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

Bakos, G. Á.; Kovács, G.; Torres, Guillermo; Fischer, Debra A.; Latham, David W.; Noyes, R. W.; Sasselov, Dimitar; Mazeh, T.; Shporer, Avi; Butler, R. Paul; Stefanik, R. P.; Fernández, J. M.; Sozzetti, A.; Pál, András; Johnson, J. A.; Marcy, Geoffrey W.; Winn, Joshua N.; Sipőcz, Brigitta; Lázár, J.; Papp, I.; Sári, P.

doi:10.1086/521866

Cited by 207 publications

(225 citation statements)

References 55 publications

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“…Only the properties of HAT-P-2 appear discrepant to a very significant extent. While Bakos et al (2007a) derived an effective temperature of 6290 K for HAT-P-2 and an iron abundance of 0.12 dex, the present work infers a temperature that is higher by 700 K and an iron abundance of 0.49 dex (see Figs. 1a and d).…”

Section: Systematics and Possible Explanationscontrasting

confidence: 57%

“…Bakos et al (2007b), Bakos et al (2007a), Burke et al (2007), Fischer et al (2007), Kovács et al (2007), McCullough et al (2006), Noyes et al (2008), Pál et al (2008), and Sato et al (2005) all of which are referred to , mostly explicitly state the use of the SME (Spectroscopy Made Easy) software (Valenti & Piskunov 1996), which is based on ATLAS model atmospheres. This spectral fitting technique varies the stellar parameters and the abundances of some species to minimize the differences between the synthetic spectra and observed spectrum.…”

Section: Only Few Different Techniquesmentioning

confidence: 99%

“…Half of the studies mentioned in Table 3 are based on spectra taken with the Keck HIRES spectrograph, although with slightly different configurations. Bakos et al (2007b), Bakos et al (2007a), Kovács et al (2007), Noyes et al (2008), and Pál et al (2008) obtained Keck HIRES spectra with a resolving power of λ Δλ = 55 000, while the HIRES spectra used by Sozzetti et al (2007Sozzetti et al ( , 2009a have λ Δλ = 71 000. Burke et al (2007) and McCullough et al (2006) obtained spectra with λ Δλ = 60 000 with the Échelle spectrograph at the Harlan J. Smith telescope.…”

Section: Small Amount Of Variety Between Spectrographs Usedmentioning

confidence: 99%

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A homogeneous spectroscopic analysis of host stars of transiting planets

Eiff

Santos

Sousa

et al. 2009

A&A

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Context. The analysis of transiting extra-solar planets provides an enormous amount of information about the formation and evolution of planetary systems. A precise knowledge of the host stars is necessary to derive the planetary properties accurately. The properties of the host stars, especially their chemical composition, are also of interest in their own right. Aims. Information about planet formation is inferred by, among others, correlations between different parameters such as the orbital period and the metallicity of the host stars. The stellar properties studied should be derived as homogeneously as possible. The present work provides new, uniformly derived parameters for 13 host stars of transiting planets. Methods. Effective temperature, surface gravity, microturbulence parameter, and iron abundance were derived from spectra of both high signal-to-noise ratio and high resolution by assuming iron excitation and ionization equilibria. Results. For some stars, the new parameters differ from previous determinations, which is indicative of changes in the planetary radii. A systematic offset in the abundance scale with respect to previous assessments is found for the TrES and HAT objects. Our abundance measurements are remarkably robust in terms of the uncertainties in surface gravities. The iron abundances measured in the present work are supplemented by all previous determinations using the same analysis technique. The distribution of iron abundance then agrees well with the known metal-rich distribution of planet host stars. To facilitate future studies, the spectroscopic results of the current work are supplemented by the findings for other host stars of transiting planets, for a total dataset of 50 objects.

