Catalog of Nearby Exoplanets

Butler, R. Paul; Wright, Jason T.; Marcy, Geoffrey W.; Fischer, Debra A.; Vogt, S. S.; Tinney, C. G.; Jones, H. R. A.; Carter, B. D.; Johnson, John Asher; McCarthy, C.; Penny, A. J.

doi:10.1086/504701

Cited by 871 publications

(1,216 citation statements)

References 105 publications

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“…We adopted the size distribution from the outer disk simulation and calculated the thermal emission of the dust. The orbital solutions for the inner planet found by Benedict et al (2006) (e = 0.7) and Butler et al (2006) (e = 0.25) have little influence on the SED. In both cases one can match the Spitzer/IRS spectrum with nearly the same dust mass of ≈ 10 −7 M ⊕ for the inner disk.…”

Section: Reidemeister Et Almentioning

confidence: 89%

Warm dust around ϵ Eridani

et al. 2010

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Abstract. ε Eridani hosts one known inner planet and an outer Kuiper belt analog. Further, Spitzer/IRS measurements indicate that warm dust is present at distances as close as a few AU from the star. Its origin is puzzling, since an "asteroid belt" that could produce this dust would be unstable because of the inner planet. We tested a hypothesis that the observed warm dust is generated by collisions in the outer belt and is transported inward by P-R drag and strong stellar winds. With numerical simulation we investigated how the dust streams from the outer ring into the inner system, and calculated the thermal emission of the dust. We show that the observed warm dust can indeed stem from the outer belt. Our models reproduce the shape and magnitude of the observed SED from mid-IR to sub-mm wavelengths, as well as the Spitzer/MIPS radial brightness profiles.

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Section: Reidemeister Et Almentioning

confidence: 89%

Warm dust around ϵ Eridani

et al. 2010

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“…Giant planet masses were drawn randomly according to the observed exoplanet mass function (Butler et al 2006) …”

Section: Methodsmentioning

confidence: 99%

“…Despite their large masses, gas giants must form within the few million year lifetime of gaseous disks (Haisch et al The debris disk -terrestrial planet connection 83 2001) and be present during the late phases of terrestrial planet growth. The known extrasolar giant planets have a broad eccentricity distribution (Butler et al 2006) that is quantitatively reproduced if dynamical instabilities occurred in 70-100% of all observed systems (Chatterjee et al 2008;Juric & Tremaine 2008;Raymond et al 2010). The onset of instability may be caused by the changing planet-planet stability criterion as the gas disk dissipates (Iwasaki et al 2001), resonant migration (Adams & Laughlin 2003), or chaotic dynamics (Chambers et al 2006), leading to a phase of planet-planet scattering and the removal of one or more planets from the system by collision or hyperbolic ejection (Rasio & Ford 1996;Weidenschilling & Marzari 1996).…”

Section: Introductionmentioning

confidence: 99%

The debris disk – terrestrial planet connection

et al. 2010

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Abstract. The eccentric orbits of the known extrasolar giant planets provide evidence that most planet-forming environments undergo violent dynamical instabilities. Here, we numerically simulate the impact of giant planet instabilities on planetary systems as a whole. We find that populations of inner rocky and outer icy bodies are both shaped by the giant planet dynamics and are naturally correlated. Strong instabilities -those with very eccentric surviving giant planets -completely clear out their inner and outer regions. In contrast, systems with stable or low-mass giant planets form terrestrial planets in their inner regions and outer icy bodies produce dust that is observable as debris disks at mid-infrared wavelengths. Fifteen to twenty percent of old stars are observed to have bright debris disks (at λ ∼ 70µm) and we predict that these signpost dynamically calm environments that should contain terrestrial planets.

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“…Most affected are the longer period planets whose eccentric orbits can raise their likelihood of transit from a negligible value to a statistically viable number for photometric follow-up. Figure 3 shows the transit probability calculated from orbital parameters provided by Butler et al (2006) for planets with estimates of e and ω (203 planets in total). For the purposes of comparison, we assume a Jupiter and Solar radius for the values of R p and R , respectively, and include a solid line which indicates the transit probability for a circular orbit.…”

Section: Period Dependencementioning

confidence: 99%

Transit Detection of Radial Velocity Planets

Kane

Braun

2008

Proc. IAU

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Abstract.The orbital parameters of extra-solar planets have a significant impact on the probability that the planet will transit the host star. This was recently demonstrated by the transit detection of HD 17156b whose favourable eccentricity and argument of periastron dramatically increased its transit likelihood. We present a study which provides a quantitative analysis of how these two orbital parameters affect the geometric transit probability as a function of period. Further, we apply these results to known radial velocity planets and show that there are unexpectedly high transit probabilities for planets at relatively long periods. For a photometric monitoring campaign which aims to determine if the planet indeed transits, we calculate the significance of a null result and the subsequent constraints that may be applied to orbital parameters. Transit ProbabilityThere have been at least five cases in which planetary transits were detected through photometric follow-up of planets already known via their radial velocity (RV) discoveries. The case of HD 17156b (Barbieri et al. 2007) is of particular interest since it is a 21.2 day period planet which happens to have a large eccentricity (e = 0.67) and an argument of periastron which places the periapsis of its orbit in the direction toward the observer and close to parallel to the line of sight, resulting in an increased transit probability.Recent work by Barnes (2007) and Burke (2008) showed that higher eccentricities of planetary orbits will increase their transit probabilities and, consequently, expected yield for transit surveys. We demonstrate the combined effect of the eccentricity, e, and argument of periastron, ω, on transit probability. As shown by Kane (2007), the place in a planetary orbit where it is possible for a transit to occur (where the planet passes the star-observer plane perpendicular to the planetary orbit) is when ω + f = π/2. The probability of such a transit occurring, P t , is given bywhere R p and R are the radii of the planet and star respectively, and a is the semi-major axis. The orbital configuration, especially with regards to the values of e and ω, plays a major role in determining the likelihood of a planet transiting the parent star.

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Catalog of Nearby Exoplanets

Cited by 871 publications

References 105 publications

Warm dust around ϵ Eridani

Warm dust around ϵ Eridani

The debris disk – terrestrial planet connection

Transit Detection of Radial Velocity Planets

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