Carl Schmidt

Investigation of the environment around close-in transiting exoplanets using cloudy

It has been suggested that hot stellar wind gas in a bow shock around an exoplanet is sufficiently opaque to absorb stellar photons and give rise to an observable transit depth at optical and UV wavelengths. In the first part of this paper, we use the CLOUDY plasma simulation code to model the absorption from X-ray to radio wavelengths by 1-D slabs of gas in coronal equilibrium with varying densities (

VOLATILE LOSS AND CLASSIFICATION OF KUIPER BELT OBJECTS

10^{4}-10^{8} \, {\rm cm^{-3}}

Observations of sodium in the coma of Comet C/2012 S1 (ISON) during outburst

) and temperatures (

Dynamics of HVECs emitted from comet C/2011 L4 as observed by STEREO

2000-10^{6} \ {\rm K}

3D multispecies collisional model of Ganymede's atmosphere

) illuminated by a solar spectrum. For slabs at coronal temperatures (

Orbital effects on Mercurys escaping sodium exosphere

10^{6} \ {\rm K}

The origin and fate of O

) and densities even orders of magnitude larger than expected for the compressed stellar wind (

_2

10^{4}-10^{5} \, {\rm cm^{-3}}

in Europa's ice: an atmospheric perspective

), we find optical depths orders of magnitude too small (

Dusk Over Dawn O

> 3\times10^{-7}