Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski and Maxim Markevitch
{"title":"论英仙座星系团中古老的大规模冷锋的起源","authors":"Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski and Maxim Markevitch","doi":"10.3847/1538-4357/ad6e83","DOIUrl":null,"url":null,"abstract":"The intracluster medium of the Perseus Cluster exhibits spiral-shaped X-ray surface brightness discontinuities known as “cold fronts,” which simulations indicate are caused by the sloshing motion of the gas after the passage of a subcluster. Recent observations of Perseus have shown that these fronts extend to large radii. In this work, we present simulations of the formation of sloshing cold fronts in Perseus using the AREPO magnetohydrodynamics code, to produce a plausible scenario for the formation of the large front at a radius of 700 kpc. Our simulations explore a range of subcluster masses and impact parameters. We find that low-mass subclusters cannot generate a cold front that can propagate to such a large radius, and that small impact parameters create too much turbulence, which leads to the disruption of the cold front before it reaches such a large distance. Subclusters that make only one core passage produce a stable initial front that expands to large radii, but without a second core passage of the subcluster, other fronts are not created at a later time in the core region. We find a small range of simulations with subclusters with mass ratios of R ∼ 1:5 and an initial impact parameter of θ ∼ 20°–25° that not only produce the large cold front but a second set in the core region at later times. These simulations indicate that the “ancient” cold front is ∼6–8.5 Gyr old. For the simulations providing the closest match with observations, the subcluster has completely merged into the main cluster.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":null,"pages":null},"PeriodicalIF":0.0000,"publicationDate":"2024-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies\",\"authors\":\"Elena Bellomi, John A. ZuHone, Rainer Weinberger, Stephen A. Walker, Irina Zhuravleva, Mateusz Ruszkowski and Maxim Markevitch\",\"doi\":\"10.3847/1538-4357/ad6e83\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The intracluster medium of the Perseus Cluster exhibits spiral-shaped X-ray surface brightness discontinuities known as “cold fronts,” which simulations indicate are caused by the sloshing motion of the gas after the passage of a subcluster. Recent observations of Perseus have shown that these fronts extend to large radii. In this work, we present simulations of the formation of sloshing cold fronts in Perseus using the AREPO magnetohydrodynamics code, to produce a plausible scenario for the formation of the large front at a radius of 700 kpc. Our simulations explore a range of subcluster masses and impact parameters. We find that low-mass subclusters cannot generate a cold front that can propagate to such a large radius, and that small impact parameters create too much turbulence, which leads to the disruption of the cold front before it reaches such a large distance. Subclusters that make only one core passage produce a stable initial front that expands to large radii, but without a second core passage of the subcluster, other fronts are not created at a later time in the core region. We find a small range of simulations with subclusters with mass ratios of R ∼ 1:5 and an initial impact parameter of θ ∼ 20°–25° that not only produce the large cold front but a second set in the core region at later times. These simulations indicate that the “ancient” cold front is ∼6–8.5 Gyr old. For the simulations providing the closest match with observations, the subcluster has completely merged into the main cluster.\",\"PeriodicalId\":501813,\"journal\":{\"name\":\"The Astrophysical Journal\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2024-10-14\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The Astrophysical Journal\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.3847/1538-4357/ad6e83\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The Astrophysical Journal","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/1538-4357/ad6e83","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
摘要
英仙座星团的星团内介质呈现出螺旋形的 X 射线表面亮度不连续现象,这种现象被称为 "冷锋",模拟结果表明它是由子星团通过后气体的滑动运动引起的。最近对英仙座的观测表明,这些冷锋的半径很大。在这项工作中,我们使用 AREPO 磁流体力学代码模拟了英仙座中荡漾冷锋的形成,为半径为 700 kpc 的大锋面的形成提出了一个合理的方案。我们的模拟探索了一系列亚星团质量和撞击参数。我们发现,低质量的亚星团无法产生能够传播到如此大半径的冷锋,而小的撞击参数会产生过多的湍流,导致冷锋在到达如此大的距离之前就被破坏。只通过一次核心的子团会产生一个稳定的初始锋面,并扩展到较大的半径,但如果没有子团的第二次核心通过,就不会在以后的核心区域产生其他锋面。我们发现在质量比为 R ∼ 1:5 和初始撞击参数为 θ ∼ 20°-25°的亚星团的小范围模拟中,不仅产生了大的冷锋,而且在后来的时间里在核心区域产生了第二组冷锋。这些模拟结果表明,"古老的 "冷锋的年龄为 ∼6-8.5 Gyr。在与观测结果最接近的模拟中,子星团完全并入了主星团。
On the Origin of the Ancient, Large-scale Cold Front in the Perseus Cluster of Galaxies
The intracluster medium of the Perseus Cluster exhibits spiral-shaped X-ray surface brightness discontinuities known as “cold fronts,” which simulations indicate are caused by the sloshing motion of the gas after the passage of a subcluster. Recent observations of Perseus have shown that these fronts extend to large radii. In this work, we present simulations of the formation of sloshing cold fronts in Perseus using the AREPO magnetohydrodynamics code, to produce a plausible scenario for the formation of the large front at a radius of 700 kpc. Our simulations explore a range of subcluster masses and impact parameters. We find that low-mass subclusters cannot generate a cold front that can propagate to such a large radius, and that small impact parameters create too much turbulence, which leads to the disruption of the cold front before it reaches such a large distance. Subclusters that make only one core passage produce a stable initial front that expands to large radii, but without a second core passage of the subcluster, other fronts are not created at a later time in the core region. We find a small range of simulations with subclusters with mass ratios of R ∼ 1:5 and an initial impact parameter of θ ∼ 20°–25° that not only produce the large cold front but a second set in the core region at later times. These simulations indicate that the “ancient” cold front is ∼6–8.5 Gyr old. For the simulations providing the closest match with observations, the subcluster has completely merged into the main cluster.