Pulsational Pair-instability Model for Superluminous Supernova PTF12dam:Interaction and Radioactive Decay

A Criterion for Nuclear-Energized Pulsational Instability

Multimodal Radial Pulsational Instability In A Prenova Model

A prenova model, consisting of a white dwarf unstably burning a shell of accreted hydrogen, was tested for stability against radial pulsations. The pulsational analysis included terms due to thermal imbalance. The model was found to be pulsationally unstable in all of the modes examined, save one in which the thermal-imbalance integrals made the crucial damping contribution. An evaluation of so...

The Light Curve in Supernova Modeled by a Continuous Radioactive Decay of 56

The UVOIR bolometric light curves are usually modeled by the radioactive decay. In order to model more precisely the absolute/apparent magnitude versus time relationship the continuous production of radioactive isotopes is introduced. A differential equation of the first order with separable variables is solved.

Condensation of carbon in radioactive supernova gas.

Chemistry resulting in the formation of large carbon-bearing molecules and dust in the interior of an expanding supernova was explored, and the equations governing their abundances were solved numerically. Carbon dust condenses from initially gaseous carbon and oxygen atoms because energetic electrons produced by radioactivity in the supernova cause dissociation of the carbon monoxide molecules...

Poisson Distribution of Radioactive Decay

In this experiment we observe the distribution of radiation emitted by a Cs source. Using a scintillation counter, we count the number of gamma rays emitted by the radiation source at four different mean count rates: 1 sec−1, 4 sec−1, 10 sec−1, and 100 sec−1. From this we can plot the distribution of counts/sec versus the frequency of count rate. We find the distributions for the different mean...