HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star

By Gáspár Á. Bakos, G. Kovacs, G. Torres, Debra A. Fischer, D. Latham, R. W. Noyes, D. Sasselov, T. Mazeh, Avi Shporer, R. P. Butler and 11 more. 2007

170 citations recorded by the source corpus.

We report the discovery of a massive (Mp = 9.04 ± 0.50 MJ) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341 ± 0.00013 days and an eccentricity of e = 0.520 ± 0.010. From the transit light curve we determine that the radius of the planet is Rp = 0.982 RJ. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously known transiting exoplanets and a density of ρp ≈ 12 g cm-3, greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and accounting for them may require a large (≳100 M⊕) core. The high eccentricity causes a ninefold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is Tmid = 2,454,212.8559 ± 0.0007 (HJD) and the transit duration is 0.177 ± 0.002 days.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a20847702388fe321f8683aa7c33899dacdaebe2

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In Astronomy and Astrophysics

1. Jon Fortney
2. D. Charbonneau
3. J. Southworth
4. J. Winn
5. N. Madhusudhan
6. J. Johnson
7. Sara Seager
8. A. Showman

Citations in the corpus

• The 3.6-8.0 μm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion (2007, background): “The planet HATP-1b (Bakos et al. 2007a) was initially thought to share this property as well, but subsequent observations (Winn et al. 2007) revealed that its radius was smaller than initially estimated.”
• ORBITAL PHASE VARIATIONS OF THE ECCENTRIC GIANT PLANET HAT-P-2b (2013, methodology): “Rapidly rotating stars are known to have an increased scatter in their RV velocity distribution beyond the reported internal errors (as discussed in Bakos et al. 2007b; Winn et al. 2007a).”
• HAT-P-11b: A SUPER-NEPTUNE PLANET TRANSITING A BRIGHT K STAR IN THE KEPLER FIELD (2009, methodology): “We have carried out an analysis of the bisector span based on the Keck spectra as described in earlier HATNet detection papers (see Bakos et al. 2007a), and do not see any statistically significant correlation between the line bisector spans and the measured radial velocities (confer Fig.”
• DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205 (2009, background): “Subsequent follow-up observations showed that HTR205-023 is the star hosting a transiting planet (Bakos et al. 2007b), not HTR205022.”
• Tidal Heating of Extrasolar Planets (2008, background): “HAT-P-1b is also larger than predicted by theory (Bakos et al. 2007a).”
• HAT-P-16b: A 4 MJ PLANET TRANSITING A BRIGHT STAR ON AN ECCENTRIC ORBIT, (2010, methodology): “The bisector analysis was performed on the Keck spectra as described in § 5 of Bakos et al. (2007a); the spectra from the NOT were analyzed in a similar manner.”
• Misaligned spin-orbit in the XO-3 planetary system?† (2008, background): “Among the forty transiting extra-solar planets known to date, XO-3b is particular as it is among the few on an eccentric orbit, together with HD 147506b (Bakos et al. 2007), HD 17156b (Fischer et al. 2007; Barbieri et al. 2007), and GJ 436b (Butler et al. 2004; Gillon et al. 2007).”
• Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “Two other examples are WASP-1b (Cameron et al. 2007) and HAT-P-1b (Bakos et al. 2007b).”
• Tidal Evolution of Close-in Extrasolar Planets (2007, background): “Planetary data were taken from a variety of sources: Bakos et al. 2007a; Bakos et al. 2007b; Butler et al. 2006; Da Silva et al. 2006; Deming et al. 2007; Gillon et al. 2007; Johnson et al. 2006; Knutson et al. 2007; Laughlin et al. 2005; Lovis et al. 2006; McArthur et al. 2004; Maness 2007; Mayor…”
• EVIDENCE OF POSSIBLE SPIN–ORBIT MISALIGNMENT ALONG THE LINE OF SIGHT IN TRANSITING EXOPLANET SYSTEMS (2010, background): “HAT-P-2 has been observed to have a large radial velocity jitter, which may indicate an active and possibly quickly rotating star (Bakos et al. 2007a).”
• Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution (2009, background): “Internal structure models (Baraffe et al. 2008) do however require comparable amounts of heavy elements to reproduced the observed mass-radius relation of the transiting “Hot Super Jupiter” HD 147506b (Bakos et al. 2007).”
• Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, methodology): “My ABSDIM solutions prefer theTeff value used in Paper II (Bakos et al. 2007a) to the higher one found by Ammler-von Eiff et al. (2009).”
• Extrasolar planet population synthesis - II. Statistical comparison with observations (2009, background): “In any case, these planets which start their formation inside the iceline in extremely metal rich disks ([Fe/H]& 0.4 and Σ0 & 800 g/cm2) are extreme in terms of composition also: They typically have a Mheavy of 100-200 M⊕ and MZ,tot of 200-800 M⊕, reminiscent of the internal composition deduced by B”
• A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres (2007, methodology): “For comparison we also plot a pL Class model for potential transition object HAT-P-1b (Bakos et al. 2007b; Winn et al. 2007), which transits one member of a main sequence G star binary system.”