利用Н110a射电重组线观测确定W40 HII区域的物理参数

IF 0.2 Q4 PHYSICS, MULTIDISCIPLINARY
A.B. Manapbayeva
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引用次数: 0

摘要

HII区域是星际气体的电离区域,它被附近热恒星强烈的紫外线辐射电离。射电复合谱线是研究HII区域的主要工具之一,特别是通过氢谱线获得HII的分布,确定星际物质的主要物理条件。本研究是基于对Aquila分子云中最活跃的恒星形成区之一W40 HII区域的H110a重组发射线的分析进行的。我们使用了2015年2月中国科学院新疆天文台26m南山射电望远镜在Aquila分子云中获得的H110a射电重组线的档案观测数据。在研究期间,构建了H110a向W40 HII区域的综合强度图和相应的光谱。计算了HII区的电子密度和温度、发射量、光学厚度、莱曼连续通量、激发参数、Strömgren球半径和球内电离氢的质量。发射测量值和光学厚度表明,h10a复合射电谱线在光学上很薄,并在高电子温度下追踪到一个非常致密的区域(<6462 AU)。莱曼连续体的光子数量表明存在一颗巨大的O9.5恒星,相当于一颗位于HII区域的零年龄主序星。得到的物理参数值表明,所研究的电离氢区域是一个超紧区。本文的研究结果为进一步研究HII区域的演化及其在恒星形成过程中的作用奠定了基础。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Determination of physical parameters of the W40 HII region using observations of Н110a radio recombination line
HII regions are ionized regions of interstellar gas, which ionized by intensive ultraviolet radiation from nearby hot stars. Radio recombination line is one of the main tools for investigating the HII region, in particular, the distribution of HII is obtained and the main physical conditions of the interstellar matter are determined from hydrogen lines. This study was carried out based on the analysis of the H110a recombination emission line toward the W40 HII region, which is one of the most active star-forming regions in the Aquila Molecular Cloud. We used archival observational data of the H110a radio recombination line in the Aquila Molecular Cloud, obtained during February in 2015 using the 26m NanShan radiotelescope in the Xinjiang Astronomical Observatory of the Chinese Academy of Sciences. During the period of the study, an integrated intensity map of H110a toward the W40 HII region and the corresponding spectra were constructed. The electron density and temperature of the HII region, the emission measure, the optical thickness, the Lyman continuum flux, the excitation parameter, the radius of the Strömgren sphere, and the mass of ionized hydrogen inside the sphere were calculated. The values of the emission measure and optical thickness indicate that the H110a recombination radio line is optically thin and traces a very dense region (<6462 AU) with a high electron temperature. The numbers of photons of the Lyman continuum indicates the presence of a massive O9.5 star, that equivalent to a zero-age main-sequence star located within the HII region. The obtained values of the physical parameters indicate that the region of ionized hydrogen under study is an ultracompact region. The results of this article lay the foundation for further research aimed at studying the evolution of HII regions, as well as their role in the processes of starformation.
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