论文标题
恒星形成由扩展的气泡S111触发
Star Formation Triggered by the expanding bubble S111
论文作者
论文摘要
本文研究了O型恒星的辐射和机械反馈对其母体分子云的影响，并触发了未来一代恒星的形成。我们研究由嵌入式巨大恒星簇G316.80-0.05创建的红外气泡S111。由于恒星辐射，由于膨胀气泡通过膨胀而产生的壳中的气体大部分。因此，最好使用单一离子化碳（最主要的物种）的光谱观测来对壳的运动学进行研究。我们已经使用了$^2 {\ rm p} _ {\ rm p} _ {3/2} \ rightarrow^2 {\ rm p} _ {1/2} $在158 micron，j = 2-1的13co和c18o tribe j = 1-1-0的hh = 2-1的hH = 2-1的themim he = 2-1的+ = 1-1co^h的速度^2 {1/2} $ the [c ii]的过渡+ = 1-1-0这部分与红外深色山脊G316.75的南部相吻合。 [C II]光谱最终显示了壳膨胀的证据，中度速度约为7 km/s，相当于动能，大约是H II区域热能的0.5-40倍。引起H II区域膨胀的压力主要源于氢离子化和粉尘处理的辐射。在压缩壳中的远红外源中，我们发现Core G316.7799-0.0942显示出与流出活动一致的宽光谱特征，并得出结论，它是活动恒星形成的位点。根据H II区域的年龄，我们得出结论，该扩展的H II区域是触发该区域当前恒星形成活性的原因。
This paper investigates the impact of radiative and mechanical feedback from O-type stars on their parent molecular clouds and the triggering of formation of future generation of stars. We study the infrared bubble S111 created by the embedded massive stellar cluster G316.80-0.05. A significant fraction of gas in shells created due to the compression of the ambient medium by expanding bubbles is photodissociated by the stellar radiation. The kinematics of the shells are thus best studied using spectroscopic observations of singly ionized carbon, the most dominant species. We have used the velocity-resolved maps of the $^2{\rm P}_{3/2}\rightarrow ^2{\rm P}_{1/2}$ transition of [C II] at 158 micron, the J=2-1 transition of 13CO and C18O, and the J=1-0 transition of HCO^+ to study the rim of the bubble S111 that partly coincides with the southern part of the infrared dark ridge G316.75. The [C II] spectra conclusively show evidence of a shell expanding with a moderate velocity of ~7 km/s, which amounts to a kinetic energy that is ~0.5-40 times the thermal energy of the H II region. The pressure causing the expansion of the H II region arises mainly from the hydrogen ionization and the dust-processed radiation. Among the far-infrared sources located in the compressed shells, we find the core G316.7799-0.0942 to show broad spectral features consistent with outflow activity and conclude that it is a site of active star formation. Based on the age of the H II region we conclude that this expanding H II region is responsible for the triggering of the current star formation activity in the region.
