We present new results on the structure of the solar core, obtained with new sets of frequencies of solar low-degree p modes obtained from the BiSON network. We find that different methods used in extracting the different sets of frequencies cause shifts in frequencies, but the shifts are not large enough to affect solar structure results. We find that the BiSON frequencies show that the solar sound speed in the core is slightly larger than that inferred from data from MDI low-degree modes, and the uncertainties on the inversion results are smaller. Density results also change by a larger amount, and we find that solar models now tend to show smaller differences in density compared to the Sun. The result is seen at all radii, a result of the fact that conservation of mass implies that density differences in one region have to cancel out density differences in others, since our models are constructed to have the same mass as the Sun. The uncertainties on the density results are much smaller too. We attribute the change in results to having more, and lower frequency, low-degree mode frequencies available. These modes provide greater sensitivity to conditions in the core.
Impact of rotation on the amplitude of acoustic modes in solar-like stars: Insights from hydrodynamical simulations
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心、天体物理学与分子相互作用研究所）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University（西北大学跨学科天文探索与研究中心）
The Celestial Sign in the Anglo-Saxon Chronicle in the 770s: Insights on Contemporary Solar Activity
774/775年的异常放射性碳浓度引起了人们对其起源的激烈讨论，包括可能的极端太阳事件，超过了观测历史上的任何事件。由于预见到这种极端的太阳事件，历史文献中也对极光记录进行了调查，包括盎格鲁-撒克逊编年史（ASC）中日落后的红色天体标志在内的极光记录也受到了考虑。Usoskin等人（2013：U13）将这一记录解释为极光，并建议在774/775附近增强太阳活动。与此相反，诺伊豪泽和诺伊豪泽（Neuhauser，2015 b：N15 a and N15 b）将“日落后”解释为日落或黄昏时;他们认为这是一个光环显示，并建议太阳极小期在774年左右。然而，到目前为止，这些记录还没有与已知极端空间天气事件期间目击者的极光记录进行比较，尽管它们与774/775年潜在极端事件的关系进行了讨论。因此，我们重建的观测细节的基础上的原始记录在ASC和文献参考，比较它们与目击者极光观测在已知的极端空间天气事件，并考虑当代太阳活动。我们澄清观察确实是“日落之后”，拒绝日晕假设，定义观察时间跨度为775年3月25日至777年12月25日，并注意到N15 b所示ASC中806处的平行晕绘制不是基于英国的原始观测。我们展示了在已知的空间天气事件中，在黄昏期间目击极光观测的例子，这个天体标志并不与观测证据相矛盾。因此，我们认为这一事件发生在774/775年事件开始之后，但显示出相对增强的太阳活动，其他历史极光记…
Velocity-space turbulent cascade in the near-Sun solar wind: first insights from the Parker Solar Probe mission
University of California, Berkeley（加州大学伯克利分校）；Space Sciences Laboratory, University of California, Berkeley（加州大学伯克利分校空间科学实验室）；KTH Royal Institute of Technology（瑞典皇家理工学院）；European Space Agency (ESA), European Space Astronomy Centre (ESAC)（欧洲航天局（ESA）欧洲空间天文中心）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；Laboratory of Atmospheric and Space Physics, University of Colorado, Boulder（科罗拉多大学博尔德校区大气与空间物理实验室）；Dipartimento di Fisica, Universita` della Calabria（卡塔尼亚大学物理系）
Chromospheric Flashes in a Solar Pore: Insights from Multi-line Spectropolarimetric Diagnostics
Physical Research Laboratory（物理研究实验室）；Udaipur Solar Observatory, Physical Research Laboratory（乌代浦尔太阳观测台，物理研究实验室）；Indian Institute of Technology, Gandhinagar（甘地纳加尔印度理工学院）；National Solar Observatory (NSO)（国家太阳天文台）；Laboratory for Atmospheric and Space Physics, University of Colorado（科罗拉多大学大气与空间物理实验室）；Instituto de Astrofı́sica de Canarias (IAC)（加那利群岛天体物理学研究所）；Universidad de La Laguna（拉古纳大学）
Statistical insights on the decorrelation lengths of solar wind parameters at L1 point under varying conditions
Department of Physics and Astronomy, Iowa City（爱荷华大学物理与天文学系）；Dept. of Physics, Assam（阿萨姆大学物理系）；Centre for Atmospheric Studies, Assam（阿萨姆大气研究中心）；Physical Research Laboratory, Ahmedabad（艾哈迈达巴德物理研究所）；Indian Institute of Technology (IIT), Gandhinagar（甘地纳加尔印度理工学院）
Coronal Mass Ejections from Young Suns: Insights from Solar and Stellar Observations and Models
NASA Goddard Space Flight Center（NASA戈达德太空飞行中心）；The Catholic University of America（美国天主教大学）；The Hakubi Center for Advanced Research, Kyoto University（京都大学Hakubi高级研究中心）；Department of Physics, Kyoto University（京都大学物理系）
Nature of Transonic Sub-Alfvénic Turbulence and Density Fluctuations in the Near-Sun Solar Wind: Insights from Magnetohydrodynamic Simulations and Nearly-Incompressible Models
University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；University of Alabama in Huntsville（阿拉巴马大学亨茨维尔分校）；Center for Space Plasma and Aeronomic Research (CSPAR)（空间等离子体与航空研究发展中心）
What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
MMS Insights into CME Driven Sub-Alfvénic Solar Wind at 1 AU
University of Maryland（马里兰大学）；NASA Goddard Space Flight Center（NASA戈达德太空飞行中心）；University of New Hampshire（新罕布什尔大学）；University of Delaware（特拉华大学）；University of Colorado Boulder（科罗拉多大学博尔德分校）
