We present results of two-hour non-interrupted observations of solar granulation obtained under excellent seeing conditions with the largest aperture ground-based solar telescope - the New Solar Telescope (NST) - of Big Bear Solar Observatory. Observations were performed with adaptive optics correction using a broad-band TiO filter in the 705.7 nm spectral line with a time cadence of 10 s and a pixel size of 0.0375". Photospheric bright points (BPs) were detected and tracked. We find that the BPs detected in NST images are co-spatial with those visible in Hinode/SOT G-band images. In cases where Hinode/SOT detects one large BP, NST detects several separated BPs. Extended filigree features are clearly fragmented into separate BPs in NST images. The distribution function of BP sizes extends to the diffraction limit of NST (77 km) without saturation and corresponds to a log-normal distribution. The lifetime distribution function follows a log-normal approximation for all BPs with lifetime exceeding 100 s. A majority of BPs are transient events reflecting the strong dynamics of the quiet sun: 98.6% of BPs live less than 120 s. The longest registered life time was 44 minutes. The size and maximum intensity of BPs were found to be proportional to their life times.
Investigation of Umbral Dots with the New Vacuum Solar Telescope
本影点（UDs）是在太阳黑子本影中观测到的孤立的小亮斑。它们是存在于本影内部的对流现象。根据UDs在本影中的位置，通常将其分为中心UDs（CUDs）和外围UDs（PUDs）。我们的目的是研究UD的性质，分析它们之间的关系，并进一步发现这些性质是否依赖于本影磁场强度。因此，我们选择了中国云南天文台富县太阳天文台的\textit{New Vacuum Solar Telescope}在最佳视宁条件下拍摄的四个活动区（AR）的高分辨率TiO图像。四个AR（NOAA 11598、11801、12158和12178）包含六个太阳黑子。共确定了1220个CUD和603个PUD。同时，利用\textit{Solar Dynamics Observatory}上的\textit{Helioseismic and Magnetic Imager}拍摄的太阳黑子矢量磁场的径向分量，分析了UD特性与本影磁场强度之间的关系。我们发现，直径和寿命的UD表现出增加的趋势与亮度，但速度不。此外，直径、强度、寿命和速度取决于周围的磁场。CUD的直径被发现更大，CUD更明亮，它的寿命更长，它的运动在弱的阴影磁场环境中比在一个强的慢。
Goldstone Apple Valley Radio Telescope Observations of 2012 Solar Eclipse: A Multi-wavelength study of cm-wavelength Gyroresonance Emission from Active Regions
Accessing the fine temporal scale of EUV brightenings and their quasi-periodic pulsations: 1 second cadence observations by Solar Orbiter/EUI
Solar-Terrestrial Centre of Excellence – SIDC, Royal Observatory of Belgium（太阳-地球卓越中心–SIDC，比利时皇家天文台）；Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven（荷语鲁汶大学数学系数学等离子体天体物理学中心）；Astronomy & Astrophysics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, DIAS Dunsink Observatory（都柏林高等研究院宇宙物理学院天文学与天体物理系，DIAS邓辛克天文台）；ETH-Zurich（苏黎世联邦理工学院）；Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center（达沃斯物理气象观测站，世界辐射中心）
Red Giant Branch Bump Brightness and Number Counts in 72 Galactic Globular Clusters Observed with the Hubble Space Telescope
我们提出了最广泛和最精确的红巨星分支凸块（RGBB）的亮度和数量计数进行了实证调查。我们实现了一种新的方法，并使用来自两个\textit{Hubble Space Telescope (HST)}球状星团（GC）调查的数据来测量72个GC中RGBB的亮度和恒星计数。亮度测量精度优于0.01 mag，计数精度达到10%。在适当的情况下，主序星关闭（MSTO）的位置和水平分支（HB）星的数量被用作比较。几个独立的科学结论是新的可能与我们的参数化的RGBB。亮度和计数被证明有第二个参数，除了他们的强烈依赖于金属丰度。在GC NGC 2808、5286、6388和6441中发现RGBB异常，可能是由于存在多个种群。最后，我们使用我们的经验校准来预测的性质的星系核球RGBB，如果类似的恒星物理的核球和银河系GC系统的假设成立。的RGBB性质的凸起被证明是不同的银河系GC系统，与前者具有较低的数量计数，较低的亮度色散和更明亮的峰值亮度比预期从后者。这种差异很好地解释了银河系隆起有一个更高的氦丰度比预期的GC，$Δ$ Y $\sim +$ 0.06的金属丰度中位数。
Nancy Grace Roman Space Telescope Wide Field Instrument: Bright Point Source Saturation Response and Persistence Properties from Thermal-Vacuum Testing
Catholic University of America（天主教大学）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；University of Maryland, College Park（马里兰大学帕克分校）；ADNET Systems, Inc.（ADNET系统公司）；KBR（KBR公司）
