Supernova interaction with dense mass loss
نویسندگان
چکیده
منابع مشابه
Mass loss and supernova progenitors
We first discuss the mass range of type IIP SN progenitors and how the upper and lower limits impose interesting constraints on stellar evolution. Then we discuss the possible implications of two SNe, 2002ap and 2006jc, for Wolf-Rayet star mass-loss rates and long Gamma-ray bursts.
متن کاملPre-supernova mass loss predictions for massive stars
Massive stars and supernovae (SNe) have a huge impact on their environment. Despite their importance, a comprehensive knowledge of which massive stars produce which SNe is hitherto lacking. We use a Monte Carlo method to predict the mass-loss rates of massive stars in the Hertzsprung-Russell Diagram (HRD) covering all phases from the OB main sequence, the unstable Luminous Blue Variable (LBV) s...
متن کاملSupernova 1994 aj : a probe for pre - supernova evolution and mass loss from the progenitor . ?
Extensive photometric and spectroscopic observations of SN 1994aj until 540d after maximum light have been obtained. The photometry around maximum suggests that the SN belongs to the Type II Linear class, with a peak absolute magnitude of MV ∼ −17.8 (assuming H0 = 75km s−1 Mpc−1). The spectra of SN 1994aj were unusual with the presence of a narrow line with a P-Cygni profile on the top of the b...
متن کاملUnifying Type II Supernova Light Curves with Dense Circumstellar Material
A longstanding problem in the study of supernovae (SNe) has been the relationship between the Type IIP and Type IIL subclasses. Whether they come from distinct progenitors or they are from similar stars with some property that smoothly transitions from one class to another has been the subject of much debate. Here we show using one-dimensional radiation-hydrodynamic SN models that the multi-ban...
متن کاملSupernova Interaction with a Circumstellar Medium
The explosion of a core collapse supernova drives a powerful shock front into the wind from the progenitor star. A layer of shocked circumstellar gas and ejecta develops that is subject to hydrodynamic instabilities. The hot gas can be observed directly by its X-ray emission, some of which is absorbed and re-radiated at lower frequencies by the ejecta and the circumstellar gas. Synchrotron radi...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2013
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921313009290