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Barry Wardell - One of the best experts on this subject based on the ideXlab platform.
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spin Orbit precession along Eccentric Orbits for extreme mass ratio black hole binaries and its effective one body transcription
Physical Review D, 2017Co-Authors: Chris Kavanagh, Thibault Damour, Donato Bini, Barry Wardell, Seth Hopper, Adrian C OttewillAbstract:In this work we present an analytical gravitational self-force calculation of the spin-Orbit precession along an Eccentric Orbit around a Schwarzschild black hole, following closely the recent prescription of Akcay, Dempsey, and Dolan, giving results to six post-Newtonian orders expanded in small Eccentricity through ${e}^{2}$. We then transcribe this quantity within the effective-one-body (EOB) formalism, thereby determining several new, linear-in-mass-ratio contributions in the post-Newtonian expansion of the spin-Orbit couplings entering the EOB Hamiltonian. Namely, we determine the second gyrogravitomagnetic ratio ${g}_{{S}_{*}}(r,{p}_{r},{p}_{\ensuremath{\phi}})$ up to order ${p}_{r}^{2}/{r}^{4}$ included.
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Scalar self-force for Eccentric Orbits around a Schwarzschild black hole
Physical Review D, 2013Co-Authors: Ian Vega, Barry Wardell, Peter Diener, Samuel Cupp, Roland HaasAbstract:We revisit the problem of computing the self-force on a scalar charge moving along an Eccentric geodesic Orbit around a Schwarzschild black hole. This work extends previous scalar self-force calculations for circular Orbits, which were based on a regular “effective” point-particle source and a full 3D evolution code. We find good agreement between our results and previous calculations based on a (1+1) time-domain code. Finally, our data visualization is unconventional: we plot the self-force through full radial cycles to create “self-force loops,” which reveal many interesting features that are less apparent in standard presentations of Eccentric-Orbit self-force data.
A Jordan - One of the best experts on this subject based on the ideXlab platform.
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hats 59b c a transiting hot jupiter and a cold massive giant planet around a sun like star
The Astronomical Journal, 2018Co-Authors: P Sarkis, Th Henning, J D Hartman, G A Bakos, R Brahm, A Jordan, D BaylissAbstract:We report the first discovery of a multi-planetary system by the HATSouth network, HATS-59b,c, a planetary system with an inner transiting hot Jupiter and an outer cold massive giant planet, which was detected via radial velocity. The inner transiting planet, HATS-59b, is on an Eccentric Orbit with e = 0.129 +/- 0.049, Orbiting a V = 13.951 +/- 0.030 mag solar-like star (M-star = 1.038 +/- 0.039 M-circle dot and R-star = 1.036 +/- 0.067 R-circle dot) with a period of 5.416081 +/- 0.000016 days. The outer companion, HATS-59c is on a circular Orbit with m sin i = 12.70 +/- 0.87 M-J and a period of 1422 +/- 14 days. The inner planet has a mass of 0.806 +/- 0.069 M-J and a radius of 1.126 +/- 0.077 R-J, yielding a density of 0.70 +/- 0.16 g cm(-3). Unlike most planetary systems that include only a single hot Jupiter, HATS-59b, c includes, in addition to the transiting hot Jupiter, a massive outer companion. The architecture of this system is valuable for understanding planet migration.
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hats 59b c a transiting hot jupiter and a cold massive giant planet around a sun like star
arXiv: Earth and Planetary Astrophysics, 2018Co-Authors: P Sarkis, Th Henning, J D Hartman, G A Bakos, R Brahm, A Jordan, D BaylissAbstract:We report the first discovery of a multi-planetary system by the HATSouth network, HATS-59b,c, a planetary system with an inner transiting hot Jupiter and an outer cold massive giant planet, which was detected via radial velocity. The inner transiting planet, HATS-59b, is on an Eccentric Orbit with $e = 0.129\pm0.049$, Orbiting a $V=13.951\pm0.030$ mag solar-like star ($M_* = 1.038\pm0.039 M_{\odot}$, and $R_* = 1.036\pm0.067 R_{\odot}$) with a period of $5.416077\pm0.000017$ days. The outer companion, HATS-59c is on a circular Orbit with $ m \sin i = 12.8\pm1.1 M_\mathrm{J}$, and a period of $1422\pm14$ days. The inner planet has a mass of $0.806\pm0.069 M_\mathrm{J}$ and a radius of $1.126\pm0.077 M_\mathrm{J}$, yielding a density of $0.70\pm0.16 {\rm g\,cm^{-3}}$. Unlike most of the planetary systems that include only a single hot Jupiter, HATS-59b,c includes, in addition to the transiting hot Jupiter, a massive outer companion. The architecture of this system is valuable for understanding planet migration.
