Interaction between supernova ejecta and circumstellar outflowing disks

KURFÜRST, Petr a Jiří KRTIČKA. Interaction between supernova ejecta and circumstellar outflowing disks. In Bridging the gap: from massive stars to supernovae, Kavli Event, June 01 - June 02, 2016, Kavli Royal Society Centre, Chicheley Hall, UK. 2016.

Základní údaje

• Originální název: Interaction between supernova ejecta and circumstellar outflowing disks
• Název anglicky: Interaction between supernova ejecta and circumstellar outflowing disks
• Autoři: KURFÜRST, Petr a Jiří KRTIČKA.
• Vydání: Bridging the gap: from massive stars to supernovae, Kavli Event, June 01 - June 02, 2016, Kavli Royal Society Centre, Chicheley Hall, UK, 2016.

Další údaje

• Typ výsledku: Prezentace na konferencích
• Utajení: není předmětem státního či obchodního tajemství
• WWW: URL
• Příznaky: Mezinárodní význam

Anotace

Massive stars are characterized by a significant loss of mass either via the spherically symmetric stellar winds or by aspherical forms such as bipolar lobes or outflowing equatorial disks. Since a portion of most massive stars end their lives as a core-collapse supernovae, they are always located inside a large circumstellar envelopes, created by their progenitors. We study the dynamic and thermal effects of collision between the expanding ejecta of supernova and circumstellar disks that may be formed during, e.g., B[e] star phase, LBV phase, or by various forms of accretion. We simulate the supernova explosion as a spherically symmetric blast wave. The initial geometries of the disks correspond to a density structure of a material that orbits in Keplerian trajectories. Using our own multidimensional hydrodynamic code, based on Roe's method, we examine the behavior of basic hydrodynamic characteristics, i.e., the density, pressure, escape velocity and temperature structure in the interaction zone under various geometrical configurations and various initial densities of the circumstellar medium. We calculate the rate of the aspherical deceleration of the supernova ejecta as well as the rate of conversion of the kinetic energy of the supernova ejecta into thermal energy. We expect that subsequent study of the supernova light curves powered by such interaction thermal energy excess will lead to a better understanding of the mass and density distribution of the circumstellar medium. It may also provide more precise estimates of the disk mass-loss rates and to a deeper knowledge of the geometry and mechanism of the mass loss of massive stars.