Kate Blackham
Career Stage
Recent Graduate
Poster Abstract
This project sought to find a Galactic birth rate for Type Ia supernovae (SNe Ia) with progenitors that are a white dwarf (WD) accreting mass from a companion non-WD. SNe Ia are used as ‘standard candles’ to measure intergalactic distances and occur when a WD exceeds its maximum mass: the Chandrasekhar mass. The accepted Galactic birth rate of SNe Ia is (4 ± 1) × 10^(-3) per year. It is not known what proportion of SNe Ia occur via the potential progenitor types; if more SNe Ia are the result of a WD-WD collision than a single WD accreting matter from a companion, is our assumption that SNe Ia are standard candles valid?
Plain text summary
There is a QR code towards the bottom left to allow viewers to read the PDF of full report.
Next to the abstract is a graphic illustrating an accretion disk from a non-WD companion dumping material onto a WD.
The normalized histogram shows that while He white dwarfs produce the majority of Type Ia supernovae when the mass is below 2 solar masses, Carbon-Oxygen white dwarfs are likely to be significant contributors to the number of Type Ia supernovae for those with primary masses 2-8 solar masses.
To the right of the poster, a graph shows that the peak edge-lit detonation birth rate occurs at 2 Gyr.
The code used did not allow for a time-varying novae mass retention factor (Greek letter epsilon), however with a value of 1, the accretion phase is short lived as shown in the graph in the bottom right corner where the density of data points is much greater along a straight line where t1 (onset time of accretion in Myr) = t2 (time of edge-lit detonation in Myr) and much more sparsely spread out along the t2 axis.
Next to the abstract is a graphic illustrating an accretion disk from a non-WD companion dumping material onto a WD.
The normalized histogram shows that while He white dwarfs produce the majority of Type Ia supernovae when the mass is below 2 solar masses, Carbon-Oxygen white dwarfs are likely to be significant contributors to the number of Type Ia supernovae for those with primary masses 2-8 solar masses.
To the right of the poster, a graph shows that the peak edge-lit detonation birth rate occurs at 2 Gyr.
The code used did not allow for a time-varying novae mass retention factor (Greek letter epsilon), however with a value of 1, the accretion phase is short lived as shown in the graph in the bottom right corner where the density of data points is much greater along a straight line where t1 (onset time of accretion in Myr) = t2 (time of edge-lit detonation in Myr) and much more sparsely spread out along the t2 axis.
Poster file
Poster Title
Modelling Type Ia supernovae with single white dwarf progenitors
Url
100627671@student.swin.edu.au