The page contains results of simulations described in the paper [pdf]

Cooling curves and models of the post-shock:
logN=12; V= 150 | 200 | 300 | 400 | 500 km/s.
V=300 km/s, logN= 10| 11| 12| 13| 14

Combined models of the pre-shock, post-shock and hotspot. The HHeCO models.
logN=12; V= 150 | 200 | 300 | 400 | 500 km/s.
V=300 km/s, logN= 10| 11| 12| 13| 14

Low resolution spectra from the accretion region (pre-shock+post-shock+hotspot, the HHeCO models). The Eddington flux H_λ [erg/s/cm^2/A/sr]
logN=12; V= 150 | 200 | 300 | 400 | 500 km/s.
V=300 km/s, logN= 10| 11| 12| 13| 14

Emerging intensities from the accretion region (pre-shock+post-shock+hotspot)
H α, H β, Br γ,
HeI 4921 A, HeI 5876 A, HeI 6678 A, HeI 10830 A,
HeII 1640 A, HeII 4686 A
The intensities are written in the fits format and can be browsered with your favorite fits viewer. In ds9 fits files look like this:

Here the horizontal graph represents the line profile at given μ (see y value), and the vertical graph is for the limb darkening (brightening) at a given wavelength (see x value). All wavelengths are in vacuum.

Related conference paper (2017ASPC..510..110D) and presentation
The hotspot emission in the case of the oblique shock is described in the paper [pdf]

The page contains results of the non-LTE calculations described in the paper [pdf] as well as some additional information. Spectra and models of the hot spot, which are given below, were calculated taking into account departures from LTE for hydrogen and helium. Other elements were calculated in LTE with solar abundances.

The description and tests of the computer program and atomic data [pdf]

Models of the hot spots [tar.gz][list of files]

Spectra of the hot spots. Eddington flux H_hs [tar.gz][list of files]
Spectra of the pre-shock. Eddington flux H_pre [tar.gz][list of files]
The sum H_hs+H_pre [tar.gz][list of files]

Small grid of stellar LTE-spectra calculated with ATLAS9/SYNTHE between 0.3 -- 1.2 mkm [tar.gz][list of files]