Relativistic stellar pulsations with near-zone boundary conditions

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 56, Issue 4, 1997, Pages 2118-2126

  Lindblom, Lee ^a   Mendell, Gregory ^b   Ipser, James R ^b  

^a CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^b University of Florida   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0000106373     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.56.2118     Document Type: Article

References (19)

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14. The function (Formula presented) vanishes linearly at the surface of any equilibrium stellar model. This makes (Formula presented) the most slowly vanishing thermodynamic function at the stellar suface having a finite gradient there. Imposing the boundary condition (Formula presented) at the surface of the star ensures that the Lagrangian changes in other more rapidly vanishing potentials (such as the pressure) will also vanish there.
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18. Unfortunately the (Formula presented) dependence of the exact expression for (Formula presented) is a very slowly converging series in (Formula presented). Adding the first order (Formula presented) correction to the imaginary part of Eq. (28) can be accomplished by multiplying that term by (Formula presented). This correction reduces the accuracy of the frequencies of the modes in the most relativistic models. Presumably a more accurate boundary condition than Eq. (28) could be constructed by adding the appropriate higher-order terms in (Formula presented).
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