Resonant excitation of white dwarf oscillations in compact object binaries – I. The no back reaction approximation
Identifieur interne : 000294 ( Main/Exploration ); précédent : 000293; suivant : 000295Resonant excitation of white dwarf oscillations in compact object binaries – I. The no back reaction approximation
Auteurs : Yasser Rathore [États-Unis] ; Roger D. Blandford [États-Unis] ; Avery E. Broderick [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005-03.
English descriptors
Abstract
We consider the evolution of white dwarfs with compact object companions (specifically black holes with masses up to ∼106 M⊙, neutron stars, and other white dwarfs). We suppose that the orbits are initially quite elliptical and then shrink and circularize under the action of gravitational radiation. During this evolution, the white dwarfs will pass through resonances when harmonics of the orbital frequency match the stellar oscillation eigenfrequencies. As a star passes through these resonances, the associated modes will be excited and can be driven to amplitudes that are so large that there is a back reaction on the orbit which, in turn, limits the growth of the modes. A formalism is presented for describing this dynamical interaction for a non‐rotating star in the linear approximation when the orbit can be treated as non‐relativistic. A semi‐analytical expression is found for computing the resonant energy transfer as a function of stellar and orbital parameters for the regime where back reaction may be neglected. This is used to calculate the results of passage through a sequence of resonances for several hypothetical systems. It is found that the amplitude of the ℓ=m= 2f‐mode can be driven into the non‐linear regime for appropriate initial conditions. We also discuss where the no back reaction approximation is expected to fail, and the qualitative effects of back reaction.
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DOI: 10.1111/j.1365-2966.2004.08459.x
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The no back reaction approximation</title><author><name sortKey="Rathore, Yasser" sort="Rathore, Yasser" uniqKey="Rathore Y" first="Yasser" last="Rathore">Yasser Rathore</name><affiliation wicri:level="1"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Theoretical Astrophysics, Caltech 130‐33, Pasadena, CA 91125</wicri:regionArea><wicri:noRegion>CA 91125</wicri:noRegion></affiliation></author><author><name sortKey="Blandford, Roger D" sort="Blandford, Roger D" uniqKey="Blandford R" first="Roger D." last="Blandford">Roger D. 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We suppose that the orbits are initially quite elliptical and then shrink and circularize under the action of gravitational radiation. During this evolution, the white dwarfs will pass through resonances when harmonics of the orbital frequency match the stellar oscillation eigenfrequencies. As a star passes through these resonances, the associated modes will be excited and can be driven to amplitudes that are so large that there is a back reaction on the orbit which, in turn, limits the growth of the modes. A formalism is presented for describing this dynamical interaction for a non‐rotating star in the linear approximation when the orbit can be treated as non‐relativistic. A semi‐analytical expression is found for computing the resonant energy transfer as a function of stellar and orbital parameters for the regime where back reaction may be neglected. This is used to calculate the results of passage through a sequence of resonances for several hypothetical systems. It is found that the amplitude of the ℓ=m= 2f‐mode can be driven into the non‐linear regime for appropriate initial conditions. We also discuss where the no back reaction approximation is expected to fail, and the qualitative effects of back reaction.</div></front></TEI><affiliations><list><country><li>États-Unis</li></country></list><tree><country name="États-Unis"><noRegion><name sortKey="Rathore, Yasser" sort="Rathore, Yasser" uniqKey="Rathore Y" first="Yasser" last="Rathore">Yasser Rathore</name></noRegion><name sortKey="Blandford, Roger D" sort="Blandford, Roger D" uniqKey="Blandford R" first="Roger D." last="Blandford">Roger D. Blandford</name><name sortKey="Blandford, Roger D" sort="Blandford, Roger D" uniqKey="Blandford R" first="Roger D." last="Blandford">Roger D. Blandford</name><name sortKey="Broderick, Avery E" sort="Broderick, Avery E" uniqKey="Broderick A" first="Avery E." last="Broderick">Avery E. 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