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K. G. Arun - One of the best experts on this subject based on the ideXlab platform.
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Third post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact binaries in quasi-Elliptical Orbits
Physical Review D, 2009Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Siddhartha SinhaAbstract:The angular momentum flux from an inspiralling binary system of compact objects moving in quasi-Elliptical Orbits is computed at the third post-Newtonian (3PN) order using the multipolar post-Minkowskian wave generation formalism. The 3PN angular momentum flux involves the instantaneous, tail, and tail-of-tails contributions as for the 3PN energy flux, and in addition a contribution due to non-linear memory. We average the angular momentum flux over the binary's orbit using the 3PN quasi-Keplerian representation of Elliptical Orbits. The averaged angular momentum flux provides the final input needed for gravitational wave phasing of binaries moving in quasi-Elliptical Orbits. We obtain the evolution of orbital elements under 3PN gravitational radiation reaction in the quasi-elliptic case. For small eccentricities, we give simpler limiting expressions relevant for phasing up to order $e^2$. This work is important for the construction of templates for quasi-eccentric binaries, and for the comparison of post-Newtonian results with the numerical relativity simulations of the plunge and merger of eccentric binaries.
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tail effects in the third post newtonian gravitational wave energy flux of compact binaries in quasi Elliptical Orbits
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The far-zone flux of energy contains hereditary (tail) contr ibutions that depend on the entire past history of the source. Using the multipolar post-Minkowskian wave generation formalism, we propose and implement a semi-analytical method in the frequency domain to compute these contributions from the inspiral phase of a binary system of compact objects moving in quasi-Elliptical Orbits up to third post-Newtonian (3PN) order. The method explicitly uses the quasi-Keplerian representation of Elliptical Orbits at 1PN order and exploits the doubly periodic nature of the motion to average the 3PN flu xes over the binary’s orbit. Together with the instantaneous (non-tail) contributions evaluated in a companion paper, it provides crucial inputs for the construction of ready-to-use templates for compact binaries moving on quasi-elliptic Orbits, an interesting class of sources for the ground based gravitational wave detectors such as LIGO and Virgo as well as space based detectors like LISA.
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inspiralling compact binaries in quasi Elliptical Orbits the complete third post newtonian energy flux
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The instantaneous contributions to the third post-Newtonian (3PN) gravitational wave luminosity from the inspiral phase of a binary system of compact objects moving in a quasi-Elliptical orbit is computed using the multipolar post-Minkowskian wave generation formalism. The necessary inputs for this calculation include the 3PN accurate mass quadrupole moment for general Orbits and the mass octupole and current quadrupole moments at 2PN. Using the recently obtained 3PN quasi-Keplerian representation of Elliptical Orbits, the flux is averaged over the binary's orbit. Supplementing this by the important hereditary contributions arising from tails, tails of tails, and tails-squared terms calculated in a previous paper, the complete 3PN energy flux is obtained. The final result presented in this paper would be needed for the construction of ready-to-use templates for binaries moving on noncircular Orbits, a plausible class of sources not only for the space-based detectors like LISA but also for the ground-based ones.
Edgard G. Rivera-valentin - One of the best experts on this subject based on the ideXlab platform.
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The Equilibrium Temperature of Planets in Elliptical Orbits
The Astrophysical Journal, 2017Co-Authors: Abel Méndez, Edgard G. Rivera-valentinAbstract:There exists a positive correlation between orbital eccentricity and the average stellar flux that planets receive from their parent star. Often, though, it is assumed that the average equilibrium temperature would correspondingly increase with eccentricity. Here, we test this assumption by calculating and comparing analytic solutions for both the spatial and temporal averages of orbital distance, stellar flux, and equilibrium temperature. Our solutions show that the average equilibrium temperature of a planet, with a constant albedo, slowly decreases with eccentricity until converging to a value 90% that of a circular orbit. This might be the case for many types of planets (e.g., hot Jupiters); however, the actual equilibrium and surface temperature of planets also depend on orbital variations of albedo and greenhouse. Our results also have implications in understanding the climate, habitability, and the occurrence of potential Earth-like planets. For instance, it helps explain why the limits of the habitable zone for planets in highly Elliptical Orbits are wider than expected from the mean flux approximation, as shown by climate models.
