A companion to AB Pic at the planet/brown dwarf boundary

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

doi:10.1051/0004-6361:200500111

Cited by 232 publications

(228 citation statements)

References 33 publications

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“…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. Note that centimeter wavelength radio observations of a very young (<0.1 Myr) disk around HL Tau, presented by Greaves et al (2008), revealed the possibility of a 12 Jupiter mass giant planet being in formation at ∼75 AU.…”

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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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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“…Known systems with a star similar to the Sun and a planet in an orbit with large a semimajor axis are: GQ Lup (M = 0.8 ± 0.2 M , Seperuelo et al 2008; a P ≈ 100 AU, Neuhäuser et al 2005), 1RXS J160929.1-210524 (M = 0.85 +0.20 −0.10 M ; a P ≈ 330 AU, Lafreniere et al 2008). Also AB Pic has a planet candidate at a separation of ≈258 AU (Chauvin et al 2005). But AB Pic is classified as a dwarf star, similar to many known systems with large semimajor axes.…”

Section: Discussionmentioning

confidence: 99%

Eccentricity evolution in mean motion resonance and non-radial solar wind

Pástor¹,

Klačka²,

Petržala³

et al. 2009

A&A

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Eccentricity evolution of a dust particle in a mean motion orbital resonance with a planet in circular orbit is investigated. The action of solar electromagnetic and corpuscular radiation, including non-radial components of the solar wind velocity, is taken into account. Various types of eccentricity evolution depend on the angle between the radial direction and the direction of the solar wind velocity. The evolution changes at the analytically derived angles. Its application to exosolar systems is included.

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“…It is a probable member of the Tucana-Horologium association with an age of 10-50 Myrs. AB Pic b is a ∼13 M Jupiter mass object at the planet/BD boundary (Chauvin et al 2005b) and separation of 275 AU. It is also member of the Tucana-Horologium association.…”

Section: Datasetmentioning

confidence: 99%

“…Other than a few planets (e.g., Kuzuhara et al 2013;Rameau et al 2013b) and brown dwarfs (BDs; e.g., Chauvin et al 2005b;Biller et al 2010;Mugrauer et al 2010;Wahhaj et al 2011;Carson et al 2013) detected, many surveys found no planetary companions. The null results cannot be used to fit power-laws to the planetary distributions beyond 10 AU.…”

Section: Introductionmentioning

confidence: 99%

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The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

Reggiani

Meyer

Chauvin

et al. 2016

A&A

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Context. In recent years there have been many attempts to characterize the occurrence and distribution of stellar, brown dwarf (BD), and planetary-mass companions to solar-type stars with the aim of constraining formation mechanisms. From radial velocity observations a dearth of companions with masses between 10-40 M Jupiter has been noticed at close separations, suggesting the possibility of a distinct formation mechanism for objects above and below this range. Aims. We present a model for the substellar companion mass function (CMF). This model consists of the superposition of the planet and BD companion mass distributions, assuming that we can extrapolate the radial velocity measured CMF for planets to larger separations and the stellar companion mass-ratio distribution over all separations into the BD mass regime. By using both the results of the VLT/NaCo large program (NaCo-LP) and the complementary archive datasets, which probe the occurrence of planets and BDs on wide orbits around solar-type stars, we place some constraints on the planet and BD distributions. Methods. We developed a Monte Carlo simulation tool to predict the outcome of a given survey, depending on the shape of the orbital parameter distributions (mass, semimajor axis, eccentricity, and inclination). Comparing the predictions with the results of the observations, we calculate the likelihood of different models and which models can be ruled out. Results. Current observations are consistent with the proposed model for the CMF, as long as a sufficiently small outer truncation radius ( 100 AU) is introduced for the planet separation distribution. Some regions of parameter space can be excluded by the observations. Conclusions. We conclude that the results of the direct imaging surveys searching for substellar companions around Sun-like stars are consistent with a combined substellar mass spectrum of planets and BDs. This mass distribution has a minimum between 10 and 50 M Jupiter , in agreement with radial velocity measurements. In this picture the dearth of objects in this mass range would naturally arise from the shape of the mass distribution, without the introduction of any distinct formation mechanism for BDs. This kind of model for the CMF allows us to determine the probability for a substellar companion as a function of mass to have formed in a disk or from protostellar core fragmentation, as such mechanisms overlap in this mass range.

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A companion to AB Pic at the planet/brown dwarf boundary

Cited by 232 publications

References 33 publications

Detectability of giant planets in protoplanetary disks by CO emission lines

Detectability of giant planets in protoplanetary disks by CO emission lines

Eccentricity evolution in mean motion resonance and non-radial solar wind

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

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