Axially Symmetric Post-Newtonian Stellar Systems
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Universidad Industrial de Santander
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Presentamos un método para obtener modelos estelares discoidales,axialmente simétricos, auto-consistentes en la primera aproximaciónpost-Newtoniana (1PN). Usando en las ecuaciones de campo de la aproximación1PN una función de distribución conocida (DF) que correspondea un modelo Newtoniano, se obtienen dos ecuaciones fundamentales paradeterminar las correcciones 1PN. Las curvas de rotación de los modelos corregidosdifieren de las clásicas y las correcciones son claramente apreciablescon los valores de la masa y el radio de una galaxia típica. Por otro lado, lacorrección relativista de la masa se puede ignorar para todos los modelos.
We introduce a method to obtain self-consistent, axially symmetricdisklike stellar models in the first post-Newtonian (1PN) approximation.By using in the field equations of the 1PN approximation a distributionfunction (DF) corresponding to a Newtonian model, two fundamental equationsdetermining the 1PN corrections are obtained. The rotation curves ofthe corrected models differs from the classical ones and the corrections areclearly appreciable with values of the mass and radius of a typical galaxy.On the other hand, the relativistic mass correction can be ignored for allmodels.
We introduce a method to obtain self-consistent, axially symmetricdisklike stellar models in the first post-Newtonian (1PN) approximation.By using in the field equations of the 1PN approximation a distributionfunction (DF) corresponding to a Newtonian model, two fundamental equationsdetermining the 1PN corrections are obtained. The rotation curves ofthe corrected models differs from the classical ones and the corrections areclearly appreciable with values of the mass and radius of a typical galaxy.On the other hand, the relativistic mass correction can be ignored for allmodels.
Keywords
Post-Newtonian approximation, galactic and stellar dynamics, Primer aproximación post-newtoniana, dinámicas estelar ygaláctica