POSYDON: A General-Purpose Population Synthesis Code with Detailed Binary-Evolution Simulations
Tassos Fragos, Jeff J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konst… 展开作者
Tassos Fragos, Jeff J. Andrews, Simone S. Bavera, Christopher P. L. Berry, Scott Coughlin, Aaron Dotter, Prabin Giri, Vicky Kalogera, Aggelos Katsaggelos, Konstantinos Kovlakas, Shamal Lalvani, Devina Misra, Philipp M. Srivastava, Ying Qin, Kyle A. Rocha, Jaime Roman-Garza, Juan Gabriel Serra, Petter Stahle, Meng Sun, Xu Teng, Goce Trajcevski, Nam Hai Tran, Zepei Xing, Emmanouil Zapartas, Michael Zevin
备注：
60 pages, 33 figures, 8 tables, referee's comments addressed. The code and the accompanying documentations and data products are available at https:\\posydon.org
Most massive stars are members of a binary or a higher-order stellar systems, where the presence of a binary companion can decisively alter their evolution via binary interactions. Interacting binaries are also important astrophysical laboratories for the study of compact objects. Binary population synthesis studies have been used extensively over the last two decades to interpret observations of compact-object binaries and to decipher the physical processes that lead to their formation. Here, we present POSYDON, a novel, binary population synthesis code that incorporates full stellar-structure and binary-evolution modeling, using the MESA code, throughout the whole evolution of the binaries. The use of POSYDON enables the self-consistent treatment of physical processes in stellar and binary evolution, including: realistic mass-transfer calculations and assessment of stability, internal angular-momentum transport and tides, stellar core sizes, mass-transfer rates and orbital periods. This paper describes the detailed methodology and implementation of POSYDON, including the assumed physics of stellar- and binary-evolution, the extensive grids of detailed single- and binary-star models, the post-processing, classification and interpolation methods we developed for use with the grids, and the treatment of evolutionary phases that are not based on pre-calculated grids. The first version of POSYDON targets binaries with massive primary stars (potential progenitors of neutron stars or black holes) at solar metallicity.
Stellar Population Spectra Incorporating Detailed Binary Evolution using POSYDON
University of Florida（佛罗里达大学）；Institute for Fundamental Theory（基础理论研究所）；University of Arkansas（阿肯色大学）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；National and Kapodistrian University of Athens（雅典国立卡波季斯特里亚斯大学）；Foundation for Research and Technology – Hellas（希腊研究与技术基金会）；University of Crete（克里特大学）；Université de Genève（日内瓦大学）
Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)（天体物理学跨学科探索与研究中心（CIERA））；University of Florida（佛罗里达大学）；University of Glasgow（格拉斯哥大学）；Northwestern University（西北大学）；KU Leuven（鲁汶大学）
Binary stars undergo a variety of interactions and evolutionary phases, critical for predicting and explaining observed properties. Binary population synthesis with full stellar-structure and evolution simulations are computationally expensive requiring a large number of mass-transfer sequences. The recently developed binary population synthesis code POSYDON incorporates grids of MESA binary star simulations which are then interpolated to model large-scale populations of massive binaries. The traditional method of computing a high-density rectilinear grid of simulations is not scalable for hig…
The Demographics of Binary Companions to Stripped-Envelope Supernovae: Confronting Observations with Population Synthesis
Foundation for Research and Technology（研究与技术基金会）；Space Telescope Science Institute（太空望远镜科学研究所）；University of Toronto（多伦多大学）；Carnegie Institution for Science（卡内基科学促进会）；Northwestern University（西北大学）；Caltech/IPAC（加州理工学院/IPAC）；University of Washington（华盛顿大学）
When the stars don't align: Investigating inconsistencies in binary black hole formation across population synthesis codes
The University of Chicago（芝加哥大学）；Adler Planetarium（阿德勒天文馆）；Northwestern University（西北大学）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）；Carnegie Mellon University（卡内基梅隆大学）；Université de Genève（日内瓦大学）
Emulators for stellar profiles in binary population modeling
Northwestern University（西北大学）；Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University（西北大学跨学科天体物理探索与研究中心）；NSF-Simons AI Institute for the Sky (SkAI)（NSF-西蒙斯天空人工智能研究所）；Department of Electrical and Computer Engineering, Northwestern University（西北大学电气与计算机工程系）；University of Florida（佛罗里达大学）；Institute for Fundamental Theory（基础理论研究所）；Gravitational Wave Science Center (GWSC), Université de Genève（日内瓦大学引力波科学中心）；Institute of Space Sciences (ICE), CSIC, Campus UAB（西班牙国家研究委员会空间科学研究所（加泰罗尼亚理工大学校区））；Institute of Astrophysics, Foundation for Research and Technology（希腊研究与技术基金会天体物理研究所）
The power of binaries on stripped-envelope supernovae across metallicity: uniform progenitor parameter space and persistently low ejecta masses, but subtype diversity
The Mass-Ratio Distribution of the Low-Mass Binary Black Hole Subpopulation: A Natural Outcome of Isolated Binary Evolution
Harvard Society of Fellows（哈佛学会）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心 | 哈佛与史密森尼学会）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)（天体物理学跨学科探索与研究中心）；Department of Physics and Astronomy, Northwestern University（西北大学物理与天文系）；Département d’Astronomie, Université de Genève（日内瓦大学天文学系）；Gravitational Wave Science Center (GWSC), Université de Genève（日内瓦大学引力波科学中心）；The Adler Planetarium（阿德勒天文馆）
X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations
Double Neutron Star Delay Times Across Cosmic Metallicities: The Role of Helium Star Progenitors
University of Florida（佛罗里达大学）；Institute for Fundamental Theory（基础理论研究所）；Université de Genève（日内瓦大学）；Gravitational Wave Science Center (GWSC)（引力波科学中心）；Northwestern University（西北大学）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)（天体物理学跨学科探索与研究中心）
From the Milky Way to the Early Universe: How Metallicity Shapes the Formation of Double Neutron Stars
University of Florida（佛罗里达大学）；Harvard Society of Fellows（哈佛学会）；Center for Astrophysics | Harvard & Smithsonian（天体物理中心（哈佛大学与史密森尼学会））；Université de Genève（日内瓦大学）；The Adler Planetarium（阿德勒天文馆）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)（天体物理学跨学科探索与研究中心）