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The Equilibrium Temperature of Planets in Elliptical Orbits
The Astrophysical Journal, 2017Co-Authors: Abel Méndez, Edgard G. Rivera-valentinAbstract:There exists a positive correlation between orbital eccentricity and the average stellar flux that planets receive from their parent star. Often, though, it is assumed that the average equilibrium temperature would correspondingly increase with eccentricity. Here, we test this assumption by calculating and comparing analytic solutions for both the spatial and temporal averages of orbital distance, stellar flux, and equilibrium temperature. Our solutions show that the average equilibrium temperature of a planet, with a constant albedo, slowly decreases with eccentricity until converging to a value 90% that of a circular orbit. This might be the case for many types of planets (e.g., hot Jupiters); however, the actual equilibrium and surface temperature of planets also depend on orbital variations of albedo and greenhouse. Our results also have implications in understanding the climate, habitability, and the occurrence of potential Earth-like planets. For instance, it helps explain why the limits of the habitable zone for planets in highly Elliptical Orbits are wider than expected from the mean flux approximation, as shown by climate models.
Mohd S S Qusailah - One of the best experts on this subject based on the ideXlab platform.
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tail effects in the third post newtonian gravitational wave energy flux of compact binaries in quasi Elliptical Orbits
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The far-zone flux of energy contains hereditary (tail) contr ibutions that depend on the entire past history of the source. Using the multipolar post-Minkowskian wave generation formalism, we propose and implement a semi-analytical method in the frequency domain to compute these contributions from the inspiral phase of a binary system of compact objects moving in quasi-Elliptical Orbits up to third post-Newtonian (3PN) order. The method explicitly uses the quasi-Keplerian representation of Elliptical Orbits at 1PN order and exploits the doubly periodic nature of the motion to average the 3PN flu xes over the binary’s orbit. Together with the instantaneous (non-tail) contributions evaluated in a companion paper, it provides crucial inputs for the construction of ready-to-use templates for compact binaries moving on quasi-elliptic Orbits, an interesting class of sources for the ground based gravitational wave detectors such as LIGO and Virgo as well as space based detectors like LISA.
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inspiralling compact binaries in quasi Elliptical Orbits the complete third post newtonian energy flux
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The instantaneous contributions to the third post-Newtonian (3PN) gravitational wave luminosity from the inspiral phase of a binary system of compact objects moving in a quasi-Elliptical orbit is computed using the multipolar post-Minkowskian wave generation formalism. The necessary inputs for this calculation include the 3PN accurate mass quadrupole moment for general Orbits and the mass octupole and current quadrupole moments at 2PN. Using the recently obtained 3PN quasi-Keplerian representation of Elliptical Orbits, the flux is averaged over the binary's orbit. Supplementing this by the important hereditary contributions arising from tails, tails of tails, and tails-squared terms calculated in a previous paper, the complete 3PN energy flux is obtained. The final result presented in this paper would be needed for the construction of ready-to-use templates for binaries moving on noncircular Orbits, a plausible class of sources not only for the space-based detectors like LISA but also for the ground-based ones.
Bala R. Iyer - One of the best experts on this subject based on the ideXlab platform.
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Third post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact binaries in quasi-Elliptical Orbits
Physical Review D, 2009Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Siddhartha SinhaAbstract:The angular momentum flux from an inspiralling binary system of compact objects moving in quasi-Elliptical Orbits is computed at the third post-Newtonian (3PN) order using the multipolar post-Minkowskian wave generation formalism. The 3PN angular momentum flux involves the instantaneous, tail, and tail-of-tails contributions as for the 3PN energy flux, and in addition a contribution due to non-linear memory. We average the angular momentum flux over the binary's orbit using the 3PN quasi-Keplerian representation of Elliptical Orbits. The averaged angular momentum flux provides the final input needed for gravitational wave phasing of binaries moving in quasi-Elliptical Orbits. We obtain the evolution of orbital elements under 3PN gravitational radiation reaction in the quasi-elliptic case. For small eccentricities, we give simpler limiting expressions relevant for phasing up to order $e^2$. This work is important for the construction of templates for quasi-eccentric binaries, and for the comparison of post-Newtonian results with the numerical relativity simulations of the plunge and merger of eccentric binaries.
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tail effects in the third post newtonian gravitational wave energy flux of compact binaries in quasi Elliptical Orbits
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The far-zone flux of energy contains hereditary (tail) contr ibutions that depend on the entire past history of the source. Using the multipolar post-Minkowskian wave generation formalism, we propose and implement a semi-analytical method in the frequency domain to compute these contributions from the inspiral phase of a binary system of compact objects moving in quasi-Elliptical Orbits up to third post-Newtonian (3PN) order. The method explicitly uses the quasi-Keplerian representation of Elliptical Orbits at 1PN order and exploits the doubly periodic nature of the motion to average the 3PN flu xes over the binary’s orbit. Together with the instantaneous (non-tail) contributions evaluated in a companion paper, it provides crucial inputs for the construction of ready-to-use templates for compact binaries moving on quasi-elliptic Orbits, an interesting class of sources for the ground based gravitational wave detectors such as LIGO and Virgo as well as space based detectors like LISA.