G Hebrard - One of the best experts on this subject based on the ideXlab platform.
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WASP-54b, WASP-56b, and WASP-57b: Three new sub-Jupiter mass planets from SuperWASP
2013Co-Authors: F Faedi, D. Pollacco, S. C. C. Barros, D. Brown, A. C. Cameron, A. P. Doyle, R. Enoch, M. Gillon, Y. G. M. Chew, G HebrardAbstract:We present three newly discovered sub-Jupiter mass planets from the SuperWASP survey: WASP-54b is a heavily bloated planet of mass 0.636[Superscript: +0.025][Subscript: -0.024]MJ and radius 1.653[Superscript: +0.090][Subscript: -0.083]RJ. It Orbits a F9 star, evolving off the main sequence, every 3.69 days. Our MCMC fit of the system yields a slightly Eccentric Orbit (e = 0.067[Superscript: +0.033][Subscript: -0.025]) for WASP-54b. We investigated further the veracity of our detection of the Eccentric Orbit for WASP-54b, and we find that it could be real. However, given the brightness of WASP-54 V = 10.42 mag, we encourage observations of a secondary eclipse to draw robust conclusions on both the Orbital Eccentricity and the thermal structure of the planet. WASP-56b and WASP-57b have masses of 0.571[Superscript: +0.034][Subscript: -0.035]MJ and 0.672[Superscript: +0.049][Subscript: -0.046]MJ, respectively; and radii of 1.092[Superscript: +0.035][Subscript: -0.033]RJ for WASP-56b and 0.916[Superscript: +0.017][Subscript: -0.014]RJ for WASP-57b. They Orbit main sequence stars of spectral type G6 every 4.67 and 2.84 days, respectively. WASP-56b and WASP-57b show no radius anomaly and a high density possibly implying a large core of heavy elements; possibly as high as ~50 M⊕ in the case of WASP-57b. However,the composition of the deep interior of exoplanets remains still undetermined. Thus, more exoplanet discoveries such as the ones presented in this paper, are needed to understand and constrain giant planets’ physical properties
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Orbital Eccentricity of wasp 12 and wasp 14 from new radial velocity monitoring with sophie
Monthly Notices of the Royal Astronomical Society, 2011Co-Authors: Nawal Husnoo, F Bouchy, C Moutou, G Hebrard, F Pont, E K Simpson, T Mazeh, L ArnoldAbstract:As part of the long-term radial velocity monitoring of known transiting planets, we have acquired new radial velocity data for the two transiting systems WASP-12 and WASP-14, each harbouring a gas giant on a close Orbit (Orbital period of 1.09 and 2.24 d, respectively). In both cases, the initial Orbital solution suggested a significant Orbital Eccentricity, 0.049 +/- 0.015 for WASP-12b and 0.091 +/- 0.003 for WASP-14b. Since then, measurements of the occultation of WASP-12 in the infrared have indicated that one projection of the Eccentricity (e cos omega) was close to zero, casting doubt on the Eccentricity from the initial radial velocity Orbit. Our measurements show that the radial velocity data are compatible with a circular Orbit. A MCMC analysis taking into account the presence of correlated systematic noise in both the radial velocity and photometric data gives e = 0.017+0.015(-0.010). In contrast, we confirm the Orbital Eccentricity of WASP-14b, and refine its value to e = 0.0877 +/- 0.0030, a 10 Sigma detection. WASP-14b is thus the closest presently known planet with a confirmed Eccentric Orbit.
