Theoretical model services
Theoretical spectra
Available theoretical spectra models
 
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Theoretical Models Web Server

Stellar Spectra Models

Dalessio disk models:
Models of irradiated accretion disks around pre-main sequence stars by D'Alessio et al. (1998,1999,2001).
 
Coelho Synthetic stellar library:
Synthetic stellar library by P. Coelho, fully described in Coelho et al. (2005) (Astron.and.Astroph., in press)
 
Allard, NextGen:
The NextGen Model grid of theoretical spectra; Hauschildt, P.H., Allard, F., Baron, E., Schweitzer, A., ApJ 312, 377, 1999
 
Allard, COND 2000:
The COND00 Model grid of theoretical spectra. (Chabrier et al. 2000, ApJ, 542,464)
 
Allard, DUSTY 2000:
The DUSTY00 Model grid of theoretical spectra (Allard et al. 2001, ApJ, 556, 357)
 
Kurucz ODFNEW /NOVER models:
ODFNEW /NOVER models. Newly computed ODFs with better opacities and better abundances have been used. (The convective treatment is described in Castelli et al. 1997, AA 318, 841)
 
Husfeld et al models for non-LTE Helium-rich stars:
Husfeld et al models for non-LTE Helium-rich stars (Husfeld et al. 1989 A%26A, 222, 150)
 
TLUSTY BSTAR2006:
TLUSTY BSTAR2006 Grid: Early B-type stars, Teff = 15000K - 30000 K (Lanz, T., Hubeny, I. 2007, ApJS, 169, 83)
 
TLUSTY OSTAR2002:
TLUSTY OSTAR2002 Grid: O-type stars, Teff = 27500K - 55000 K (Lanz, T., & Hubeny, I. 2003, ApJS, 146, 417)
 
TLUSTY OSTAR2002+BSTAR2006:
TLUSTY OSTAR2002+BSTAR2006 Grid, The merged files use the BSTAR2006 models for effective temperatures up to 30,000 K and the OSTAR2002 models for higher temperatures. (TLusty web page)
 

Evolutionary Synthesis Models

POPSTAR with Chabrier IMF:
PopStar Evolutionary synthesis models. Using IMF from Chabrier (2003). This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Ferrini IMF:
PopStar Evolutionary synthesis models. Using IMF from Ferrini, Penco, Palla (1990). This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Kroupa IMF:
PopStar Evolutionary synthesis models. Using IMF from Kroupa (2002). This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Salpeter IMF (1):
PopStar Evolutionary synthesis models. Using IMF from Salpeter (1955) with m=(0.85-120)Msun. This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))
 
POPSTAR with Salpeter IMF (2):
PopStar Evolutionary synthesis models. Using IMF from Salpeter (1955) with m=(0.15-100)Msun. This grid of Single Stellar Populations covers a wide range in both, age and metallicity. The models use the most recent evolutionary tracks together with the use of new NLTE atmosphere models. (Mollá, García-Vargas & Bressan (2009))