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inspiralling compact binaries in quasi Elliptical Orbits the complete third post newtonian energy flux
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The instantaneous contributions to the third post-Newtonian (3PN) gravitational wave luminosity from the inspiral phase of a binary system of compact objects moving in a quasi-Elliptical orbit is computed using the multipolar post-Minkowskian wave generation formalism. The necessary inputs for this calculation include the 3PN accurate mass quadrupole moment for general Orbits and the mass octupole and current quadrupole moments at 2PN. Using the recently obtained 3PN quasi-Keplerian representation of Elliptical Orbits, the flux is averaged over the binary's orbit. Supplementing this by the important hereditary contributions arising from tails, tails of tails, and tails-squared terms calculated in a previous paper, the complete 3PN energy flux is obtained. The final result presented in this paper would be needed for the construction of ready-to-use templates for binaries moving on noncircular Orbits, a plausible class of sources not only for the space-based detectors like LISA but also for the ground-based ones.
Luc Blanchet - One of the best experts on this subject based on the ideXlab platform.
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Third post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact binaries in quasi-Elliptical Orbits
Physical Review D, 2009Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Siddhartha SinhaAbstract:The angular momentum flux from an inspiralling binary system of compact objects moving in quasi-Elliptical Orbits is computed at the third post-Newtonian (3PN) order using the multipolar post-Minkowskian wave generation formalism. The 3PN angular momentum flux involves the instantaneous, tail, and tail-of-tails contributions as for the 3PN energy flux, and in addition a contribution due to non-linear memory. We average the angular momentum flux over the binary's orbit using the 3PN quasi-Keplerian representation of Elliptical Orbits. The averaged angular momentum flux provides the final input needed for gravitational wave phasing of binaries moving in quasi-Elliptical Orbits. We obtain the evolution of orbital elements under 3PN gravitational radiation reaction in the quasi-elliptic case. For small eccentricities, we give simpler limiting expressions relevant for phasing up to order $e^2$. This work is important for the construction of templates for quasi-eccentric binaries, and for the comparison of post-Newtonian results with the numerical relativity simulations of the plunge and merger of eccentric binaries.
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tail effects in the third post newtonian gravitational wave energy flux of compact binaries in quasi Elliptical Orbits
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The far-zone flux of energy contains hereditary (tail) contr ibutions that depend on the entire past history of the source. Using the multipolar post-Minkowskian wave generation formalism, we propose and implement a semi-analytical method in the frequency domain to compute these contributions from the inspiral phase of a binary system of compact objects moving in quasi-Elliptical Orbits up to third post-Newtonian (3PN) order. The method explicitly uses the quasi-Keplerian representation of Elliptical Orbits at 1PN order and exploits the doubly periodic nature of the motion to average the 3PN flu xes over the binary’s orbit. Together with the instantaneous (non-tail) contributions evaluated in a companion paper, it provides crucial inputs for the construction of ready-to-use templates for compact binaries moving on quasi-elliptic Orbits, an interesting class of sources for the ground based gravitational wave detectors such as LIGO and Virgo as well as space based detectors like LISA.
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inspiralling compact binaries in quasi Elliptical Orbits the complete third post newtonian energy flux
Physical Review D, 2008Co-Authors: K. G. Arun, Luc Blanchet, Bala R. Iyer, Mohd S S QusailahAbstract:The instantaneous contributions to the third post-Newtonian (3PN) gravitational wave luminosity from the inspiral phase of a binary system of compact objects moving in a quasi-Elliptical orbit is computed using the multipolar post-Minkowskian wave generation formalism. The necessary inputs for this calculation include the 3PN accurate mass quadrupole moment for general Orbits and the mass octupole and current quadrupole moments at 2PN. Using the recently obtained 3PN quasi-Keplerian representation of Elliptical Orbits, the flux is averaged over the binary's orbit. Supplementing this by the important hereditary contributions arising from tails, tails of tails, and tails-squared terms calculated in a previous paper, the complete 3PN energy flux is obtained. The final result presented in this paper would be needed for the construction of ready-to-use templates for binaries moving on noncircular Orbits, a plausible class of sources not only for the space-based detectors like LISA but also for the ground-based ones.