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Introduction to astrochemistry: chemical evolution from interstellar clouds to star and planet formation
Contemporary Physics ( IF 2 ) Pub Date : 2019-06-20 , DOI: 10.1080/00107514.2019.1621938
B. Ishak 1
Affiliation  

That helium hydride, HeH+, should exist in astrophysical plasma was just an idea to begin with [1]. The odds that this super-ancient molecule – the first ever to have been synthesised after the Big Bang – could be found today have always been very slim. Therefore, when the news broke out on 17 April 2019 that it has at last been detected [2], some took it with only the proverbial amount of salt. While it is understood that one signature is somewhat dicey, the result is still a big milestone in astrophysics and astrochemistry. Helium hydride is essentially the beginning of everything. The entire history of the chemical evolution of the Universe rides on it. ‘The depletion of molecules onto dust grains is widely recognized as playing an important role in chemical evolution of molecular cloud’ is one of the takeaways of this book. Using ‘molecular clouds are where stars are born’ as the basis, it starts by taking us through the step-by-step journey of how carbon-, oxygen-, nitrogenand sulphur-bearing molecules are formed in these clouds. We are then introduced to the significance of the gas-phase and the gas-grain chemical processes. Although the chemistry of molecular clouds can be explained by both, the latter is more preferable when it comes to modelling. From molecular clouds, we continue with the chemical evolution that gives us the lowand high-mass stars and the proto-planets. The book does not go any further, but knowing what the clouds, starforming regions and protoplanetary disks are like at that particular phases is more than enough for a taster course. Written to be read sequentially unless the readers are already familiar with blackbody, radiative transfer, molecular abundance and chemical reaction that the first three chapters can be passed over, Introduction to Astrochemistry assumes an adequate background in chemistry (and, naturally, astrophysics). Designed for serious researchers in astrochemistry, planetary science and molecular science as well as those new to the subjects, it comes with end-ofchapter problems that are worth tackling; solutions to them are available, too. Others who are merely curious will also find it a good alternative (relatively) light reading.

中文翻译:

天体化学导论:从星际云到恒星和行星形成的化学演化

天体物理等离子体中应该存在氢化氦 HeH+ 只是一个想法 [1]。这种超古老的分子——第一个在大爆炸后合成的分子——在今天被发现的可能性一直很小。因此,当 2019 年 4 月 17 日消息传出它终于被检测到 [2] 时,有些人只用了众所周知的盐量。据了解,一个签名有点冒险,但结果仍然是天体物理学和天体化学的一个重要里程碑。氢化氦本质上是一切的开始。宇宙化学演化的整个历史都基于它。“分子在尘埃颗粒上的消耗被广泛认为在分子云的化学演化中起着重要作用”是本书的要点之一。以“分子云是恒星诞生的地方”为基础,它首先带我们逐步了解这些云中含碳、氧、氮和硫的分子是如何形成的。然后我们将介绍气相和气粒化学过程的重要性。虽然分子云的化学性质可以用两者来解释,但在建模时后者更可取。从分子云中,我们继续进行化学演化,从而为我们提供了低质量和高质量恒星以及原始行星。这本书没有更进一步,但了解云、恒星形成区域和原行星盘在特定阶段的情况对于品尝课程来说已经绰绰有余了。除非读者已经熟悉黑体、辐射转移、前三章可以跳过分子丰度和化学反应,天体化学导论假设有足够的化学背景(当然还有天体物理学)。专为天体化学、行星科学和分子科学领域的认真研究人员以及这些学科的新手而设计,它带有值得解决的章末问题;他们的解决方案也是可用的。其他只是好奇的人也会发现它是一个很好的替代(相对)轻松阅读。它带有值得解决的章末问题;他们的解决方案也是可用的。其他只是好奇的人也会发现它是一个很好的替代(相对)轻松阅读。它带有值得解决的章末问题;他们的解决方案也是可用的。其他只是好奇的人也会发现它是一个很好的替代(相对)轻松阅读。
更新日期:2019-06-20
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