Abstract Details

Name: Jagriti Gaba
Affiliation: G D Goenka Education City, Sohna - Gurgaon Rd, Sohna, Haryana 122103
Conference ID: ASI2021_182
Title : Estimation of $^{56}$Ni mass of Type Ia Supernovae
Authors and Co-Authors : Jagriti Gaba1, Ashima Goel1, Naresh Sharma1, Abhinav Gupta1, and Shashikant Gupta1 1. GD Goenka University, Gurugram
Abstract Type : Poster
Abstract Category : Stars, ISM and Galaxy
Abstract : One of the most important extra-galactic distance indicators the Type Ia Supernovae (SNe Ia) have played a crucial role in the discovery of dark energy. However, the physics of explosion mechanism is not fully understood. The light curves (LC) of SNe Ia are characterised by a sharp rise, reaching a peak and a slow decline after that. The decline phase is powered by the radio-active decay of $^{56}$Ni and $^{56}$Co which are produced via nuclear reactions in the explosion along with the other intermediate mass elements. The amount of $^{56}$Ni decides the decline rate and hence the width of LC. Modeling the LC and measuring the mass of $^{56}$Ni is still a challenging issue despite the several attempts made through observations and numerical simulations. However, the IR light curves show a secondary maxima after the prominent bolometric peak. It is suggested that the time of the secondary peak ($t_2$) is correlated with the bolometric luminosity of the first peak. We fit a cubic spline to obtain the peak luminosity from $t_2$. Now the Arnett's rule with a fixed rise time is implemented to calculate the $^{56}$Ni mass. For a sample of 58 SNe Ia, the relation between peak luminosity and $t_2$ is applied. The Carneige Supernova Project is the main source of the data for SNe Ia. The $^{56}$Ni mass calculated using the above method is in good agreement with the literature. The advantage of the method is that it is un-affected by the reddening.