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misaligned spin Orbit in the xo 3 planetary system
Astronomy and Astrophysics, 2008Co-Authors: G Hebrard, X Bonfils, F Bouchy, C Moutou, F Pont, B Loeillet, M Rabus, I BoisseAbstract:The transiting extrasolar planet XO-3b is remarkable, with a high mass and Eccentric Orbit. These unusual characteristics make it interesting to test whether its Orbital plane is parallel to the equator of its host star, as it is observed for other transiting planets. We performed radial velocity measurements of XO-3 with the SOPHIE spectrograph at the 1.93 m telescope of Haute-Provence Observatory during a planetary transit and at other Orbital phases. This allowed us to observe the Rossiter-McLaughlin effect and, together with a new analysis of the transit light curve, to refine the parameters of the planet. The unusual shape of the radial velocity anomaly during the transit provides a hint of a nearly transverse Rossiter-McLaughlin effect. The sky-projected angle between the planetary Orbital axis and the stellar rotation axis should be λ = 70 ◦ ± 15 ◦ to be compatible with our observations. This suggests that some close-in planets might result from gravitational interaction between planets and/or stars rather than migration due to interaction with the accretion disk. This surprising result requires confirmation by additional observations, especially at lower airmass, to fully exclude the possibility that the signal is due to systematic effects.
Donato Bini - One of the best experts on this subject based on the ideXlab platform.
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Spin-Orbit precession along Eccentric Orbits: improving the knowledge of self-force corrections and of their effective-one-body counterparts
Phys.Rev.D, 2018Co-Authors: Donato Bini, Thibault Damour, Andrea GeralicoAbstract:The (first-order) gravitational self-force correction to the spin-Orbit precession of a spinning compact body along a slightly Eccentric Orbit around a Schwarzschild black hole is computed through the ninth post-Newtonian order and to second order in the Eccentricity, improving recent results by Kavanagh et al. [Phys. Rev. D 96, 064012 (2017)10.1103/PhysRevD.96.064012]. We show that our higher-accurate theoretical estimates of the spin precession exhibits an improved agreement with corresponding numerical self-force data. We convert our new theoretical results into its corresponding effective-one-body counterpart, thereby determining several new post-Newtonian terms in the gyrogravitomagnetic ratio gS*.
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spin Orbit precession along Eccentric Orbits for extreme mass ratio black hole binaries and its effective one body transcription
Physical Review D, 2017Co-Authors: Chris Kavanagh, Thibault Damour, Donato Bini, Barry Wardell, Seth Hopper, Adrian C OttewillAbstract:In this work we present an analytical gravitational self-force calculation of the spin-Orbit precession along an Eccentric Orbit around a Schwarzschild black hole, following closely the recent prescription of Akcay, Dempsey, and Dolan, giving results to six post-Newtonian orders expanded in small Eccentricity through ${e}^{2}$. We then transcribe this quantity within the effective-one-body (EOB) formalism, thereby determining several new, linear-in-mass-ratio contributions in the post-Newtonian expansion of the spin-Orbit couplings entering the EOB Hamiltonian. Namely, we determine the second gyrogravitomagnetic ratio ${g}_{{S}_{*}}(r,{p}_{r},{p}_{\ensuremath{\phi}})$ up to order ${p}_{r}^{2}/{r}^{4}$ included.
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confirming and improving post newtonian and effective one body results from self force computations along Eccentric Orbits around a schwarzschild black hole
Physical Review D, 2016Co-Authors: Donato Bini, Thibault Damour, Andrea GeralicoAbstract:We analytically compute, through the six-and-a-half post-Newtonian order, the second-order-in-Eccentricity piece of the Detweiler-Barack-Sago gauge-invariant redshift function for a small mass in Eccentric Orbit around a Schwarzschild black hole. Using the first law of mechanics for Eccentric Orbits [A. Le Tiec, First law of mechanics for compact binaries on Eccentric Orbits, Phys. Rev. D 92, 084021 (2015).] we transcribe our result into a correspondingly accurate knowledge of the second radial potential of the effective-one-body formalism [A. Buonanno and T. Damour, Effective one-body approach to general relativistic two-body dynamics, Phys. Rev. D 59, 084006 (1999).]. We compare our newly acquired analytical information to several different numerical self-force data and find good agreement, within estimated error bars. We also obtain, for the first time, independent analytical checks of the recently derived, comparable-mass fourth-post-Newtonian order dynamics [T. Damour, P. Jaranowski, and G. Schaefer, Nonlocal-in-time action for the fourth post-Newtonian conservative dynamics of two-body systems, Phys. Rev. D 89, 064058 (2014).].
