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Massive stars play an important role in many astrophysical systems by providing the radiative and mechanical energy output. They can also produce black holes and neutron stars when they explode. However, the traditional 1D stellar evolution models provide very uncertain predictions for the structure and evolution of massive stars because radiation acceleration around the envelopes of massive stars at the iron opacity regions can be much larger than the gravitational acceleration. I will show how we can understand convection in massive star envelopes and observational properties of massive stars in different locations of the HR diagram based on a series of first principle global 3D radiation hydrodynamic simulations. These simulations can be used to understand the physical origin of super-Eddington outflows from massive stars and the outburst behavior of luminous blue variables. I will demonstrate these simulations can directly produce the low frequency variabilities of many O stars as observed by TESS recently. I will also show simulations of Red Supergiants, which are used to predict observational properties of supernova shock breakouts. Finally, I will illustrate how these simulation results can be used to improve the traditional 1D binary evolution models.
Yan-Fei Jiang joined the Center for Computational of Astrophysics, Flatiron Institute as an associate research scientist in September 2019. He earned his Ph.D. in astrophysical sciences from Princeton University and his B.S. in physics from Tsinghua University. Jiang is the recipient of the 2013 ITC Fellowship and the Einstein Fellowship. He also won the 2012 Ray Grimm Memorial Prize in Computational Physics. Prior to joining CCA, he was a KITP Fellow at the Kavli Institute.
Location: N602（TDLI）
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