Direct Imaging of Multiple Planets Orbiting the Star HR 8799

Marois, Christian; Macintosh, Bruce; Barman, Travis; Zuckerman, B.; Song, Inseok; Patience, Jennifer; Lafrenière, David; Doyon, René

doi:10.1126/science.1166585

Cited by 1,714 publications

(2,185 citation statements)

References 40 publications

(55 reference statements)

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“…The fragment contracts, and eventually evolves to become a giant planet. Numerical investigations suggest that planets in wide orbits, such as those recently observed by direct imaging (Marois et al 2008), could form by disk instability.…”

Section: Gravitational Instabilitymentioning

confidence: 99%

Composition of massive giant planets

Helled

Bodenheimer

Lissauer³

2010

Proc. IAU

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Abstract. The two current models for giant planet formation are core accretion and disk instability. We discuss the core masses and overall planetary enrichment in heavy elements predicted by the two formation models, and show that both models could lead to a large range of final compositions. For example, both can form giant planets with nearly stellar compositions. However, low-mass giant planets, enriched in heavy elements compared to their host stars, are more easily explained by the core accretion model. The final structure of the planets, i.e., the distribution of heavy elements, is not firmly constrained in either formation model.

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Section: Gravitational Instabilitymentioning

confidence: 99%

Composition of massive giant planets

Helled

Bodenheimer

Lissauer³

2010

Proc. IAU

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“…The objects included 3 planets about 60 million years old orbiting the star HR 8799 (ref. 7), and a single planet more than 100 million years old orbiting Fomalhaut (ref. 8), a bright star some 8 parsecs from Earth.…”

Section: Direct Imagingmentioning

confidence: 99%

The truth about exoplanets

Hecht¹

2016

Nature

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“…• Planets orbiting pulsating A stars: Near-diffraction-limited, infrared adaptiveoptics imaging instruments such as GPI , SPHERE (Beuzit et al, 2008) and SCExAO (Guyon et al, 2010) will soon provide an increasing number of directly imaged planets orbiting young stars, including pulsating A stars such as HR 8799 (Zerbi et al, 1999;Marois et al, 2008). A common limitation for interpreting these discoveries is their unknown age, which is needed to determine whether the detected substellar companions are indeed planets.…”

Section: Future Prospectsmentioning

confidence: 99%

Synergies Between Asteroseismology and Exoplanetary Science

Huber

2017

Astrophysics and Space Science Proceedings

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Over the past decade asteroseismology has become a powerful method to systematically characterize host stars and dynamical architectures of exoplanet systems. In this contribution I review current key synergies between asteroseismology and exoplanetary science such as the precise determination of planet radii and ages, the measurement of orbital eccentricities, stellar obliquities and their impact on hot Jupiter formation theories, and the importance of asteroseismology on spectroscopic analyses of exoplanet hosts. I also give an outlook on future synergies such as the characterization of sub-Neptune-size planets orbiting solar-type stars, the study of planet populations orbiting evolved stars, and the determination of ages of intermediate-mass stars hosting directly imaged planets.

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Direct Imaging of Multiple Planets Orbiting the Star HR 8799

Cited by 1,714 publications

References 40 publications

Composition of massive giant planets

Composition of massive giant planets

The truth about exoplanets

Synergies Between Asteroseismology and Exoplanetary Science

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