone consists of single spots and spot clusters arranged along an arc, which is associated with a ram shock front. This shock front is nonsta-tionary, and its position changes with time. The front position probably depends on the state of activity of the central star. There can be turbulent motions of material in clusters as well as individual maser spots (such as turbulent vortices). In the turbulent-vortex model, the size of an H2O maser spot is estimated to be 0.07-0.1 AU. Flux-correlated radial-velocity drifts of emission features have been detected, which can be accompanied by spatial displacement (proper motion) of maser spots.
引用
收藏
页码：509 / 513
页数：5
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