摘要

The first stars to form in the universe may have had very different properties from later generations of stars. They were uniquely made from just primordial gas and also their formation process and characteristic masses may have been quite different.  No direct observations of these star are possible at this time, however, so our ability to study these early stars is limited to indirect measurements and numerical simulations.  For example, stellar forensics based on nucleosynthesis patterns preserved in subsequent generations of stars may be used in an attempt to reconstruct the properties of the first stars.

The overarching big questions are: What are the typical masses of this first generation of stars?  What is the initial mass function?  And how did these stars live and die? These will determine how the universe transitioned from the first stars to the formation of the first galaxies, and what observations of them may be possible in the future.

Early simulation of formation of the first stars and simple theoretical arguments suggested the these stars may have been quite massive, possibly massive enough to explode as pair instability supernovae.  Interestingly, there is an increasing number of observations suggesting that even in the present universe very massive stars form and live to explode as powerful pair instability supernovae.  But is this also the outcome we should generally expect for the majority of the first stars and is it supported by observations of the "ashes" of the first stars? This talk will review the recent progress in seeking answers to these questions.

报告人简介

Alexander works in the School of Mathematical Sciences at Monash University as a Professor.

Alexander’s research areas of interest are:

• Life and explosive death of massive stars
• The origin of the elements
• Nuclear astrophysics

Current work comprises the study of massive to supermassive stars (10-100,000 solar masses); the first generations of stars in the universe (Pop III stars); evolution of rotating massive stars and the spin of their remnants; mixing and transport processes in the stellar interior; nucleosynthesis and the origin of elements, including galacto-chemical evolution - which elements are made where and when; supernovae (mechanisms and nucleosynthesis); gamma-ray bursts (collapsars and similar models) and their progenitors; modeling of Type I X-ray bursts and superbursts (thermonuclear explosions on the surface of neutron stars).