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High post-Newtonian order gravitational self-force analytical results for Eccentric equatorial Orbits around a Kerr black hole
Physical Review D, 2016Co-Authors: Donato Bini, Thibault Damour, Andrea GeralicoAbstract:We present the first analytic computation of the Detweiler-Barack-Sago gauge-invariant redshift function for a small mass in {\it Eccentric} Orbit around a {\it spinning} black hole. Our results give the redshift contributions that mix Eccentricity and spin effects, through second order in Eccentricity, second order in spin parameter, and the eight-and-a-half post-Newtonian order.
D Bayliss - One of the best experts on this subject based on the ideXlab platform.
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hats 59b c a transiting hot jupiter and a cold massive giant planet around a sun like star
The Astronomical Journal, 2018Co-Authors: P Sarkis, Th Henning, J D Hartman, G A Bakos, R Brahm, A Jordan, D BaylissAbstract:We report the first discovery of a multi-planetary system by the HATSouth network, HATS-59b,c, a planetary system with an inner transiting hot Jupiter and an outer cold massive giant planet, which was detected via radial velocity. The inner transiting planet, HATS-59b, is on an Eccentric Orbit with e = 0.129 +/- 0.049, Orbiting a V = 13.951 +/- 0.030 mag solar-like star (M-star = 1.038 +/- 0.039 M-circle dot and R-star = 1.036 +/- 0.067 R-circle dot) with a period of 5.416081 +/- 0.000016 days. The outer companion, HATS-59c is on a circular Orbit with m sin i = 12.70 +/- 0.87 M-J and a period of 1422 +/- 14 days. The inner planet has a mass of 0.806 +/- 0.069 M-J and a radius of 1.126 +/- 0.077 R-J, yielding a density of 0.70 +/- 0.16 g cm(-3). Unlike most planetary systems that include only a single hot Jupiter, HATS-59b, c includes, in addition to the transiting hot Jupiter, a massive outer companion. The architecture of this system is valuable for understanding planet migration.
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hats 59b c a transiting hot jupiter and a cold massive giant planet around a sun like star
arXiv: Earth and Planetary Astrophysics, 2018Co-Authors: P Sarkis, Th Henning, J D Hartman, G A Bakos, R Brahm, A Jordan, D BaylissAbstract:We report the first discovery of a multi-planetary system by the HATSouth network, HATS-59b,c, a planetary system with an inner transiting hot Jupiter and an outer cold massive giant planet, which was detected via radial velocity. The inner transiting planet, HATS-59b, is on an Eccentric Orbit with $e = 0.129\pm0.049$, Orbiting a $V=13.951\pm0.030$ mag solar-like star ($M_* = 1.038\pm0.039 M_{\odot}$, and $R_* = 1.036\pm0.067 R_{\odot}$) with a period of $5.416077\pm0.000017$ days. The outer companion, HATS-59c is on a circular Orbit with $ m \sin i = 12.8\pm1.1 M_\mathrm{J}$, and a period of $1422\pm14$ days. The inner planet has a mass of $0.806\pm0.069 M_\mathrm{J}$ and a radius of $1.126\pm0.077 M_\mathrm{J}$, yielding a density of $0.70\pm0.16 {\rm g\,cm^{-3}}$. Unlike most of the planetary systems that include only a single hot Jupiter, HATS-59b,c includes, in addition to the transiting hot Jupiter, a massive outer companion. The architecture of this system is valuable for understanding planet migration.