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))
|
 |
|
