Simulating Dense Gas in Active Galactic Nuclei, Tidal Disruption Events, and Supernovae

模拟活跃星系核、潮汐破裂事件和超新星中的致密气体

• 批准号: 1816537
• 负责人: Gary Ferland
• 金额: $ 47.51万
• 依托单位: University of Kentucky Research Foundation
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2018
• 资助国家: 美国
• 起止时间: 2018-07-01 至 2023-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1816537&HistoricalAwards=false
• 关键词: Simulating; Dense; Gas; Active; Galactic

Part 1Astronomy is an observational, not experimental, science. We cannot go to a star and directly measure its temperature, density, or how it makes energy. Rather, we discover these things by careful study of their light at different colors. Complex interactions between atoms and molecules produce light. The PIs are developing a large computer program, Cloudy, to predict this. Cloudy solves the complex equations of quantum mechanics and relativity. Astronomers use Cloudy to simulate what is happening in a distant star or galaxy and predict the emitted light. This is compared with what is seen through telescopes. This comparison makes it possible to understand what is happening. Cloudy is freely available and is among the more widely used codes in astronomy.The PIs will do two types of broader impact. They organize international workshops showing how to apply Cloudy to research projects. The Co-PI, a native of Spain, will visit local K-12 schools with large Hispanic populations. He does Spanish language talks and presentations. Hispanic students and their families visit the university for astronomy talks and viewing with the MacAdam Student Observatory.Part 2 Astronomy is an observational, not experimental, science. We cannot directly measure the temperature, density, or energy source for a star or galaxy. We discover these things by quantitative spectroscopy, the careful study of the observed spectrum. Astronomical sources are usually far from equilibrium. Their spectra depend on a number of thermal, plasma, chemical, and condensed matter processes. Analytical solutions are not possible. The code Cloudy solves all of this, numerically, to predict the spectrum. These predictions are compared that observations to infer properties of a star or galaxy. Cloudy is one of the more widely used theory codes in astrophysics with more than 300 papers citing its documentation per year.Cloudy has long solved these problems using available computers and atomic data. The simulations can be improved as computers become more powerful and the atomic data more accurate. We are developing techniques to improve modeling of the dense gas found near black holes or exploding stars. A full treatment of the "Rydberg levels," the highly excited orbits of electrons around ions, is the key improvement. This work will have an influence well beyond this project because of Cloudy's broad community use.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.

第1部分是一种观察性的，而不是实验性的科学。 我们不能去恒星，直接测量其温度，密度或如何产生能量。 相反，我们通过仔细研究它们的光线以不同的颜色发现了这些东西。 原子与分子之间的复杂相互作用会产生光。 PI正在开发一个大型计算机程序Cloudy，以预测这一点。 多云解决了量子力学和相对论的复杂方程。 天文学家使用多云来模拟遥远的恒星或星系中发生的事情，并预测发射光。 这与通过望远镜看到的相比。 这种比较使您可以了解正在发生的事情。 多云可自由使用，并且是天文学中使用最广泛的代码之一。PIS将对两种类型的更广泛的影响产生更广泛的影响。 他们组织了国际研讨会，展示了如何将多云应用于研究项目。 Co-Pi是西班牙人，将访问拥有大量西班牙裔人口的当地K-12学校。 他进行西班牙语的演讲和演讲。 西班牙裔学生及其家人访问大学进行天文学谈判，并与麦克丹学生天文台进行观看。第2部分天文学是一种观察性的，而不是实验性的科学。 我们无法直接测量恒星或星系的温度，密度或能源。 我们通过定量光谱法发现了这些事物，这是对观察到的光谱的仔细研究。 天文来源通常远非平衡。 它们的光谱取决于许多热，等离子体，化学和冷凝物质过程。 分析解决方案是不可能的。 代码多云在数值上解决了所有这些，以预测频谱。 比较了这些预测，即观察到推断恒星或星系的性质。 多云是天体物理学中使用的最广泛使用的理论代码之一，每年引用了300多篇论文。Cloudy长期以来使用可用的计算机和原子数据解决了这些问题。 随着计算机变得更强大，原子数据更准确，可以改进模拟。 我们正在开发技术来改善黑洞附近发现的密集气体建模或爆炸恒星。 对“ Rydberg水平”的完整处理是离子周围电子的高度激发轨道，是关键的改进。 由于多云的广泛社区使用，这项工作将超出该项目的影响。该奖项反映了NSF的法定任务，并被认为是值得通过基金会的知识分子优点和更广泛影响的评论标准来评估的。

项目成果

Space Telescope and Optical Reverberation Mapping Project. XI. Disk-wind Characteristics and Contributions to the Very Broad Emission Lines of NGC 5548

• DOI: 10.3847/1538-4357/ab9cb2
• 发表时间: 2020-06
• 期刊: The Astrophysical Journal
• 作者: M. Dehghanian;G. Ferland;G. Kriss;B. Peterson;K. Korista;M. Goad;M. Chatzikos;F. Guzmán;G. D. Rosa;M. Mehdipour;J. Kaastra;S. Mathur;M. Vestergaard;D. Proga;T. Waters;M. Bentz;S. Bisogni;W. Brandt;E. Bontà;M. Fausnaugh;J. Gelbord;K. Horne;I. McHardy;R. Pogge;D. Starkey

Current and future development of the photoionization code Cloudy

光电离码的当前和未来发展 Cloudy

• DOI: 10.31577/caosp.2020.50.1.32
• 发表时间: 2020
• 期刊: Contributions of the Astronomical Observatory Skalnaté Pleso
• 作者: vanHoof, P.A.M.;VandeSteene, G.C.;Guzmán, F.;Dehghanian, M.;Chatzikos, M.;Ferland, G.J.
• 通讯作者: Ferland, G.J.

Challenges and Techniques for Simulating Line Emission

• DOI: 10.3390/galaxies6040100
• 发表时间: 2018-08
• 期刊: Galaxies
• 影响因子: 2.5
• 作者: K. Olsen;A. Pallottini;A. Wofford;Marios Chatzikos;Mitchell Revalski;F. Guzm'an;G. Popping;E. V'azquez-Semadeni;G. Magdis;M. Richardson;M. Hirschmann;W. Gray

Deciphering the 3D Orion Nebula. III. Structure on the NE Boundary of the Orion-S Embedded Molecular Cloud

破译 3D 猎户座星云。

• DOI: 10.3847/1538-4357/abd856
• 发表时间: 2021
• 期刊: The Astrophysical Journal
• 作者: O’Dell, C. R.;Abel, N. P.;Ferland, G. J.
• 通讯作者: Ferland, G. J.

Excitation mechanisms in the intracluster filaments surrounding brightest cluster galaxies

最亮星团星系周围星团内细丝的激发机制

• DOI: 10.1051/0004-6361/202039730
• 发表时间: 2021
• 期刊: Astronomy & Astrophysics
• 影响因子: 6.5
• 作者: Polles, F. L.;Salomé, P.;Guillard, P.;Godard, B.;Pineau des Forêts, G.;Olivares, V.;Beckmann, R. S.;Canning, R. E.;Combes, F.;Dubois, Y.
• 通讯作者: Dubois, Y.