output from rotating models

[Simon Murphy]

Hello,

I have just been reading about the rotating models you are constructing for stars more massive than 2 M_sun. Specifically, I stumbled across ESTER in the Astrophysics Source Code Library. I have need for a code that treats rotation for A and B stars with accurate physics. I would like to be able to vary the rotation velocity and the inclination angle of each model. I was hoping you could tell me if this is possible.

I would like to ask what the output from the models can be. Can they give a mean Teff (because, of course, the rotators have different pole temperatures and gravities to the equatorial regions) and log g? And how about uvby\beta photometry? Or a synthetic spectrum?

I hope the project is alive and well.

Kind regards,
Simon Murphy.

PhD Student
Jeremiah Horrocks Institute,
University of Central Lancashire (UCLan),
Preston, PR1 2HE, UK

[Francisco Espinosa]

Dear Simon,

At this moment, the output of the ESTER code contains only the internal structure of the star. It gives Teff and log g as a function of latitude but not the synthetic spectrum or photometry, as they depend on the modelisation of the atmosphere.

There are plans to include these calculations on the code, but for the moment the only thing you can do is to use the values of Teff and log g given by the code to calculate a set of synthetic spectra using another tool and integrate over the surface of the star. 

Please, let me know if you have any problem using the code, or you have any other question.

Thanks for your interest in the project.

Kind regards,

Francisco Espinosa

Simon Murphy <si...@simonmurphy.info> escribió:

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