Quasinormal modes of relativistic stars and interacting fields
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Quasinormal modes of relativistic stars and interacting fields. / Macedo, Caio F. B.; Cardoso, Vitor; Crispino, Luis C. B.; Pani, Paolo.
I: Physical Review D, Bind 93, Nr. 6, 064053, 21.03.2016.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Quasinormal modes of relativistic stars and interacting fields
AU - Macedo, Caio F. B.
AU - Cardoso, Vitor
AU - Crispino, Luis C. B.
AU - Pani, Paolo
PY - 2016/3/21
Y1 - 2016/3/21
N2 - The quasinormal modes of relativistic compact objects encode important information about the gravitational response associated with astrophysical phenomena. Detecting such oscillations would provide us with a unique understanding of the properties of compact stars and may give definitive evidence for the existence of black holes. However, computing quasinormal modes in realistic astrophysical environments is challenging due to the complexity of the spacetime background and of the dynamics of the perturbations. We discuss two complementary methods for computing the quasinormal modes of spherically symmetric astrophysical systems, namely, the direct integration method and the continued-fraction method. We extend these techniques to dealing with generic coupled systems of linear equations, with the only assumption being that the interaction between different fields is effectively localized within a finite region. In particular, we adapt the continued-fraction method to include cases where a series solution can be obtained only outside an effective region. As an application, we compute the polar quasinormal modes of boson stars by using the continued-fraction method for the first time. The methods discussed here can be applied to other situations in which the perturbations effectively couple only within a finite region of space.
AB - The quasinormal modes of relativistic compact objects encode important information about the gravitational response associated with astrophysical phenomena. Detecting such oscillations would provide us with a unique understanding of the properties of compact stars and may give definitive evidence for the existence of black holes. However, computing quasinormal modes in realistic astrophysical environments is challenging due to the complexity of the spacetime background and of the dynamics of the perturbations. We discuss two complementary methods for computing the quasinormal modes of spherically symmetric astrophysical systems, namely, the direct integration method and the continued-fraction method. We extend these techniques to dealing with generic coupled systems of linear equations, with the only assumption being that the interaction between different fields is effectively localized within a finite region. In particular, we adapt the continued-fraction method to include cases where a series solution can be obtained only outside an effective region. As an application, we compute the polar quasinormal modes of boson stars by using the continued-fraction method for the first time. The methods discussed here can be applied to other situations in which the perturbations effectively couple only within a finite region of space.
KW - BLACK-HOLES
KW - BOSON
KW - STABILITY
KW - OSCILLATIONS
U2 - 10.1103/PhysRevD.93.064053
DO - 10.1103/PhysRevD.93.064053
M3 - Journal article
VL - 93
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 6
M1 - 064053
ER -
ID: 299821245