8th HEAD Meeting, 8-11 September, 2004
Session 8 Pulsars and Magnetars
Poster, Wednesday, September 8, 2004, 9:00am-10:00pm

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[8.04] Neutron Star Structure in the Presence of Scalar Fields

D. Kazanas (NASA/GSFC, LHEA), J.P. Crawford (Dept. of Physics, Penn State U.)

Motivated by the possible presence of scalar fields on astrophysical scales, suggested by the apparent acceleration of the universe implied by the supernovae surveys, we present models of neutron star structure including the contribution of a (massless) scalar field to the stress energy momentum tensor, in addition to that made by the normal matter. To that end we solve the coupled Einstein -- scalar field -- hydrostatic balance equations to compute the effect of the presence of the scalar field on the neutron star structure. We find that the presence of the scalar field does change the structure of the neutron star, especially in cases of strong coupling between the scalar field and the matter density. We present the neutron star radius as a function of the matter--scalar field coupling constant for different values of the neutron star central density. The presence of the scalar field affects both the maximum neutron star mass and its radius, the latter increasing with the value of the above coupling constant. We also compute particle and photon geodesics in the geometry of these neutron stars as well as to the geometry of black holes with different values of the scalar field. Our results may be testable with timing observations of accreting neutron stars.

The author(s) of this abstract have provided an email address for comments about the abstract: Demos.Kazanas-1@nasa.gov

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