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### Model atmospheres and synthetic spectra

The following data is available for each model:

### Model parameters and organisation

## Wolf-Rayet model grids

### Recent Updates

## OB model grids

### Recent Updates

This WEB interface allows to inspect and download synthetic spectra for Wolf-Rayet and OB stars. The spectra are calculated from PoWR model atmospheres which account for Non-LTE, spherical expansion and metal line blanketing.

- Spectral Energy Distribution

(emergent flux received at 10pc distance, low spectral resolution) - Line spectrum in high resolution for different wavelength bands

(optionally normalized or flux-calibrated) - Atmosphere stratification

(incl. electron temperature, density, optical depth, etc.) - Colors and ionizing photons

The models are arranged in different *Model Grids*.
Each model grid is characterized by a set of common parameters, such as
stellar luminosity, terminal wind velocity, clumping contrast, and
chemical composition. For Wolf-Rayet stars of the nitrogen subclass (WN)
there are grids of hydrogen-free models (WNE) and of models with
a specified mass fraction of hydrogen (WNL). The iron-group and total CNO
mass fractions correspond to the metallicity of the Galaxy, the Large
Magellanic Cloud (LMC), or the Small Magellanic Cloud (SMC),
respectively.

log L | v_{final} | D_{max} |
X_{H} |
X_{He} | X_{C} |
X_{N} | X_{O} |
X_{Ne} | X_{Fe} |
|||
---|---|---|---|---|---|---|---|---|---|---|---|---|

[L_{sun}] | [km/s] | mass fractions | ||||||||||

Galactic Metallicity | ||||||||||||

MW WNE | Details | 5.3 | 1600 | 4 | - | 0.98 | 1.0E-4 | 0.015 | - | - | 1.4E-3 | |

MW WNL-H20 | Details | 5.3 | 1000 | 4 | 0.2 | 0.78 | 1.0E-4 | 0.015 | - | - | 1.4E-3 | |

MW WNL-H50 | Details | 5.3 | 1000 | 4 | 0.5 | 0.48 | 1.0E-4 | 0.015 | - | - | 1.4E-3 | |

MW WC | Details | 5.3 | 2000 | 10 | - | 0.55 | 0.4 | - | 0.05 | - | 1.6E-3 | |

LMC Metallicity | ||||||||||||

LMC WNE | Details | 5.3 | 1600 | 10 | - | 0.995 | 7.0E-5 | 4.0E-3 | - | - | 7.0E-4 | |

LMC WNL-H20 | Details | 5.3 | 1000 | 10 | 0.2 | 0.795 | 7.0E-5 | 4.0E-3 | - | - | 7.0E-4 | |

LMC WNL-H40 | Details | 5.3 | 1000 | 10 | 0.4 | 0.595 | 7.0E-5 | 4.0E-3 | - | - | 7.0E-4 | |

LMC WC | Details | 5.3 | 2000 | 10 | - | 0.55 | 0.4 | - | 0.05 | 1.0E-3 | 7.0E-4 | |

SMC Metallicity | ||||||||||||

SMC WNE | Details | 5.3 | 1600^{‡} | 4 | - | 0.998 | 2.5E-5 | 1.5E-3 | - | - | 3.0E-4 | |

SMC WNL-H20 | Details | 5.3 | 1600^{‡} | 4 | 0.2 | 0.798 | 2.5E-5 | 1.5E-3 | - | - | 3.0E-4 | |

SMC WNL-H40 | Details | 5.3 | 1600^{‡} | 4 | 0.4 | 0.598 | 2.5E-5 | 1.5E-3 | - | - | 3.0E-4 | |

SMC WNL-H60 | Details | 5.3 | 1600^{‡} | 4 | 0.6 | 0.398 | 2.5E-5 | 1.5E-3 | - | - | 3.0E-4 | |

SMC WC | Details | 5.3 | 2000 | 10 | - | 0.547 | 0.4 | - | 0.05 | 2.4E-3 | 3.0E-4 | |

sub-SMC Metallicity (0.07 solar) | ||||||||||||

Z0.07 WNE | Details | 5.3 | 1600 | 10 | - | 0.999 | 1.0E-5 | 6.1E-4 | 1.0E-5 | - | 9.2E-5 | |

Z0.07 WNL-H20 | Details | 5.3 | 1600 | 10 | 0.2 | 0.799 | 1.0E-5 | 6.1E-4 | 1.0E-5 | - | 9.2E-5 | |

Z0.07 WNL-H40 | Details | 5.3 | 1600 | 10 | 0.4 | 0.599 | 1.0E-5 | 6.1E-4 | 1.0E-5 | - | 9.2E-5 | |

Z0.07 WNL-H60 | Details | 5.3 | 1600 | 10 | 0.6 | 0.399 | 1.0E-5 | 6.1E-4 | 1.0E-5 | - | 9.2E-5 | |

Z0.07 WC | Details | 5.3 | 2000 | 10 | - | 0.549 | 0.4 | - | 0.05 | 8.3E-4 | 9.2E-5 |

^{‡} "Double beta-law", see *WR model parameter details* dropdown below

WR model parameter details
▼

Each grid has a two-dimensional parameter space,
namely the stellar temperature T and the
"transformed radius" R_{t}. The latter is a function of the
mass-loss rate and the stellar radius. Thanks to an approximate
scaling invariance of WR atmospheres, the same model spectrum can be
applied to stars with different luminosities, but same T and R_{t}. When doing so, the absolute
fluxes must be scaled proportional to L, the radius R proportional to L^{1/2}, and the
mass-loss rate proportional to L^{3/4}.

