Title:

Populations in the Kepler field

Using a population synthesis model I have created a synthetic catalogue of stars in
the Kepler field of view. This model has then been subjected to the same biases and
selection effects inherent in the selection of stars for the Kepler transit survey mission.
This produced a synthetic Kepler Input Catalogue (KIC) which was subjected
to the Kepler Stellar Classification Program (SCP) method for determining stellar
parameters. I achieve a satisfactory match between the synthetic KIC and the real
KIC in the logg vs log Teff diagram. I find a median difference of ~Teff = +500 K
and ~ ~logg = 0.2 dex for main sequence stars, although there is a large variation
across parameter space. I find no significant difference between ~Teff and ~logg
for single stars and the primary star in a binary system. I also recreated the Kepler
target selection method and found that the binary fraction is unchanged by the target
selection. The fraction of main sequence stars in the sample increases from 75%
to 80%, and the giant star fraction decreases from 25% to 20%.
I have then used the synthetic KIC to build a of synthetic sample of eclipsing binaries
(EBs) in the Kepler field. Comparing the synthetic catalogue to the Kepler EB
catalogue I find that the Kepler EB pipeline introduces significant biases into the derived
temperature ratio and fractional radii. I then tested the effect of different initial
mass ratio distributions (IMRDs) and initial binary fraction distributions (IBFDs). At
this time, all distributions fail to match the data, such that their parameters can not
be constrained.
Modelling the population of asteroseismic binaries, where both stars have a detectable
asteroseismic signal, have shown a way to constrain the IMRD for equal
mass systems. This method is independent of the binary period and orbital orientation.
The number of detectable asteroseismic binaries increases from 87 for the IMR
parameter s = 0.5 to 256 for s = 1.0. The number of detectable asteroseismic EBs
increases from 34.0 ± 6.0 (s = 0.5) to 59.0 ± 6.0 (s = 1.0). This number shows disagreement
with the number of actual systems detected (2 for P orb < 40 days), which
can not be explained by incompleteness alone.
