恒星形成区G10.32-0.15中反馈机制的研究  

Study the Feedback Mechanism in Star Forming Region G10.32-0.15

作　　者：张幸 李大磊[2] 加尔肯·叶生别克[1,2] ZHANG Xing;LI Dalei;ESIMBEK Jarken(University of Xingjing,Urumqi 830046,China;XinJiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China)

机构地区：[1]新疆大学,乌鲁木齐830046 [2]中国科学院新疆天文台,乌鲁木齐830011

出　　处：《天文学进展》2024年第4期639-649,共11页Progress In Astronomy

基　　金：中国科学院青年创新促进会;上海合作组织科技伙伴计划及国际科技合作计划(2022E01050)。

摘　　要：反馈在恒星形成过程中扮演着重要角色,对于恒星和行星的形成、星团和母体分子云的演化都具有重要影响。利用多波段的红外数据以及亚毫米波的连续谱数据确定了恒星星团的位置以及致密尘埃团块C1、C2、C3、C4和C5的分布。NH_(3)速度积分强度的分布与870μm示踪的致密尘埃的分布具有很好的成协性,表明NH_(3)能很好地示踪致密分子气体。在局域热动平衡的假设下,结合NH_(3)(1,1)和NH_(3)(2,2)的分子谱线数据,通过辐射转移计算获取了分子气体的速度场、速度弥散、旋转温度、NH_(3)柱密度以及波束填充因子的分布。通过进一步的计算,得到了G10.32-0.15中气体的运动温度、声速、非热速度弥散、热压与非热压的比值以及马赫数。综合分析以上结果,表明G10.32-0.15中的致密气体可能受到了恒星形成区多种反馈机制的影响:C1区域的气体可能受到热反馈的影响,C2和C3区域的气体可能受到爆炸反馈的影响,C4和C5区域的气体可能受到动量反馈的影响。恒星形成区G10.32-0.15与周围的致密气体存在着复杂的相互作用,不同区域的气体可能由不同反馈机制主导。Feedback plays an important role in star formation and strongly impacts the formation of stars and planets,and the evolution of the star cluster and the parental molecular cloud.Multi-wavelength studies of star forming region G10.32-0.15 were conducted using the NH_(3)(1,1)and NH_(3)(2,2)spectrum line data of the ammonia molecule observed with the GBT and with the inclusion of multi-wavelength continuum data from the cm,sub-mm to infrared bands.The infrared star cluster and dense dust clumps C1,C2,C3,C4 and C5 are identified in the source based on the multi-wavelength infrared and sub-mm continuum data.The NH_(3) velocity-integrated intensity distribution is clearly associated with the dense dust distribution detected by 870m emission,indicating that NH_(3) is a good dense gas tracer.The distribution of velocity,velocity dispersion,rotation temperature,NH_(3) column density and filling factor can be derived by fitting a radiation transfer model to the NH_(3)(1,1)and NH_(3)(2,2)data under the assumption of Local Thermal Equilibrium.Furthermore,the kinetic temperature,the sound speed,the non-thermal velocity dispersion,the ratio between thermal pressure and non-thermal pressure,and the Mach number are derived based on those fitted parameters.From the above results,the dense gas in G10.32-0.15 is affected by multiple feedback processes:the dense gas in C1 is likely affected by thermal feedback,the dense gas in C2 and C3 is likely affected by explosive feedback,and the dense gas in C4 and C5 is likely affected by momentum feedback.Therefore,very complicated interactions exist between the infrared star cluster and the surrounding gas and different feedback mechanisms maybe dominate the different regions in G10.32-0.15.

关 键 词：分子云 分子谱线 恒星形成 

分 类 号：P142.9[天文地球—天体物理]