| Authors : | Kuntal Misra (1), Bhavya Ailawadhi (1, 2), Naveen Dukiya (1, 3), Monalisa Dubey (1,3), Raya Dastidar (4, 5), Anjasha Gangopadhyay (6), Mridweeka Singh (7) |
| Authors Affiliation: | 1 Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263 001, India
2 Department of Physics, Deen Dayal Upadhyaya Gorakhpur University, Gorakhpur-273009, India
3 Department of Applied Physics, Mahatma Jyotiba Phule Rohilkhand University, Bareilly, 243006, India
4 Instituto de Astrofísica, Universidad Andres Bello, Fernandez Concha 700, Las Condes, Santiago RM, Chile
5 Millennium Institute of Astrophysics (MAS), Nuncio Monsenor Sòtero Sanz 100, Providencia, Santiago RM, Chile
6 Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Japan
7 Indian Institute of Astrophysics, Koramangala 2nd Block, Bangalore 560034, India |
| Abstract : | Supernovae of core-collapse origin result from the core collapse of massive stars. Based on spectral features' presence/absence, they are sub-classified into different categories. The progenitors of the supernovae sub-types also differ. Direct imaging has detected progenitors of about two dozen type IIP supernovae ranging between 8-20 M_sun. Direct imaging has not resulted in progenitor detection for other subtypes except in a few cases. Indirect methods can be used to determine the nature of the progenitor, such as light curve modelling, nebular phase spectrum modelling, and the use of line ratios and nucleosynthesis yields. In this talk, I will review the different methods and discuss the results obtained for the supernovae sub-types. I will briefly discuss the continuity between the progenitors of various core-collapse supernova sub-types. |