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Section: Systematics and Possible Explanationscontrasting

confidence: 57%

Section: Only Few Different Techniquesmentioning

confidence: 99%

Section: Small Amount Of Variety Between Spectrographs Usedmentioning

confidence: 99%

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A homogeneous spectroscopic analysis of host stars of transiting planets

Eiff

Santos

Sousa

et al. 2009

A&A

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“…At a semimajor axis of 0.0674 AU we encounter an eccentricity of 0.5171 for HAT-P-2b (Bakos et al 2007). The simulation depicted in Figure 4 produces an exoplanet with a similar orbit; with a=0.034 AU and e=0.62, it is slightly more "extreme" than HAT-P-2b.…”

Section: Comparison With Known Extreme Exoplanetsmentioning

confidence: 84%

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Shara

Hurley

Mardling

2016

ApJ

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Explaining the origin and evolution of exoplanetary hot Jupiters remains a significant challenge. One possible mechanism for the production of hot Jupitersis planet-planet interactions, which produce them from planets born far from their host stars but near their dynamical stability limits. In the much more likely case of planets born far from their dynamical stability limits, can hot Jupiters be formed in star clusters? Our N-body simulations answer this question in the affirmative, and show that hot Jupiter formation is not a rare event, occurring in ∼1% of star cluster planetary systems. We detail three case studies of the dynamics-induced births of hot Jupiters on highly eccentric orbits that can only occur inside star clusters. The hot Jupiters' orbits bear remarkable similarities to those of some of the most extreme exoplanets known: HAT-P-32b, HAT-P-2b, HD 80606b, and GJ 876d. If stellar perturbations formed these hot Jupiters, then our simulations predict that these very hot inner planets are often accompanied by much more distant gas giants in highly eccentric orbits.

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“…The reason is that due to their extreme mass, their a touch is very large (several tenths of an AU) so that it is not clear if they can be classified as "Hot" planets. These planets, which start their formation inside the iceline in extremely metal rich disks ([Fe/H] 0.4 and Σ 0 800 g/cm 2 ), are also extreme in terms of composition: They typically have a M heavy of 100-200 M ⊕ and M Z,tot of 200-800 M ⊕ , reminiscent of the internal composition deduced by Baraffe et al (2008) for HD 147506 b (aka HAT-P-2b, Bakos et al 2007) where a higher disk mass (due to the higher primary mass) could compensate for the lower [Fe/H]. 5.9.5.…”

Section: Heavy Element Content Of "Hot" Planetsmentioning

confidence: 99%

Extrasolar planet population synthesis

Mordasini¹,

Alibert

Benz³

et al. 2009

A&A

341

362

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Context. This is the second paper in a series of papers showing the results of extrasolar planet population synthesis calculations using our extended core accretion model. In the companion paper (Paper I), we presented in detail the methods we use. In subsequent papers, we shall discuss the effect of the host star's mass on the planetary population and the influence of various properties of protoplanetary disks. Aims. In this second paper, we focus on planets orbiting solar-like stars. The goal is to use the main characteristics of the actually observed extrasolar planet population to derive in a statistical manner constraints on the planet formation models. Methods. Drawing initial conditions for our models at random from probability distributions derived as closely as possible from observations, we synthesize a number of planetary populations. By applying an observational detection bias appropriate for radial velocity surveys, we identify the potentially detectable synthetic planets. The properties of these planets are compared in quantitative statistical tests with the properties of a carefully selected sub-population of actually observed extrasolar planets. Results. We use a two dimensional Kolmogorov-Smirnov test to compare the mass-distance distributions of synthetic and observed planets, as well as the one dimensional version of the test to compare the M sin i, the semimajor axis and the [Fe/H] distribution. We find that while many combinations of parameters lead to unacceptable distributions, a number of models can account to a reasonable degree of statistical significance for most of the properties of the observed sample. We concurrently account for many other observed features, e.g. the "metallicity effect". This gives us confidence that our model captures several essential features of giant planet formation. In addition, the fact that many parameter combinations could be rejected indicates that planet population synthesis is indeed a promising approach to constrain formation models. Our simulations allow us also to extract a number of properties of the underlying exoplanet population that are not yet directly detectable. For example, we have derived the planetary initial mass function (PIMF) and have been led to conclude that the planets detected so far represent only the tip of the iceberg (9%) of all the existing planets. The PIMF can also be used to predict how the detectable extrasolar planet population will change as the instrumental precision of radial velocity surveys improves from ∼10 m/s to ∼1 m/s, or even to an extreme precision of 0.1 m/s.

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

Cited by 207 publications

References 55 publications

A homogeneous spectroscopic analysis of host stars of transiting planets

A homogeneous spectroscopic analysis of host stars of transiting planets

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Extrasolar planet population synthesis

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