A Likely Close-in Low-Mass Stellar Companion to the Transitional Disk Star Hd 142527

Biller, Beth; Lacour, S.; Juhász, A.; Benisty, M.; Chauvin, G.; Olofsson, J.; Pott, Jörg-Uwe; Müller, André; Sicilia‐Aguilar, A.; Bonnefoy, M.; Tuthill, P. G.; Thébault, P.; Henning, Thomas; Crida, A.

doi:10.1088/2041-8205/753/2/l38

Cited by 192 publications

(187 citation statements)

References 27 publications

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“…Whether a mass ratio of q ∼ 0.02 is uncommon for binaries is not clear, because detection limits typically reach q ∼ 0.1, but Wheelwright et al (2010) noted that the companion distribution of Herbig Ae/Be companions is skewed toward higher masses than the interstellar mass function. However, we note that the companion candidate recently discovered around HD 142527 by Biller et al (2012) has a very similar mass and orbital properties. In addition, there seems to be a trend from direct imaging that A-type stars posses heavier planets than less massive stars (Marois et al 2008;Lagrange et al 2010;Carson et al 2013), a trend also seen in radial velocity surveys (Lovis & Mayor 2007).…”

Section: Planet or Brown Dwarf?mentioning

confidence: 64%

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

Mulders

Paardekooper

Panić

et al. 2013

A&A

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Context. Giant planets form in protoplanetary disks while these disks are still gas-rich, and can reveal their presence through the annular gaps they carve out. HD 100546 is a gas-rich disk with a wide gap between a radius of ∼1 and 13 AU, possibly cleared out by a planetary companion or planetary system. Aims. We aim to identify the nature of the unseen companion near the far end of the disk gap. Methods. We used mid-infrared interferometry at multiple baselines to constrain the curvature of the disk wall at the far end of the gap. We used 2D hydrodynamical simulations of embedded planets and brown dwarfs to estimate the viscosity of the disk and the mass of a companion close to the disk wall. Results. We find that the disk wall at the far end of the gap is not vertical, but rounded-off by a gradient in the surface density. This gradient can be reproduced in hydrodynamical simulations with a single, heavy companion ( 30 . . . 80 M Jup ) while the disk has a viscosity of at least α 5 × 10 −3 . Taking into account the changes in the temperature structure after gap opening reduces the lower limit on the planet mass and disk viscosity to 20 M Jup and α = 2 × 10 −3 . Conclusions. The object in the disk gap of HD 100546 that shapes the disk wall is most likely a 60 +20 −40 M Jup brown dwarf, while the disk viscosity is estimated to be at least α = 2 × 10 −3 . The disk viscosity is an important factor in estimating planetary masses from disk morphologies: more viscous disks need heavier planets to open an equally deep gap.

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Section: Planet or Brown Dwarf?mentioning

confidence: 64%

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

Mulders

Paardekooper

Panić

et al. 2013

A&A

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“…background sources. Finally, the candidate substellar companion of 0.2 M at 13 AU recently reported by Biller et al (2012) may be responsible for the structured features within the disk. These structures might also be created by type-II migration or by planetary formation through GI.…”

Section: Giant Planets Around Resolved Disksmentioning

confidence: 69%

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

Rameau

Chauvin

Lagrange

et al. 2013

A&A

105

148

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Context. Over the past decade, direct imaging has confirmed the existence of substellar companions on wide orbits from their parent stars. To understand the formation and evolution mechanisms of these companions, their individual as well as the full population properties must be characterized. Aims. We aim at detecting giant planet and/or brown dwarf companions around young, nearby, and dusty stars. Our goal is also to provide statistics on the population of giant planets at wide-orbits and discuss planet formation models. Methods. We report the results of a deep survey of 59 stars, members of young stellar associations. The observations were conducted with the ground-based adaptive optics system VLT/NaCo at L -band (3.8 μm). We used angular differential imaging to reach the best detection performances down to the planetary mass regime. A statistical analysis of about 60% of the young and southern A-F stars closer than 65 pc allowed us to derive the fraction of giant planets on wide orbits. We used gravitational instability models and planet population synthesis models following the core-accretion scenario to discuss the occurrence of these companions. Results. We resolve and characterize new visual binaries and do not detect any new substellar companion. The survey's median detection performance reaches contrasts of 10 mag at 0.5 and 11.5 mag at 1.0 . We find the occurrence of planets to be between 10.8 and 24.8% at 68% confidence level assuming a uniform distribution of planets in the interval [1, 13] M J and [1, 1000] AU. Considering the predictions of planetary formation models, we set important constraints on the occurrence of massive planets and brown dwarf companions that would have formed by gravitational instability. We show that this mechanism favors the formation of rather massive clumps (M clump > 30 M J ) at wide (a > 40 AU) orbits, which may evolve dynamically and/or fragment. For the population of close-in giant planets that would have formed by core accretion (without considering any planet -planet scattering), our survey marginally explores physical separations (≤20 AU) and cannot constrain this population. We will have to wait for the next generation of planet finders to start exploring that population, and even for the extremely large telescopes for a more complete overlap with other planet-hunting techniques.

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“…These structures suggest that these disks host a massive planet or multiple planets. Observations of planet candidates in transition disks (e.g Huélamo et al 2011;Kraus & Ireland 2012;Biller et al 2012;Quanz et al 2013) have further supported this idea. Nonetheless, other mechanisms such as photoevaporation may also play an important role and explain some of the observed structures (e.g.…”

Section: Introductionmentioning

confidence: 89%

Sequential planet formation in the HD 100546 protoplanetary disk?

Pinilla

Birnstiel

Walsh

2015

A&A

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Context. The disk around the Herbig Ae star, HD 100546, shows structures that suggest the presence of two companions in the disk at ∼10 and ∼70 AU. The outer companion seems to be in the act of formation. Aims. Our aims are to provide constraints on the age of the planets in HD 100546 and to explore the potential evidence for sequential planet formation in transition disks such as HD 100546. Methods. We compare the recent resolved continuum observations of the disk around HD 100546 with the results of dust evolution simulations using an analytical prescription for the shapes of gaps carved by massive planets.Results. An inner pressure bump must have been present since early in the disk lifetime to have good agreement between the dust evolution models and the continuum observations of HD 100546. This pressure bump may have resulted from the presence of a very massive planet (∼20 M Jup ), which formed early in the inner disk (r ∼ 10 AU). If only this single planet exists, the disk is likely to be old, comparable to the stellar age (∼5−10 Myr). Another possible explanation is an additional massive planet in the outer disk (r ∼ 70 AU): either a low-mass outer planet ( < ∼ 5 M Jup ) injected at early times, or a higher mass outer planet ( > ∼ 15 M Jup ) formed very recently, traps the right amount of dust in pressure bumps to reproduce the observations. In the latter case, the disk could be much younger (∼3.0 Myr). Conclusions. In the case in which two massive companions are embedded in the disk around HD 100546, as suggested in the literature, the outer companion could be at least > ∼ 2.5 Myr younger than the inner companion.

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A Likely Close-in Low-Mass Stellar Companion to the Transitional Disk Star Hd 142527

Cited by 192 publications

References 27 publications

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

A survey of young, nearby, and dusty stars conducted to understand the formation of wide-orbit giant planets

Sequential planet formation in the HD 100546 protoplanetary disk?

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