Peter H. Hauschildt
Dept. of Physics and Astronomy & Center for Simulational Physics, University of Georgia, Athens, GA 30602-2451
Email: yeti@hal.physast.uga.edu

France Allard
Dept. of Physics, Wichita State University, Wichita, KS 67260-0032
E-Mail: allard@eureka.physics.twsu.edu -

E. Baron
Dept. of Physics and Astronomy, University of Oklahoma,
440 W. Brooks, Rm 131, Norman, OK 73019-0225
E-Mail: baron@mail.nhn.ou.edu

Abstract:

We present our NextGen Model Atmosphere grid for low mass stars to effective temperatures larger than $3000\,{\rm K}$. These LTE models are calculated with the same basic model assumptions and input physics as the VLMS part of the NextGen grid so that the complete grid can be used, e.g., for consistent stellar evolution calculations and for internally consistent analysis of cool star spectra. This grid is also the starting point for a large grid of detailed NLTE model atmospheres for dwarfs and giants (Hauschildt et al, in preparation). The models were calculated from $3000\,{\rm K}$ to $10000\,{\rm K}$ (in steps of $200\,{\rm K}$) for $3.5 \le \log(g)\le 5.5$(in steps of 0.5) and metallicities of $-4.0 \le [{\rm M/H}]\le 0.0$.

We discuss the results of the model calculations and compare our results to the Kurucz 1994 grid. Some comparisons to standard stars like Vega and the Sun are presented and compared with detailed NLTE calculations.