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We calculated plane-parallel, chemically homogeneous model-atmospheres in hydrostatic and radiative equilibrium with the Tübingen Non-local thermodynamic equilibrium (NLTE) Model Atmosphere Package (TMAP). Model atoms were taken from the Tübingen Model Atom Database (TMAD). For further information about TMAP and TMAD see Werner et al. (2003, 2012) and Rauch & Deetjen (2003), respectivley.

On this website we presented our currently best stellar model-atmosphere (red) for the DA-type white dwarf G191-B2B (Teff = 60000 K, log (g / cm/s2) = 7.60).

In the plots below we show the complete energy distribution from the far ultraviolet (FUV) till to the ultraviolet (UV). Each plot describes a typical wavelength range (FUV, and UV) and you will find some information about the observation.
To scroll in the plots, press <SHIFT> and use your mouse wheel.

FUSE

The observation which is shown here is a combination by Rauch et al. (2013) from five separate observations (M1010201, M1010202, M1030602, P1041203, and S3070101). All observations are available in the MAST archive. The reached resolving power for FUSE is for the given wavelength range between 15000 and 20000.


STIS

The observation which is shown here is a combination by Rauch et al. (2013) from 105 separate observations. All observations are available in the MAST archive. The reached resolving power is 114000 (E140H, 1140 - 1700 Å), and 30000 (E230H, 1605 - 3110 Å).