Magnetic fields and the earliest stages of star cluster formation

磁场和星团形成的最早阶段

基本信息

  • 批准号:
    2893056
  • 负责人:
  • 金额:
    --
  • 依托单位:
  • 依托单位国家:
    英国
  • 项目类别:
    Studentship
  • 财政年份:
    2023
  • 资助国家:
    英国
  • 起止时间:
    2023 至 无数据
  • 项目状态:
    未结题

项目摘要

Stars light up every single galaxy across the Universe, allowing us to study their structure across the cosmos. Despite their importance, there are still many aspects of the star formation process that remain poorly constrained. We know that stars form as the result of the fragmentation and collapse of large interstellar clouds of cold molecular gas. However, we do not know what triggers that collapse, whether it is driven by gravitational instabilities, turbulent compression, magnetic field diffusion, or some combination of all three. The turbulence (via the measurement of the width of spectral line emission) and gravity (via the measurement of gas masses) of interstellar molecular clouds are routinely characterised. However, magnetic fields are a lot more complicated to observe. But in the past few years, as the result of technological advancements, it has become easier to derive the direction of magnetic fields in cold interstellar clouds. This is done by observing the sub-millimetre polarisation emission of dust grains that pervade the interstellar medium. The direction of the polarised light directly tells you in which direction the magnetic field is in the plane-of-the-sky. Instruments like POL2 on the JCMT is at the forefront of such state-of-the-art observations. Recently, Peretto et al. (to be submitted) showed that that clumps, i.e. the progenitors of stellar clusters, are dynamically decoupled from their parent molecular clouds, probably as the result of their global collapse. However, it is unclear if this collapse finds its origin in the change of magnetic field properties.In the context of this PhD project, the student will analyse brand new JCMT POL2 observations of a number of clumps (>10), characterise the magnetic field morphology in those. Morphology of the magnetic field in the larger scale molecular clouds will be determined by using Planck and GPIPS data. Connecting the different magnetic field datasets will allow us to determine whether or not the observed dynamical transition is matched by a transition in magnetic field properties which could be an indication that it is at the origin of the clump collapse.In a second step, the student will characterise the correlations between the clump magnetic field directions and gas velocity gradients, both in the observations and numerical simulations of cloud evolution, with the goal of determining whether magnetic fields are entrained by gravity in the densest regions or not. The student taking on this PhD will find themselves at the forefront of star formation research and will be in an excellent position to take full advantage of future polarisation instrumentations that will be developed in the next few years.
星星照亮了整个宇宙中的每个星系,使我们能够研究它们在宇宙中的结构。尽管它们的重要性,但恒星形成过程仍然有很多方面的约束。我们知道,恒星是由于冷分子气体的碎裂和崩溃的结果。但是,我们不知道是什么触发因素,无论是由重力不稳定性,湍流压缩,磁场扩散还是所有三个组合的组合驱动的。常规表征了星际分子云的湍流(通过光谱线发射的宽度测量)和重力(通过气体质量测量)。但是,磁场要观察到更为复杂。但是在过去的几年中,由于技术进步的结果,在冷星云中得出磁场方向变得更加容易。这是通过观察到星际培养基的粉尘晶粒的亚毫米偏振发射来完成的。偏振光的方向直接告诉您磁场在天空飞机中的哪个方向。 JCMT上的POL2之类的乐器处于此类最新观察的最前沿。最近,Peretto等。 (待提交)表明,团块,即恒星簇的祖细胞,可能是由于它们的全球崩溃而动态地与它们的母分子云解耦。但是,目前尚不清楚这种崩溃是否在磁场特性的变化中发现了其起源。在该博士学位项目的背景下,学生将分析全新的JCMT POL2观察到许多团块(> 10),表征了其中的磁场形态。大规模分子云中磁场的形态将通过使用Planck和GPIPS数据来确定。 Connecting the different magnetic field datasets will allow us to determine whether or not the observed dynamical transition is matched by a transition in magnetic field properties which could be an indication that it is at the origin of the clump collapse.In a second step, the student will characterise the correlations between the clump magnetic field directions and gas velocity gradients, both in the observations and numerical simulations of cloud evolution, with the goal of determining whether magnetic fields are entrained by是否在最密集区域中的重力。攻读这项博士学位的学生将发现自己处于星际构成研究的最前沿,并且将在未来几年中充分利用未来的两极分化仪器的优势。

项目成果

期刊论文数量(0)
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会议论文数量(0)
专利数量(0)

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