The physical properties of extra-solar planets
By Isabelle Baraffe, G. Chabrier, Travis S. Barman. 2010
163 citations recorded by the source corpus.
Tremendous progress in the science of extrasolar planets has been achieved since the discovery of a Jupiter orbiting the nearby Sun-like star 51 Pegasi in 1995. Theoretical models have now reached enough maturity to predict the characteristic properties of these new worlds, mass, radius, atmospheric signatures, and can be confronted with available observations. We review our current knowledge of the physical properties of exoplanets, internal structure and composition, atmospheric signatures, including expected biosignatures for exo-Earth planets, evolution, and the impact of tidal interaction and stellar irradiation on these properties for the short-period planets. We discuss the most recent theoretical achievements in the field and the still pending questions. We critically analyze the different solutions suggested to explain abnormally large radii of a significant fraction of transiting exoplanets. Special attention is devoted to the recently discovered transiting objects in the overlapping mass range between massive planets and low-mass brown dwarfs, stressing the ambiguous nature of these bodies, and we discuss the possible observable diagnostics to identify these two distinct populations. We also review our present understanding of planet formation and critically examine the different suggested formation mechanisms. We expect this review will provide the basic theoretical background to capture the essentials of the physics of exoplanet formation, structure and evolution and the related observable signatures.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/caeecb92637d21cd1960297f62eaac8d11ac81ed
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In Astronomy and Astrophysics
Citations in the corpus
- Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity (2010, background): “…to affect the planet’s inner isentrope, or inefficient large-scale convection due to a composition gradient (Chabrier & Baraffe 2007) could be the other mechanisms to be considered with tidal dissipation to lead eventually to these large planet radii (see Baraffe et al. (2010) for discussion).”
- Defining and cataloging exoplanets: the exoplanet.eu database (2011, background): “Unfortunately there is an overlap in the guessed mass distribution of planets and brown dwarfs (Baraffe et al. 2010; Spiegel et al. 2011).”
- The Properties of Hydrogen and Helium Under Extreme Conditions (2011, background): “For example, they form from 70% − 95% of the mass of Jupiter and Saturn in our own solar system, as well as being the principle components of a large number of recently discovered exo-planets (Baraffe et al., 2010).”
- Photoevaporation and high-eccentricity migration created the sub-Jovian desert (2018, background): “Hot Jupiters are known to have inflated radii (e.g. Baraffe et al. 2010; Enoch, Collier Cameron, & Horne 2012; Thorngren & Fortney 2018); the origin of this inflation remains unknown.”
- INFLATING HOT JUPITERS WITH OHMIC DISSIPATION (2010, background): “It has been shown that the required powers are rather modest (Burrows et al. 2007), but it is unlikely that any of the proposed solutions alone are able to account for all observed radii (Baraffe et al. 2010; Fortney & Nettelmann 2009).”
- Precise Radial Velocities of Giant Stars VII. Occurrence Rate of Giant Extrasolar Planets as a Function of Mass and Metallicity (2014, background): “However, taking also the formation scenario into account, one might want to include objects in the mass range from roughly 13 to 25–30 MJup among the planet category, especially those which formed around stars more massive than 1 M (see e.g. Baraffe et al. 2010; Schneider et al. 2011).”
- ON THE ANOMALOUS RADII OF THE TRANSITING EXTRASOLAR PLANETS (2011, background): “A decade of additional discoveries has made it clear that HD 209458b’s radius anomaly is by no means anomalous, and the status of discussion in the field is well-covered in the recent reviews by Showman et al. (2010), Burrows & Orton (2009), and Baraffe et al. (2010).”
- Characterization of exoplanets from their formation - II. The planetary mass-radius relationship (2012, background): “The reader is referred to Fortney & Nettelmann (2010) or Baraffe et al. (2010) for recent reviews.”
- HST hot-Jupiter transmission spectral survey: evidence for aerosols and lack of TiO in the atmosphere of WASP-12b (2013, background): “Given that WASP12b still has one of the largest radii of any transiting planet, a precise radius for this exoplanet, in particular, is crucial for understanding the hot-Jupiter inflation problem (see Baraffe et al. 2010 for a review and the references therein).”
- A new vision of giant planet interiors: Impact of double diffusive convection (2012, background): “While only the mass of most of these planets can be derived from observations, the mean density can be inferred for about 20% of these objects, as they transit their parent star, constraining the planet’s gross composition (see Baraffe et al. 2010 for a recent review).”
- LACK OF INFLATED RADII FOR KEPLER GIANT PLANET CANDIDATES RECEIVING MODEST STELLAR IRRADIATION (2011, background): “An exhaustive description can be found in, e.g., Fortney & Nettelmann (2010); Baraffe et al. (2010) but none seems to reproduce all planets with inflated radii.”
- DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, background): “The detection and characterization of extrasolar planets is one of the most exciting and fastest growing jmoses@spacescience.org fields in astronomy (e.g., Charbonneau et al. 2007; Marley et al. 2007; Udry et al. 2007; Deming & Seager 2009; Baraffe et al. 2010).”