Accreting protoplanets in the LkCa 15 transition disk

Sallum, Steph; Follette, Katherine B.; Eisner, J. A.; Close, Laird M.; Hinz, Philip M.; Kratter, Kaitlin M.; Males, Jared R.; Skemer, Andrew J.; Macintosh, Bruce; Tuthill, Peter; Bailey, Vanessa P.; Defrère, Denis; Morzinski, Katie M.; Rodigas, Timothy J.; Spalding, Eckhart; Vaz, Amali; Weinberger, Alycia J.

doi:10.1038/nature15761

Cited by 308 publications

(437 citation statements)

References 51 publications

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“…This is a highly unknown quantity with a significant effect on the resultant values of M cṀc . We arbitrarily chose our inner disc radius to be the same value as that assumed by Sallum et al (2015) for the purposes of comparison. When matching the absolute magntiudes are difficult to match we linearly interpolate.…”

Section: Resultsmentioning

confidence: 99%

“…Subaru/SEEDS survey; Hashimoto et al 2011;Grady et al 2013) and sparse aperture masking interferometry (SAM) has resulted in the detection of small-scale asymmetries in the brightness distribution around young stars that have been interpreted as low-mass companions (T Cha: Huélamo et al 2011;LkCa 15: Kraus & Ireland 2012;HD 142527: Biller et al 2012) or as disc emission of a heated wall in a centro-symmetric disc seen under intermediate inclination (FL Cha: Cieza et al 2013;T Cha: Olofsson et al 2013). Only in the case of LkCa 15 has this continuum detection been confirmed as an accreting companion, with subsequent observations using a combination of SAM and Hα spectral differential imaging performed by Sallum et al (2015) to demonstrate for the first time unambiguous evidence for the accreting nature of the companion.…”

Section: Introductionmentioning

confidence: 99%

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Sparse aperture masking interferometry survey of transitional discs

Willson

Kraus

Kluska

et al. 2016

A&A

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Context. Transitional discs are a class of circumstellar discs around young stars with extensive clearing of dusty material within their inner regions on 10s of au scales. One of the primary candidates for this kind of clearing is the formation of planet(s) within the disc that then accrete or clear their immediate area as they migrate through the disc. Aims. The goal of this survey was to search for asymmetries in the brightness distribution around a selection of transitional disc targets. We then aimed to determine whether these asymmetries trace dynamically-induced structures in the disc or the gap-opening planets themselves. Methods. Our sample included eight transitional discs. Using the Keck/NIRC2 instrument we utilised the Sparse Aperture Masking (SAM) interferometry technique to search for asymmetries indicative of ongoing planet formation. We searched for close-in companions using both model fitting and interferometric image reconstruction techniques. Using simulated data, we derived diagnostics that helped us to distinguish between point sources and extended asymmetric disc emission. In addition, we investigated the degeneracy between the contrast and separation that appear for marginally resolved companions. Results. We found FP Tau to contain a previously unseen disc wall, and DM Tau, LkHα330, and TW Hya to contain an asymmetric signal indicative of point source-like emission. We placed upper limits on the contrast of a companion in RXJ1842.9-3532 and V2246 Oph. We ruled the asymmetry signal in RXJ1615.3-3255 and V2062 Oph to be false positives. In the cases where our data indicated a potential companion we computed estimates for the value of M cṀc and found values in the range of 10 −5 − 10 −3 M 2 J yr −1 . Conclusions. We found significant asymmetries in four targets. Of these, three were consistent with companions. We resolved a previously unseen gap in the disc of FP Tau extending inwards from approximately 10 au.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Sparse aperture masking interferometry survey of transitional discs

Willson

Kraus

Kluska

et al. 2016

A&A

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“…These fascinating observations of planet formation as it happens provide an additional motivation to study the luminosity of planets already during the formation phase, whether or not their radiation can leave relatively unimpeded their natal circumstellar and -planetary disk(s). Indeed, a part of the accretion luminosity could be directly visible in H α (e.g., Sallum et al 2015), or in the infrared (van Boekel et al 2017) and the planet's radiative feedback is expected to change the local thermal and density structure of the disk (Montesinos et al 2015;Klahr & Kley 2006) and thus its chemistry (Cleeves et al 2015). In the near future, this should be accessible to the unprecedented resolution and exquisite sensitivity of the Atacama Large Millimeter Array (ALMA; Wolf 2008;Cleeves et al 2015).…”

