The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM
The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM
复制标题
SILCC（模拟分子云的生命周期）项目 – I. 超新星驱动的 ISM 的化学演化
DOI：
--
复制
发表时间：
2014
期刊：
影响因子：
--
通讯作者：
C. Baczynski
中科院分区：
文献类型：
--
作者：
S. Walch;P. Girichidis;T. Naab;A. Gatto;S. Glover;R. Wünsch;R. Klessen;R. Klessen;R. Klessen;P. Clark;T. Peters;D. Derigs;C. Baczynski
SILCC（模拟分子云的生命周期）项目旨在自洽地了解星际介质（ISM）的小尺度结构及其与星系演化的联系。我们模拟了银河盘 (500 pc)2 × ±5 kpc 区域中多相 ISM 的演化，气体表面密度为 ΣGAS=10M⊙pc−2。 flash 4 模拟包括外部电势、自重力、磁场、加热和辐射冷却、考虑（自）屏蔽的 H2 和 CO 的时间相关化学以及超新星 (SN) 反馈，但忽略了由于星系旋转而产生的剪切。我们在高密度区域（峰值）、垂直方向上具有高斯分布的随机位置（随机）、两者的组合（混合）或在空间和时间上聚集（clus/clus2）以不同速率探索超新星爆炸。只有具有自重力和相当一部分超新星在低密度气体中爆炸的模型才与观测结果一致。在没有自重力的情况下，在具有峰值驱动的模型中，H2 的形成受到强烈抑制。对于降低的 SN 率，H2 质量分数显着增加，从高 SN 率的 <10%，即高于 Kennicutt-Schmidt 0.5 dex，到低 SN 率的 70-85%，即低于 KS 0.5 dex。对于中等 SN 率，由于较大气泡中气体的相干压缩程度更高，因此集群驱动比随机驱动产生的 H2 略多。磁场对最终的盘结构影响不大，但会影响稠密气体 (n ≳ 10 cm−3) 并延迟 H2 的形成。大部分体积充满热气体（±150 pc 内约 80%）。对于除了峰值驱动之外的所有情况，原子氢的垂直膨胀的温暖成分都表明喷泉流。我们强调，各个化学物质占据不同的 ISM 相，并且无法使用基于温度/密度的相截止值进行准确建模。
The SILCC (SImulating the Life-Cycle of molecular Clouds) project aims to self-consistently understand the small-scale structure of the interstellar medium (ISM) and its link to galaxy evolution. We simulate the evolution of the multiphase ISM in a (500 pc)2 × ±5 kpc region of a galactic disc, with a gas surface density of ΣGAS=10M⊙pc−2. The flash 4 simulations include an external potential, self-gravity, magnetic fields, heating and radiative cooling, time-dependent chemistry of H2 and CO considering (self-) shielding, and supernova (SN) feedback but omit shear due to galactic rotation. We explore SN explosions at different rates in high-density regions (peak), in random locations with a Gaussian distribution in the vertical direction (random), in a combination of both (mixed), or clustered in space and time (clus/clus2). Only models with self-gravity and a significant fraction of SNe that explode in low-density gas are in agreement with observations. Without self-gravity and in models with peak driving the formation of H2 is strongly suppressed. For decreasing SN rates, the H2 mass fraction increases significantly from <10 per cent for high SN rates, i.e. 0.5 dex above Kennicutt–Schmidt, to 70–85 per cent for low SN rates, i.e. 0.5 dex below KS. For an intermediate SN rate, clustered driving results in slightly more H2 than random driving due to the more coherent compression of the gas in larger bubbles. Magnetic fields have little impact on the final disc structure but affect the dense gas (n ≳ 10 cm−3) and delay H2 formation. Most of the volume is filled with hot gas (∼80 per cent within ±150 pc). For all but peak driving a vertically expanding warm component of atomic hydrogen indicates a fountain flow. We highlight that individual chemical species populate different ISM phases and cannot be accurately modelled with temperature-/density-based phase cut-offs.
登录
查看更多内容
DOI：
10.1088/0004-637x/768/1/74
发表时间：
2012-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-
通讯作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-
影响因子：
4.8
作者：
S. Walch;T. Naab
通讯作者：
S. Walch;T. Naab
影响因子：
4.8
作者：
C. Brook;G. Stinson;Bradley K Gibson;Bradley K Gibson;S. Shen;A. Macciò;A. Obreja;J. Wadsley;Thomas P. Quinn
通讯作者：
C. Brook;G. Stinson;Bradley K Gibson;Bradley K Gibson;S. Shen;A. Macciò;A. Obreja;J. Wadsley;Thomas P. Quinn
影响因子：
4.8
作者：
F. Gent;A. Shukurov;G. Sarson;A. Fletcher;M. Mantere
通讯作者：
F. Gent;A. Shukurov;G. Sarson;A. Fletcher;M. Mantere
DOI：
10.1088/0004-637x/739/1/45
发表时间：
2011-04
期刊：
The Astrophysical Journal
影响因子：
--
作者：
N. F. Schreiber;A. Shapley;R. Genzel;N. Bouché;G. Cresci;R. Davies;D. Erb;S. Genel;D. Lutz
通讯作者：
N. F. Schreiber;A. Shapley;R. Genzel;N. Bouché;G. Cresci;R. Davies;D. Erb;S. Genel;D. Lutz