When H ii regions are complicated: considering perturbations from winds, radiation pressure, and other effects
When H ii regions are complicated: considering perturbations from winds, radiation pressure, and other effects
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当 H ii 区域复杂时：考虑风、辐射压和其他影响的扰动
DOI：
10.1093/mnras/stz3491
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发表时间：
2019
影响因子：
4.8
通讯作者：
R. Klessen
中科院分区：
文献类型：
--
作者：
S. Geen;E. Pellegrini;R. Bieri;R. Klessen
我们探索了当风、辐射压力、重力和光子爆发被包括在内时，简单代数模型在多大程度上可以用来描述H区。我们(a)建立代数模型来描述在ρ∝r−w的幂律密度场中重力和吸积影响下光电离的H ii区域的膨胀，(b)确定描述风、辐射压力、重力和光子爆发的术语何时变得足够重要，从而影响w = 2时H ii区域的动力学，以及(c)为一组物理驱动条件求解这些表达式。我们发现，来自大质量恒星的光电离反馈是分子云尺度上反馈的主要模式，在年轻大质量恒星周围的峰值密度结构被认为在~ 0.1和10 - 100pc之间的情况下，驱动分子云加速流出。在很大范围的条件下，风和辐射对H区动力学的影响约为光电离贡献的10%。风和辐射压力的影响在高密度的情况下最为重要，无论是在靠近恒星的地方，还是在非常密集的云中，比如在银河系的中央分子带。约0.1个百分点，它们是H地区的主要驱动因素。较低的金属丰度使得光电离的相对效应随着电离气体温度的升高而增强。
We explore to what extent simple algebraic models can be used to describe H ii regions when winds, radiation pressure, gravity, and photon breakout are included. We (a) develop algebraic models to describe the expansion of photoionized H ii regions under the influence of gravity and accretion in power-law density fields with ρ ∝ r−w, (b) determine when terms describing winds, radiation pressure, gravity, and photon breakout become significant enough to affect the dynamics of the H ii region where w = 2, and (c) solve these expressions for a set of physically motivated conditions. We find that photoionization feedback from massive stars is the principal mode of feedback on molecular cloud scales, driving accelerating outflows from molecular clouds in cases where the peaked density structure around young massive stars is considered at radii between ∼0.1 and 10–100 pc. Under a large range of conditions the effect of winds and radiation on the dynamics of H ii regions is around 10 per cent of the contribution from photoionization. The effect of winds and radiation pressure is most important at high densities, either close to the star or in very dense clouds such as those in the Central Molecular Zone of the Milky Way. Out to ∼0.1 pc they are the principal drivers of the H ii region. Lower metallicities make the relative effect of photoionization even stronger as the ionized gas temperature is higher.
影响因子：
56.9
作者：
H. Sana;S. D. Mink;A. D. Koter;N. Langer;C. Evans;M. Gieles;E. Gosset;R. Izzard;J. L. Bouquin-J.
通讯作者：
H. Sana;S. D. Mink;A. D. Koter;N. Langer;C. Evans;M. Gieles;E. Gosset;R. Izzard;J. L. Bouquin-J.
不同微观物理对银河系 H ii 区 D 型扩张的相对重要性
影响因子：
4.8
作者：
Haworth T
通讯作者：
Haworth T