共生复发新星（RNe）的吸积率的估计往往达不到理论预期的数量级。如果白矮星（WD）的质量积累是高度分散的，并且大多数观测都是在低状态下进行的，那么这种明显的差异就可以解决。在这里，我们使用的档案数据的重新分析，从数字访问天空世纪@哈佛大学（DASCH）调查认为，最近的新星喷发共生RN T CrB，在1946年，发生在-因此触发-一个短暂的吸积高状态。基于相似的光学光变曲线在1946年左右的前一次喷发的时间，在1866年，我们认为WD在T CrB积累的大部分燃料需要点燃热核失控（TNR）在吸积高状态。这种状态的一个自然起源是类似于矮新星的吸积盘不稳定性，这是在共生双星中可能存在的大圆盘中预期的。因此，共生RNe中TNR的时间可以由它们的吸积盘的稳定性来决定。T CrB正处于吸积的高状态，就像我们在过去两次新星爆发中看到的那样。结合TNR发生时间的临近，基于前两颗新星（$2026 \pm$ 3）之间80年的间隔，目前的吸积高状态增加了未来几年TNR发生在T CrB的可能性。
英文摘要：
Estimates of the accretion rate in symbiotic recurrent novae (RNe) often fall short of theoretical expectations by orders of magnitude. This apparent discrepancy can be resolved if the accumulation of mass by the white dwarf (WD) is highly sporadic, and most observations are performed during low states. Here we use a reanalysis of archival data from the Digital Access to a Sky Century @Harvard (DASCH) survey to argue that the most recent nova eruption in symbiotic RN T CrB, in 1946, occurred during -- and was therefore triggered by -- a transient accretion high state. Based on similarities in the optical light curve around 1946 and the time of the prior eruption, in 1866, we suggest that the WD in T CrB accumulates most of the fuel needed to ignite the thermonuclear runaways (TNRs) during accretion high states. A natural origin for such states is dwarf-nova like accretion-disk instabilities, which are expected in the presumably large disks in symbiotic binaries. The timing of the TNRs in symbiotic RNe could thus be set by the stability properties of their accretion disks. T CrB is in the midst of an accretion high state like the ones we posit led to the past two nova eruptions. Combined with the approach of the time at which a TNR would be expected based on the 80-year interval between the prior two novae ($2026 \pm$3), the current accretion high state increases the likelihood of a TNR occurring in T CrB in the next few years.
The First Multi-Messenger Nova: External Shocks, TeV Photons, and Neutrinos in the Next Eruption of T CrB
Texas Tech University（德克萨斯理工大学）；Michigan State University（密歇根州立大学）；Naval Research Laboratory（海军研究实验室）；INAF-Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；National Radio Astronomy Observatory（美国国家射电天文台）；Columbia University（哥伦比亚大学）；Flatiron Institute（平顶山研究所）；University of Virginia（弗吉尼亚大学）；NASA/GSFC（美国宇航局戈达德太空飞行中心）；University of Maryland, Baltimore County（马里兰大学巴尔的摩县分校）；University of California, Berkeley（加州大学伯克利分校）
The B & V Light Curves for Recurrent Nova T CrB From 1842--2022, the Unique Pre- and Post-Eruption High-States, the Complex Period Changes, and the Upcoming Eruption in 2025.5$\pm$1.3
Pre-nova Observations of T CrB: A view from the CHARA Array
New Mexico Institute of Mining and Technology（新墨西哥矿业与技术学院）；The CHARA Array of Georgia State University（佐治亚州立大学CHARA阵列）；Mount Wilson Observatory（威尔逊山天文台）；Department of Astronomy and Astrophysics, The Pennsylvania State University（宾夕法尼亚州立大学天文学与天体物理学系）；Astronomical Observatory Institute, Faculty of Physics and Astronomy, Adam Mickiewicz University（亚当·密茨凯维奇大学物理与天文学院天文台研究所）
利用 CHARA 阵列的 MIRC-X 和 MYSTIC 干涉测量，精确测定了共生再发新星 T CrB 红巨星的前新星角直径和半径，支持其充满洛希瓣。
Evolution of the recent high-accretion state of the recurrent nova T CrB: HST, Swift, NuSTAR, and XMM-Newton observations
Universidad Nacional de Hurlingham (UNAHUR)（乌尔沙姆国立大学）；Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET)（国家科学技术研究委员会）；Mullard Space Science Laboratory, University College London（伦敦大学学院穆拉德太空科学实验室）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Maryland, Baltimore County（马里兰大学巴尔的摩县分校）；Columbia University（哥伦比亚大学）；School of Physics and Astronomy, University of Leicester（莱斯特大学物理与天文学学院）
Hydrodynamic simulations of the recurrent nova T Coronae Borealis: Nucleosynthesis predictions
Universitat Politècnica de Catalunya (UPC)（加泰罗尼亚理工大学）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究研究所）；Institut de Ciències de l’Espai (ICE-CSIC)（空间科学研究所）
The accretion-driven eruption of the recurrent nova T Corona Borealis
Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学）；Instituto Nacional de Pesquisas Espaciais - INPE（国家空间研究所）；Universidade Estadual de Maringá - UEM（马林加州立大学）；Universidad Nacional de Hurlingham (UNAHUR)（乌尔希纳姆国立大学）；Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET)（国家科学研究委员会）
The quiescent states of V745 Sco and V3890 Sgr: VLT/X-shooter and Swift/XRT+UVOT observations
Faculty of Mathematics and Physics, University of Ljubljana（卢布尔雅那大学数学与物理学院）；INAF National Institute of Astrophysics, Astronomical Observatory of Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所天文与空间科学观测站）；Instituto de Astrofisica, Depto. de Ciencias Fisicas, Facultad de Ciencias Exactas, Universidad Andres Bello（安德烈斯贝略大学精确科学学院物理科学系天体物理研究所）
Multi-wavelength study of the pre-eruption dip in the recurrent nova T Coronae Borealis preceding imminent nova eruption
Liupanshui Normal University（六盘水师范学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；Qiannan Normal University for Nationalities（黔南民族师范学院）
Dissecting a disk-instability outburst in a symbiotic star: $NuSTAR$, and $Swift$ observations of T Coronae Borealis during the rise to the "super-active" state
