Speaker
Ms
Miyu Masuyama
(University of Tokyo, Research center for the early universe)
Description
Magnetars are neutron stars with strong magnetic fields(B~10^14-10^15G). The mechanism to make such a strong magnetic field and what kind of supernova generates a magnetar have not been well understood. Recent observations of supernova remnants associated with magnetars indicate that magnetar progenitors are massive stars and the typical explosion energy is 10^51 erg (e.g. Kumar et al., 2014, Vink & Kuiper, 2006).
We perform 1D hydrodynamical simulations of magnetar-powered supernovae to test a scenario of magnetar-powered supernovae. The explosion of a massive star triggered by the energy supply from the rotation energy of a magnetar due to the magnetic dipole radiation. If the initial spin period of a magnetar is very short(P0~1 ms), the rotation energy becomes up to 10^52 erg. A half of the energy is used to climb up the gravitational potential well of a massive star and the resultant supernova remnant possesses the rest of the energy. Our simulation results reproduce the expansion velocity, the size, and the luminosity observed for CTB109, which is one of supernova remnants associated with magnetars.
Primary author
Ms
Miyu Masuyama
(University of Tokyo, Research center for the early universe)
Co-authors
Prof.
Toshikazu Shigeyama
(University of Tokyo, Research center for the early universe)
Dr
Toshio Nakano
(High Energy Astrophysics Laboratory, RIKEN)