Bug warning (Feb. 2021): The H I Paschen line at about 8502 Angstroem (transition 3 - 16) appears shifted redwards by 2.4 Angstroem in all model spectra due to a mistake in the atomic data.

New (Oct. 2016): The WNL-H50 grid has been re-calculated in 2016; this latest version is shown by default. The previous version of the WNL-H50 grid can still be accessed by choosing "WNL-H50-2013" in the drop-down menu below.

New (Oct. 2016): The WNL grid has been re-calculated in 2016; this latest version is shown by default. The previous version of the WNL grid can still be accessed by choosing "WNL-2012" in the drop-down menu below.

New (Sept. 2016): The WNE grid has been re-calculated in 2016; this latest version is shown by default. The previous version of the WNE grid can still be accessed by choosing "WNE-2013" in the drop-down menu below.

Grids of models for O- and B-type stars are provided for solar metallicity, for a metallicity of 1/2 solar as appropriate for the Large Magellanic Cloud (LMC), and for a metallicity of 1/7 solar as appropriate for the Small Magellanic Cloud (SMC), respectively.

Each grid has a two-dimensional parameter space, namely the stellar
temperature T and the surface gravity
g_{grav}. The grid resolution is 1 kK for the stellar
temperature and 0.2dex for the surface gravity, log g. Regarding the
stellar wind, the different grids of OB-type stars which are provided
have either a fixed mass-loss rate, a fixed log Q value (see "OB model parameter details" below
for the definition of Q), or each model has a specific mass-loss rate
as predicted from theoretical mass-loss recipes (see Table below). For
more information about the individual grids click on "Details".

T | log g | log M | log Q | D_{max} |
v_{turb} |
X_{H} |
X_{He} | X_{C} |
X_{N} | X_{O} |
X_{Mg} | X_{Si} |
X_{P} | X_{S} |
X_{Fe} |
|||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|

[kK] | [cgs] | [M_{sun}/yr] | km/s | mass fractions | ||||||||||||||

Galactic Metallicity | ||||||||||||||||||

OB-I | Details | 15…56 | 2.0…4.4 | -7 | 10 | 7 | 0.738 | 0.251 | 2.4E-3 | 6.9E-4 | 5.7E-3 | 6.9E-4 | 6.7E-4 | 5.8E-6 | 3.1E-4 | 1.2E-3 | ||

LMC Metallicity | ||||||||||||||||||

LMC-OB-I | Details | 15…50 | 2.0…4.4 | -7 | 10 | 7 | 0.738 | 0.258 | 4.7E-4 | 7.8E-5 | 2.6E-3 | 2.1E-4 | 3.2E-4 | 2.9E-6 | 1.5E-4 | 7.0E-4 | ||

SMC Metallicity | ||||||||||||||||||

SMC-OB-Vd3 | Details | 15…50 | 2.0…4.4 | Vink et al. (2001) / 3 | 10 | 7 | 0.738 | 0.261 | 2.1E-4 | 3.3E-5 | 1.1E-3 | 9.9E-5 | 1.3E-4 | 8.3E-7 | 4.4E-5 | 3.5E-4 | ||

SMC-OB-I | Details | 15…50 | 2.0…4.4 | moderate | -13.0 | 10 | 10 | 0.738 | 0.261 | 2.1E-4 | 3.3E-5 | 1.1E-3 | 9.9E-5 | 1.3E-4 | 8.3E-7 | 4.4E-5 | 3.5E-4 | |

SMC-OB-II | Details | 15…50 | 2.0…4.4 | high | -12.0 | 10 | 10 | 0.738 | 0.261 | 2.1E-4 | 3.3E-5 | 1.1E-3 | 9.9E-5 | 1.3E-4 | 8.3E-7 | 4.4E-5 | 3.5E-4 | |

SMC-OB-III | Details | 15…50 | 2.0…4.4 | low | -14.0 | 10 | 10 | 0.738 | 0.261 | 2.1E-4 | 3.3E-5 | 1.1E-3 | 9.9E-5 | 1.3E-4 | 8.3E-7 | 4.4E-5 | 3.5E-4 |

OB model parameter details
▼

New (Feb. 2023): A new grid SMC-OB-Vd3 has been added. Individual mass loss rates are adopted for each of the grid models (see more Details). Hence, this grid is most appropriate for population synthesis at SMC metallicity.

Bug warning (Feb. 2021): The H I Paschen line at about 8502 Angstroem (transition 3 - 16) appears shifted redwards by 2.4 Angstroem in all model spectra with fixed log M or log Q due to a mistake in the atomic data.

Bug warning (Feb. 2021): The S IV resonance line in the UV at 1062 - 1073 Angstroem is missing in all OB-type model spectra with fixed log M or log Q due to a mistake in the atomic data.

New (Aug. 2019): The grid SMC-OB-III (low mass-loss rates) has been added.