Giant planet companion to 2MASSW J1207334-393254

Chauvin, G.; Lagrange, A.-M.; Dumas, Christophe; Zuckerman, B.; Mouillet, D.; Song, Inseok; Beuzit, J. L.; Lowrance, P.

doi:10.1051/0004-6361:200500116

Cited by 303 publications

(325 citation statements)

References 29 publications

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“…Finally, we note that given the large physical separations of the objects discovered by Chauvin et al (2004) and Neuhäuser et al (2005) from their parent stars, it is unlikely that these particular objects formed via the core accretion-gas capture method. This indeed causes some to claim these objects are not "planets" at all, which remains a point of active discussion.…”

Section: Other Detectability Issuesmentioning

confidence: 93%

“…Now, ten years after the disovery of the first extrasolar giant planet (EGP), this era is apparently now at hand. The two major discoveries to date are those of Chauvin et al (2004Chauvin et al ( , 2005, who discovered an object of 5 ± 2 M J in orbit around a 25 M J brown dwarf (2M1207), and Neuhäuser et al (2005), who discovered a ∼1 -42 M J companion to the T Tauri star GQ Lup. Both of these systems are quite young, with ages estimated to be ∼10 Myr for 2M1207 and ∼2 Myr for GQ Lup.…”

Section: Introductionmentioning

confidence: 99%

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Young Jupiters are faint: new models of the early evolution of giant planets

Fortney¹,

Marley

Hubickyj

et al. 2005

Astron Nachr

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Abstract.Here we show preliminary calculations of the cooling and contraction of a 2 MJ planet. These calculations, which are being extended to 1-10 MJ, differ from other published "cooling tracks" in that they include a core accretion-gas capture formation scenario, the leading theory for the formation of gas giant planets. We find that the initial post-accretionary intrinsic luminosity of the planet is ∼3 times less than previously published models which use arbitrary initial conditions. These differences last a few tens of millions of years. Young giant planets are intrinsically fainter than has been previously appreciated. We also discuss how uncertainties in atmospheric chemistry and the duration of the formation time of giant planets lead to challenges in deriving planetary physical properties from comparison with tabulated model values.

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Section: Other Detectability Issuesmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Young Jupiters are faint: new models of the early evolution of giant planets

Fortney¹,

Marley

Hubickyj

et al. 2005

Astron Nachr

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“…The discovery of planetary systems by direct imaging nowadays is restricted to large separations >10−100 AU (Veras et al 2009) and favors higher mass planets. As of today nine exoplanetary systems have been directly imaged in the optical or near-infrared band, but only five of them are still embedded: GQ Lup (Neuhäuser et al 2005) and CT Cha (Schmidt et al 2008), but they are rather hosting a stellar companion as the companion masses are, because high as 21.5 M J and 17 M J , respectively; 2M1207 (Chauvin et al 2004(Chauvin et al , 2005a) hosting a 4 M J mass planet; UScoCTIO 108 (Kashyap et al 2008) hosting a 14 M J mass planet; β Pic (Lagrange et al 2009a,b) hosting an 8 M J mass planet. AB Pic (Chauvin et al 2005b), HR 8799 (Marois et al 2008) (triple system), SR 1845 (Biller et al 2006) and Fomalhaut (Kalas et al 2008) are mature planetary systems with ages of about 30 Myr, 60 Myr, 100 Myr, and 200 Myr.…”

Section: Introductionmentioning

confidence: 99%

Detectability of giant planets in protoplanetary disks by CO emission lines

Regály

Sándor

Dullemond

et al. 2010

A&A

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Context. Planets are thought to form in protoplanetary accretion disks around young stars. Detecting a giant planet still embedded in a protoplanetary disk would be very important and give observational constraints on the planet-formation process. However, detecting these planets with the radial velocity technique is problematic owing to the strong stellar activity of these young objects. Aims. We intend to provide an indirect method to detect Jovian planets by studying near infrared emission spectra originating in the protoplanetary disks around T Tauri stars. Our idea is to investigate whether a massive planet could induce any observable effect on the spectral lines emerging in the disks atmosphere. As a tracer molecule we propose CO, which is excited in the ro-vibrational fundamental band in the disk atmosphere to a distance of ∼2−3 AU (depending on the stellar mass) where terrestrial planets are thought to form. Methods. We developed a semi-analytical model to calculate synthetic molecular spectral line profiles in a protoplanetary disk using a double layer disk model heated on the outside by irradiation by the central star and in the midplane by viscous dissipation due to accretion. 2D gas dynamics were incorporated in the calculation of synthetic spectral lines. The motions of gas parcels were calculated by the publicly available hydrodynamical code FARGO which was developed to study planet-disk interactions. Results. We demonstrate that a massive planet embedded in a protoplanetary disk strongly influences the originally circular Keplerian gas dynamics. The perturbed motion of the gas can be detected by comparing the CO line profiles in emission, which emerge from planet-bearing to those of planet-free disk models. The planet signal has two major characteristics: a permanent line profile asymmetry, and short timescale variability correlated with the orbital phase of the giant planet. We have found that the strength of the asymmetry depends on the physical parameters of the star-planet-disk system, such as the disk inclination angle, the planetary and stellar masses, the orbital distance, and the size of the disk inner cavity. The permanent line profile asymmetry is caused by a disk in an eccentric state in the gap opened by the giant planet. However, the variable component is a consequence of the local dynamical perturbation by the orbiting giant planet. We show that a forming giant planet, still embedded in the protoplanetary disk, can be detected using contemporary or future high-resolution near-IR spectrographs like VLT/CRIRES and ELT/METIS.

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“…Chauvin et al 2005, Close et al 2004). Atmospheric models of giant planets will then have been partly constrained by observations.…”

Section: Planet Finding With Vlt-pfmentioning

confidence: 99%

Science case for VLT-Planet Finder

Moutou¹,

Beuzit²,

Gratton³

et al. 2005

Proc. IAU

Self Cite

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Abstract. This paper presents the scientific case for a next generation adaptive optics instrument at the VLT, temporarily named "Planet Finder", that is aimed at detecting and characterizing extrasolar planets through the direct analysis of their emitted photons in the visible and at near-IR wavelengths. We discuss the observational niche of such an instrument to have first light in 2010, in complement to other planet search methods. To improve the efficiency (and consistency) of the search for planets with the PF, the observations will need to be organized in the form of an extensive survey of hundreds of nearby stars, predicted outputs of which are also described here. This summarizes the study phase of the instrument, conducted by two competitive teams and the recent merging of both studies, regarding the scientific impact of Planet Finder.

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Giant planet companion to 2MASSW J1207334-393254

Cited by 303 publications

References 29 publications

Young Jupiters are faint: new models of the early evolution of giant planets

Young Jupiters are faint: new models of the early evolution of giant planets

Detectability of giant planets in protoplanetary disks by CO emission lines

Science case for VLT-Planet Finder

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