Updates:
- In the repository you will find a pseudo code outlining the algorithm which I began to implement in the source file IclipSe.py. The other file in the repository is a mathematica notebook which you can use in order to visualize quickly certain choices for the object’s orbits (goto the WOLFRAM cloud and register for free, basic usage).
Report:
We simulate the intensity of light which reaches a $4\pi$ detector at some point in space (conveniently chosen to be at the coordinate origin). This light is reaching us from distant objects, e.g., main-sequence stars, magnetars, black holes, brown dwarfs, etc. We assume complete knowledge about the object’s trajectories and hence do not dynamically simulate their motion as dictated by their interactions. Instead, we use observational and/or hypothetical data. Hence, we need to define the amount of light which reaches us from a point in phase space
\begin{equation}\vec{p}=\left\lbrace\vec{r}(t,i),\frac{d\vec{r}(t,i)}{dt}\right\rbrace_{i=1:N}\end{equation}
where, in the first step, we should neglect effects of the objects’ velocities. However, dilatation and eclipsing/overlap effects should be considered.
The detected/predicted intensity is a function of wave length ($\lambda$) as stellar objects to not emit radiation with a constant amplitude for any $\lambda$.
Outline:
- Gather realistic spectral data about the objects we want to make up our own universe.
- Access the observed data on the dynamics of the solar system and parametrise the trajectories of those orbits in a useful-for-us way.
- In order to familiarize yourself with
Juliaand/orPython, write a program which plots a 2-dimensional circle embeded in three dimensions. Create a repository (e.g. on GitHub ) and share the project with the participants.
Resources:
- Spectra (relative intensities as functions of wavelength) of five white dwarfs in the cluster galaxy NGC 6397
- solar-system dynamics