驱动核心坍缩超新星（CCSNe）的物理机制的细节仍然不确定。虽然在2D中详细的CCSN机制模拟的定性结果上正在形成共识，但直到最近才有高保真度3D模拟成为可能。在这里，我们提出了一个广泛的3D CCSN模拟使用高保真度多维中微子输运，高分辨率流体力学和近似的广义相对论引力的结果。我们采用了最先进的20太阳质量的祖先，使用恒星天体物理学实验模块（MESA; Farmer et al.（2016）Paxton et al.（2011，2013，2015，2018）和Steiner et al.（2013）的SFHo状态方程。虽然我们的3D CCSN模拟没有在核心反弹后约500 ms内爆炸，但我们发现，在坍塌的铁芯周围的Si和O壳中存在大规模非球面运动有助于冲击波膨胀，并使模型更接近爆炸阈值。我们还发现一些依赖于分辨率和几何形状（八分圆与全4 $π$）。正如在最近的其他工作中所指出的那样，我们发现激波后湍流在确定我们模拟的整体动力学演化中起着重要作用。我们发现一个强大的常设吸积激波不稳定性（SASI），在冲击衰退时期的后期发展。SASI有助于瞬态激波扩展阶段，但不足以导致激波复活。我们还报告说，对于我们的模拟的一个子集，我们发现了Tamborra等人（2014）首次报道的LESA的确凿证据，但到目前为止，尚未得到其他模拟代码的证实。无论是祖非球面性和SASI引起的瞬态冲击膨胀阶段产生瞬态引力波和中微子信号调制通过扰动的质子中子星的湍流运动。（节略）
英文摘要：
The details of the physical mechanism that drives core-collapse supernovae (CCSNe) remain uncertain. While there is an emerging consensus on the qualitative outcome of detailed CCSN mechanism simulations in 2D, only recently have high-fidelity 3D simulations become possible. Here we present the results of an extensive set of 3D CCSN simulations using high-fidelity multidimensional neutrino transport, high-resolution hydrodynamics, and approximate general relativistic gravity. We employ a state-of-the-art 20 solar mass progenitor generated using the Modules for Experiments in Stellar Astrophysics (MESA; Farmer et al. (2016) Paxton et al. (2011, 2013, 2015, 2018) and the SFHo equation of state of Steiner et al. (2013). While none of our 3D CCSN simulations explode within ~500ms after core bounce, we find that the presence of large scale aspherical motion in the Si and O shells surrounding the collapsing iron core aid shock expansion and bring the models closer to the threshold of explosion. We also find some dependence on resolution and geometry (octant vs. full 4$π$). As has been noted in other recent works, we find that the post-shock turbulence plays an important role in determining the overall dynamical evolution of our simulations. We find a strong standing accretion shock instability (SASI) that develops at late times during the shock recession epoch. The SASI aids in transient shock expansion phases, but is not enough to result in shock revival. We also report that for a subset of our simulations, we find conclusive evidence for the LESA first reported in Tamborra et al. (2014), but until now, not confirmed by other simulation codes. Both the progenitor asphericities and the SASI-induced transient shock expansion phases generate transient gravitational waves and neutrino signal modulations via perturbations of the protoneutron star by turbulent motions. (abridged)
SN 2023gpw: exploring the diversity and power sources of hydrogen-rich superluminous supernovae
University of Turku（图尔库大学）；Aalto University（阿尔托大学）；California Institute of Technology（加州理工学院）；Aarhus University（奥胡斯大学）；Northwestern University（西北大学）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Liverpool John Moores University（利物浦约翰摩尔斯大学）；Stockholm University（斯德哥尔摩大学）；Trinity College Dublin, The University of Dublin（都柏林三一学院，都柏林大学）；Universidad Arturo Prat（阿图罗·普拉特大学）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究研究所（IEEC））；University of Warwick（华威大学）
SN 2023gpw是一颗富含氢的超亮超新星，其高辐射能量和缺乏整体减速表明可能有额外能量来源，如中心引擎或黑洞吸积。
Exploring the origins of high-velocity features in SNe Ia with the spectral synthesis code TARDIS
Trinity College Dublin（都柏林三一学院）；Heidelberg Institute for Theoretical Studies（海德堡理论研究所）；European Southern Observatory（欧洲南方天文台）；Millennium Institute of Astrophysics MAS（天体物理千年研究所）；National Central University（中央大学）；Institute of Space Sciences (ICE-CSIC)（空间科学研究所）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究研究所）；CENTRA, Instituto Superior Técnico, Universidade de Lisboa（里斯本大学高级技术学院中心天体物理学和天文学研究中心）；University of Warsaw（华沙大学）；Instituto de Alta Investigación, Universidad de Tarapacá（塔拉帕卡大学高等研究所）
