I've spent a bit of time seeing what information we can obtain about stars given the data provided in the journal and thought I'd write my notes down here in case it helps anyone else.
To recap, at current the useful (for my purposes) values available in each scan of a stellar body are:
The first additional piece of data that we can obtain is the luminosity of the body. This is purely proportional to absolute magnitude, and can be obtained using the following equation:
(4.83 is the absolute magnitude of Sol)
With the luminosity and the radius of the body we can work out the surface temperature:
(3.828e26 is the luminosity of Sol in Watts)
(5.670367e-8 is the Stefan-Boltzmann constant)
Obviously the above formula can be simplified, but I left it in its rawer form to allow people to see its derivation.
With the the surface temperature and absolute magnitude we can classify the type of star using the Hertzsprung-Russell diagram. There is no simple formula for this, and although it's crying out for a classifier I couldn't find one on the 'net.
The other immediately-obvious value that could be calculated is density, although I'm not sure if it's useful in any way.
Feel free to provide any additions or corrections.
To recap, at current the useful (for my purposes) values available in each scan of a stellar body are:
- AbsoluteMagnitude
- Radius
- StellarMass
The first additional piece of data that we can obtain is the luminosity of the body. This is purely proportional to absolute magnitude, and can be obtained using the following equation:
(4.83 is the absolute magnitude of Sol)
With the luminosity and the radius of the body we can work out the surface temperature:
(3.828e26 is the luminosity of Sol in Watts)
(5.670367e-8 is the Stefan-Boltzmann constant)
Obviously the above formula can be simplified, but I left it in its rawer form to allow people to see its derivation.
With the the surface temperature and absolute magnitude we can classify the type of star using the Hertzsprung-Russell diagram. There is no simple formula for this, and although it's crying out for a classifier I couldn't find one on the 'net.
The other immediately-obvious value that could be calculated is density, although I'm not sure if it's useful in any way.
Feel free to provide any additions or corrections.
