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首页> 外文期刊>Earth, planets and space: EPS >Dust formation history of galaxies: A critical role of metallicity for the dust mass growth by accreting materials in the interstellar medium
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Dust formation history of galaxies: A critical role of metallicity for the dust mass growth by accreting materials in the interstellar medium

机译：星系的尘埃形成历史：通过在星际介质中吸收物质，金属性对于尘埃质量增长的关键作用

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This paper investigates the main driver of dust mass growth in the interstellar medium (ISM) by using a chemical evolution model of a galaxy with metals (elements heavier than helium) in the dust phase, in addition to the total amount of metals. We consider asymptotic giant branch (AGB) stars, type II supernovae (Sne II), and dust mass growth in the ISM, as the sources of dust, and SN shocks as the destruction mechanism of dust. Furthermore, to describe the dust evolution precisely, our model takes into account the age and metallicity (the ratio of metal mass to ISM mass) dependence of the sources of dust. We have particularly focused on the dust mass growth, and found that in the ISM this is regulated by the metallicity. To quantify this aspect, we introduce a "critical metallicity", which is the metallicity at which the contribution of stars (AGB stars and Sne II) equals that of the dust mass growth in the ISM. If the star-formation timescale is shorter, the value of the critical metallicity is higher, but the galactic age at which the metallicity reaches the critical metallicity is shorter. From observations, it was expected that the dust mass growth was the dominant source of dust in the Milky Way and dusty QSOs at high redshifts. By introducing a critical metallicity, it is clearly shown that the dust mass growth is the main source of dust in such galaxies with various star-formation timescales and ages. The dust mass growth in the ISM is regulated by metallicity, and we emphasize that the critical metallicity serves as an indicator to judge whether the grain growth in the ISM is the dominant source of dust in a galaxy, especially because of the strong, and nonlinear, dependence on the metallicity.
机译：本文利用星系中尘埃相中除金属总量外还含有金属（元素比氦重）的金属化学演化模型，研究了星际介质（ISM）中尘埃质量增长的主要驱动因素。我们将ISM中的渐近巨型分支（AGB）星，II型超新星（Sne II）和尘埃质量增长视为尘埃的来源，将SN冲击视为尘埃的破坏机制。此外，为精确描述粉尘的演变，我们的模型考虑了粉尘源的年龄和金属性（金属质量与ISM质量之比）的依赖性。我们特别关注尘埃的增长，发现在ISM中这受金属性的调节。为了对此方面进行量化，我们引入“临界金属性”，即恒星（AGB恒星和Sne II）的贡献等于ISM中尘埃质量增长的贡献的金属性。如果恒星形成的时间尺度较短，则临界金属性的值较高，但是金属性达到临界金属性的星系年龄较短。根据观察，可以预见，尘埃质量的增长是银河系尘埃和高红移时尘土飞扬的QSO的主要来源。通过引入临界金属性，可以清楚地表明，尘埃质量增长是这类星系中各种恒星形成的时间尺度和年龄的主要尘埃来源。 ISM中的尘埃质量增长受金属性的调节，我们强调，临界金属性可作为判断ISM中晶粒增长是否是星系中主要尘埃来源的指标，尤其是因为其强而非线性，取决于金属性。

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