Section: Introductionmentioning

confidence: 99%

“…In only the last few years, cutting-edge observations have caught a small number of putative low-mass companions in their mass-assembly phase (around LkCa 15, HD 142527, HD 100546, and HD 169142;Kraus & Ireland 2012;Sallum et al 2015;Close et al 2014;Quanz et al 2013;Reggiani et al 2014). These fascinating observations of planet formation as it happens provide an additional motivation to study the luminosity of planets already during the formation phase, whether or not their radiation can leave relatively unimpeded their natal circumstellar and -planetary disk(s).…”

Section: Introductionmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

116

142

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Context. This paper continues a series in which we predict the main observable characteristics of exoplanets based on their formation. In Paper I we described our global planet formation and evolution model that is based on the core accretion paradigm. In Paper II we studied the planetary mass-radius relationship with population syntheses. Aims. In this paper we present an extensive study of the statistics of planetary luminosities during both formation and evolution. Our results can be compared with individual directly imaged extrasolar (proto)planets and with statistical results from surveys. Methods. We calculated three populations of synthetic planets assuming different efficiencies of the accretional heating by gas and planetesimals during formation. We describe the temporal evolution of the planetary mass-luminosity relation. We investigate the relative importance of the shock and internal luminosity during formation, and predict a statistical version of the post-formation mass vs. entropy "tuning fork" diagram. Because the calculations now include deuterium burning we also update the planetary mass-radius relationship in time.Results. We find significant overlap between the high post-formation luminosities of planets forming with hot and cold gas accretion because of the core-mass effect. Variations in the individual formation histories of planets can still lead to a factor 5 to 20 spread in the post-formation luminosity at a given mass. However, if the gas accretional heating and planetesimal accretion rate during the runaway phase is unknown, the post-formation luminosity may exhibit a spread of as much as 2-3 orders of magnitude at a fixed mass. As a key result we predict a flat log-luminosity distribution for giant planets, and a steep increase towards lower luminosities due to the higher occurrence rate of low-mass (M 10-40 M ⊕ ) planets. Future surveys may detect this upturn. Conclusions. Our results indicate that during formation an estimation of the planetary mass may be possible for cold gas accretion if the planetary gas accretion rate can be estimated. If it is unknown whether the planet still accretes gas, the spread in total luminosity (internal+accretional) at a given mass may be as large as two orders of magnitude, therefore inhibiting the mass estimation. Due to the core-mass effect even planets which underwent cold accretion can have large post-formation entropies and luminosities, such that alternative formation scenarios such as gravitational instabilities do not need to be invoked. Once the number of self-luminous exoplanets with known ages and luminosities increases, the resulting luminosity distributions may be compared with our predictions.

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“…One spectacular observed example for this process might be the LkCa 15 transitional disks. Recent adaptive optics observations by Sallum et al (2015) reveal up to three accreting giant proto-planets in the large inner cavity (r cav ≈ 50 au, ) of this disk. At the same time the outer disk of this system still remains intact and shows similar observational signatures as classical disks (Öberg et al 2011;Punzi et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Gas Disk: Evolution and Chemistry

et al. 2016

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Protoplanetary disks are the birthplaces of planetary systems. The evolution of the star-disk system and the disk chemical composition determines the initial conditions for planet formation. Therefore a comprehensive understanding of the main physical and chemical processes in disks is crucial for our understanding of planet formation. We give an overview of the early evolution of disks, discuss the importance of the stellar high-energy radiation for disk evolution and describe the general thermal and chemical structure of disks. Finally we provide an overview of observational tracers of the gas component and disk winds.

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Accreting protoplanets in the LkCa 15 transition disk

Cited by 308 publications

References 51 publications

Sparse aperture masking interferometry survey of transitional discs

Sparse aperture masking interferometry survey of transitional discs

Characterization of exoplanets from their formation

The Gas Disk: Evolution and Chemistry

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