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The Core Mass Function in the Orion Nebula Cluster Region: What Determines the Final Stellar Masses?
The Astrophysical Journal Letters ( IF 7.9 ) Pub Date : 2021-03-22 , DOI: 10.3847/2041-8213/abe7dd
Hideaki Takemura 1, 2 , Fumitaka Nakamura 1, 2, 3 , Shuo Kong 4, 5 , Hctor G. Arce 5 , John M. Carpenter 6 , Volker Ossenkopf-Okada 7 , Ralf Klessen 8, 9 , Patricio Sanhueza 1, 2 , Yoshito Shimajiri 2 , Takashi Tsukagoshi 2 , Ryohei Kawabe 1, 2 , Shun Ishii 2 , Kazuhito Dobashi 10 , Tomomi Shimoikura 11 , Paul F. Goldsmith 12 , lvaro Snchez-Monge 7 , Jens Kauffmann 13 , Thushara G. S. Pillai 14 , Paolo Padoan 15, 16 , Adam Ginsberg 17 , Rowan J. Smith 18 , John Bally 19 , Steve Mairs 20 , Jaime E. Pineda 21 , Dariusz C. Lis 12 , Blakesley Burkhart 22 , Peter Schilke 7 , Hope How-Huan Chen 23 , Andrea Isella 24 , Rachel K. Friesen 25 , Alyssa A. Goodman 26 , Doyal A. Harper 27
Affiliation  

Applying dendrogram analysis to the CARMA-NRO C18O (J = 1–0) data having an angular resolution of ∼8″, we identified 692 dense cores in the Orion Nebula Cluster region. Using this core sample, we compare the core and initial stellar mass functions in the same area to quantify the step from cores to stars. About 22% of the identified cores are gravitationally bound. The derived core mass function (CMF) for starless cores has a slope similar to Salpeter’s stellar initial mass function (IMF) for the mass range above 1 M , consistent with previous studies. Our CMF has a peak at a subsolar mass of ∼0.1 M , which is comparable to the peak mass of the IMF derived in the same area. We also find that the current star formation rate is consistent with the picture in which stars are born only from self-gravitating starless cores. However, the cores must gain additional gas from the surroundings to reproduce the current IMF (e.g., its slope and peak mass), because the core mass cannot be accreted onto the star with 100% efficiency. Thus, the mass accretion from the surroundings may play a crucial role in determining the final stellar masses of stars.



中文翻译:

猎户座星云星团区域的核心质量函数:是什么决定了最终的恒星质量?

将树状图分析应用于角分辨率约为 8 英寸的 CARMA-NRO C 18 O ( J = 1-0) 数据,我们在猎户座星云星团区域确定了 692 个致密核心。使用这个核心样本,我们比较了同一区域的核心和初始恒星质量函数,以量化从核心到恒星的步骤。大约 22% 的已识别核心受重力束缚。对于 1 M 以上的质量范围,无星核心的导出核心质量函数 (CMF) 具有类似于 Salpeter 的恒星初始质量函数 (IMF) 的斜率,这与之前的研究一致。我们的 CMF 在太阳下质量约为 0.1 M 处有一个峰值,这与在同一区域得出的 IMF 的峰值质量相当。我们还发现,目前的恒星形成率与恒星仅从自引力无星核心诞生的图景是一致的。然而,核心必须从周围获得额外的气体来重现当前的 IMF(例如,它的斜率和峰值质量),因为核心质量不能以 100% 的效率吸积到恒星上。因此,来自周围环境的质量吸积可能在确定恒星的最终恒星质量方面起着至关重要的作用。

更新日期:2021-03-22
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