探索恒星形成的物理学原理(ProPStar)

IF 5.4 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
Jaime E. Pineda, Juan D. Soler, Stella Offner, Eric W. Koch, Dominique M. Segura-Cox, Roberto Neri, Michael Kuffmeier, Alexei V. Ivlev, Maria Teresa Valdivia-Mena, Olli Sipilä, Maria Jose Maureira, Paola Caselli, Nichol Cunningham, Anika Schmiedeke, Caroline Gieser, Michael Chen, Silvia Spezzano
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引用次数: 0

摘要

背景。湍流是分子云结构的关键组成部分。它通常由能量级联直至耗散尺度来描述。亚音速不可压缩湍流的功率谱为∝k-5/3,而超音速湍流的功率谱为∝k-2。我们测定了活跃恒星形成分子云的功率谱,从等秒尺度一直到预期的磁流体动力(MHD)波截止(耗散尺度)。我们用三种不同的示踪剂分析了对附近 NGC 1333 恒星形成区的观测,涵盖了从∼10 pc 到 20 mpc 的不同尺度。最大尺度采用单碟获得的低密度气体示踪剂 13CO (1-0),中等尺度采用 C18O (3-2) 线的单碟观测,而最小尺度采用 H13CO+ (1-0) 和 HNC (1-0),结合 NOEMA 干涉仪和 IRAM 30m 单碟观测。这些观测数据的互补性使我们能够生成空间尺度超过两个数量级的组合功率谱。我们推导出了一个活跃恒星形成区的功率谱,其空间尺度跨度超过 20 倍。强度图的功率谱显示出单一的幂律行为,指数为 2.9 ± 0.1,没有耗散的迹象。此外,有证据表明,离子的功率谱在较小尺度上比中性离子具有更大的功率,这与理论预期相反。我们展示了干涉测量观测为研究恒星形成区小尺度能量耗散提供的新可能性。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Probing the physics of star formation (ProPStar)
Context. Turbulence is a key component of molecular cloud structure. It is usually described by a cascade of energy down to the dissipation scale. The power spectrum for subsonic incompressible turbulence is ∝k−5/3, while for supersonic turbulence it is ∝k−2.Aims. We determine the power spectrum in an actively star-forming molecular cloud, from parsec scales down to the expected magnetohydrodynamic (MHD) wave cutoff (dissipation scale).Methods. We analyzed observations of the nearby NGC 1333 star-forming region in three different tracers to cover the different scales from ∼10 pc down to 20 mpc. The largest scales are covered with the low-density gas tracer 13CO (1–0) obtained with a single dish, the intermediate scales are covered with single-dish observations of the C18O (3–2) line, while the smallest scales are covered in H13CO+ (1–0) and HNC (1–0) with a combination of NOEMA interferometer and IRAM 30m single-dish observations. The complementarity of these observations enables us to generate a combined power spectrum covering more than two orders of magnitude in spatial scale.Results. We derive the power spectrum in an active star-forming region spanning more than 2 decades of spatial scales. The power spectrum of the intensity maps shows a single power-law behavior, with an exponent of 2.9 ± 0.1 and no evidence of dissipation. Moreover, there is evidence that the power spectrum of the ions to have more power at smaller scales than the neutrals, which is opposite to the theoretical expectations.Conclusions. We show new possibilities for studying the dissipation of energy at small scales in star-forming regions provided by interferometric observations.
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来源期刊
Astronomy & Astrophysics
Astronomy & Astrophysics 地学天文-天文与天体物理
CiteScore
10.20
自引率
27.70%
发文量
2105
审稿时长
1-2 weeks
期刊介绍: Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
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