What is it about?
Neutron stars are thought to be formed during supernova explosions of massive stars. Neutron stars exhibit some peculiar features possibly affected by their environments. Some neutron stars emit non-thermal radiation with regular pulses known as pulsars. They are thought to rotate with periods of 0.01 s or less and have strong magnetic fields on their surface. Others emit black body radiations without pulsations. We discuss the motion of fallback matter left behind ejecta of supernova explosions using semi-analytic solutions and what determines the magnetic fields on the surface of neutron stars at the center of massive stars.
Featured Image
Why is it important?
Our solutions indicate that there was the critical accretion rate over which a neutron star cannot repel the fallback matter depending on the energy deposition rate from the neutron star. This gives some information on the fate of a newly formed neutron star depending on the surface magnetic field and the rotation period.
Perspectives
I hope that we can extend the argument in this work by performing multi-dimensional simulations to apply to real systems.
Dr. Toshikazu Shigeyama
University of Tokyo
Read the Original
This page is a summary of: Repulsion of fallback matter due to central energy source in supernova, Publications of the Astronomical Society of Japan, October 2018, Oxford University Press (OUP),
DOI: 10.1093/pasj/psy108.
You can read the full text:
Resources
Contributors
The following have contributed to this page
