Interaction between supernova ejecta and circumstellar
outflowing disks

k 2016

Interaction between supernova ejecta and circumstellar outflowing disks

KURFÜRST, Petr a Jiří KRTIČKA

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

Odkazy

URL

Příznaky

Mezinárodní význam

Změněno: 15. 6. 2016 11:41, Mgr. Ing. arch. Petr Kurfürst, Ph.D.

Anotace

V originále

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.

Citovat

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.

@proceedings{1347671,
   author = {Kurfürst, Petr and Krtička, Jiří},
   booktitle = {Bridging the gap: from massive stars to supernovae, Kavli Event, June 01 - June 02, 2016, Kavli Royal Society Centre, Chicheley Hall, UK},
   title = {Interaction between supernova ejecta and circumstellar outflowing disks},
   url = {http://physics.muni.cz/~petrk/poster.pdf},
   year = {2016}
}

TY  - CONF
ID  - 1347671
AU  - Kurfürst, Petr - Krtička, Jiří
PY  - 2016
TI  - Interaction between supernova ejecta and circumstellar outflowing disks
UR  - http://physics.muni.cz/~petrk/poster.pdf
N2  - 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.
ER  -

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

Přehled o publikaci