A precessing Be disk as a possible model for occultation events in GX 304-1
Matthias Kühnel, Richard E. Rothschild, Atsuo T. Okazaki, Sebastian Müller, Katja Pottschmidt, Ralf Ballhausen, Jieun Choi, Ingo Kreykenbohm, Felix Fürst, Diana… 展开作者
Matthias Kühnel, Richard E. Rothschild, Atsuo T. Okazaki, Sebastian Müller, Katja Pottschmidt, Ralf Ballhausen, Jieun Choi, Ingo Kreykenbohm, Felix Fürst, Diana M. Marcu-Cheatham, Paul Hemphill, Macarena Sagredo, Peter Kretschmar, Silvia Martínez-Núñez, José Miguel Torrejón, Rüdiger Staubert, Jörn Wilms
备注：
12 pages, 8 figures, 3 tables. Accepted for publication in the Monthly Notices of the Royal Astronomical Society
我们报告在2011年5月GX 304-1爆发期间，RXTE探测到吸收柱密度$N_\mathrm{H}$突然增加。$N_\mathrm{H}$增加到$^{-2}$中的${\sim}16\times 10^{22}$原子，这比RXTE报道的GX 304-1爆发期间通常测量的值大3-4倍。此外，在该时间范围内测量到从能量分辨RXTE-PCA光变曲线计算的硬度比的可变性的增加。我们将这些事实解释为中子星被视线中的物质掩星事件。使用一个简单的3D模型的倾斜和旋进盘周围的Be型同伴，我们能够定性地解释随着时间的推移，$N_\mathrm{H}$的演变。我们能够将Be盘密度限制在$10^{-11}$ g cm $^{-3}$的量级。我们的模型加强了倾斜的盘的双峰爆发的起源的想法作为派生的几何允许吸积两次，在一定条件下，每个轨道。
英文摘要：
We report on the RXTE detection of a sudden increase in the absorption column density, $N_\mathrm{H}$, during the 2011 May outburst of GX 304-1. The $N_\mathrm{H}$ increased up to ${\sim}16\times 10^{22}$ atoms cm$^{-2}$, which is a factor of 3-4 larger than what is usually measured during the outbursts of GX 304-1 as covered by RXTE. Additionally, an increase in the variability of the hardness ratio as calculated from the energy resolved RXTE-PCA light curves is measured during this time range. We interpret these facts as an occultation event of the neutron star by material in the line of sight. Using a simple 3D model of an inclined and precessing Be disk around the Be type companion, we are able to qualitatively explain the $N_\mathrm{H}$ evolution over time. We are able to constrain the Be-disk density to be on the order of $10^{-11}$ g cm$^{-3}$. Our model strengthens the idea of inclined Be disks as origin of double-peaked outbursts as the derived geometry allows accretion twice per orbit under certain conditions.
Diverse Emission Patterns from Precessing Super-Eddington Disks Formed in Tidal Disruption Events
The University of Hong Kong（香港大学）；The Hong Kong Institute for Astronomy and Astrophysics, The University of Hong Kong（香港大学香港天体物理研究所）；Shenzhen Institute of Research and Innovation, The University of Hong Kong（香港大学深圳研究院）
Even a precessing clock is right twice per orbit -- The super-periods of eRO-QPE2 and challenges for quasi-periodic eruption orbital models
Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所）；Black Hole Initiative at Harvard University（哈佛大学黑洞倡议）；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所/西班牙高等科学研究理事会天体生物学中心）；Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）；Department of Physics and Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学物理系及哥伦比亚天体物理学实验室）；Center for Cosmology and Particle Physics, Physics Department, New York University（纽约大学物理系宇宙学与粒子物理中心）；School of Natural Sciences, Institute for Advanced Study（高等研究院自然科学学院）；Università degli Studi di Milano-Bicocca（米兰比可卡大学）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所米兰比可卡分部）
A precessing jet from an active galactic nucleus drives gas outflow from a disk galaxy
University of California Irvine（加州大学尔湾分校）；California Institute of Technology（加州理工学院）；National Radio Astronomy Observatory（美国国家射电天文台）；University of Virginia（弗吉尼亚大学）；University of Arizona（亚利桑那大学）；European Southern Observatory（欧洲南方天文台）；Joint Atacama Large Millimeter Array Observatory（阿塔卡马大型毫米波/亚毫米波阵列联合观测站）；University of California Riverside（加州大学河滨分校）；University of Florida（佛罗里达大学）；Foundation for Research and Technology -Hellas（希腊研究与技术基金会）；European University Cyprus（塞浦路斯欧洲大学）；Flatiron Institute（平顿研究所）；University of California, Los Angeles（加州大学洛杉矶分校）；W. M. Keck Observatory（韦克天文台）；Carnegie Institution for Science（卡内基科学机构）；University of Toledo（托莱多大学）；Occidental College（西方学院）；University of California Santa Cruz（加州大学圣克鲁兹分校）；NPC Worldwide, LLC（NPC环球有限公司）；University of Crete（克里特大学）；Australian National University（澳大利亚国立大学）；Australian Research Council Centre of Excellence for All Sky Astrophysics in Three Dimensions（澳大利亚研究理事会三维全天空天体物理学卓越中心）；Hiroshima University（广岛大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Cahill Center for Astronomy and Astrophysics（凯尔天文学与天体物理学中心）；University of Hawaii at Manoa（夏威夷大学马诺阿分校）
