An Enigmatic Point-Like Feature Within the Hd 169142 Transitional Disk,

Biller, Beth; Males, Jared R.; Rodigas, Timothy J.; Morzinski, Katie M.; Close, Laird M.; Juhász, A.; Follette, Katherine B.; Lacour, S.; Benisty, M.; Sicilia‐Aguilar, A.; Hinz, Philip M.; Weinberger, Alycia J.; Henning, Thomas; Pott, Jörg-Uwe; Bonnefoy, M.; Köhler, Rainer H.

doi:10.1088/2041-8205/792/1/l22

Cited by 139 publications

(152 citation statements)

References 45 publications

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“…Recently, several discoveries of (candidate) low-mass companions (low-mass stars and protoplanets) embedded in the circumstellar disk of young stars were announced: around LkCa 15 (Kraus & Ireland 2012), HD 142527 (Biller et al 2012), HD 100546 (Quanz et al 2013), and HD 169142 (Reggiani et al 2014;Biller et al 2014). While the exact nature of some of these sources needs to be further investigated, some of these objects are probably indeed observed in the act of formation as indicated by the Hα emission of LkCa 15 b Sallum et al (2015) (see also HD 142527B, Close et al 2014).…”

Section: The Planetary Mass -Luminosity Relationmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

111

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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Section: The Planetary Mass -Luminosity Relationmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

111

142

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“…It also seems likely that the formation of planetary embryos (if they form at all) precedes the transition disk phase, since it makes more sense for these objects to form in the long period when sufficient mass was available, rather than during the short transition phase during which that mass was depleted. Moreover there is some observational evidence for planets or companions in transition disks (Huélamo et al 2011;Kraus and Ireland 2012;Quanz et al 2013;Biller et al 2014;Reggiani et al 2014), and the gas giant planets seen around many main sequence stars must have formed in the presence of significant quantities of gas.…”

Section: Physical Distinctionmentioning

confidence: 99%

Five steps in the evolution from protoplanetary to debris disk

Wyatt

Panić

Kennedy

et al. 2015

Astrophys Space Sci

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The protoplanetary disks seen around Herbig Ae stars eventually dissipate leaving just a tenuous debris disk, comprised of planetesimals and the dust derived from them, as well as possibly gas and planets. This paper uses the properties of the youngest (10-20 Myr) A star debris disks to consider the transition from protoplanetary to debris disk. It is argued that the physical distinction between these two classes should rest on the presence of primordial gas in sufficient quantities to dominate the motion of small dust grains (rather than on the secondary nature of the dust or its level of stirring). This motivates an observational classification based on the dust emission spectrum which is empirically defined so that A star debris disks require fractional excesses < 3 at 12 µm and < 2000 at 70 µm. We also propose that a useful hypothesis to test is that the planet and planetesimal systems seen on the main sequence are already in place during the protoplanetary disk phase, but are obscured or overwhelmed by the rest of the disk. This may be only weakly true if the architecture of the planetary system continues to change until frozen at the epoch of disk dispersal, or completely false if planets and planetesimals form during the relatively short dispersal phase. Five steps in the transition are discussed: (i) the well-known carving of an inner hole to form a transition disk ; (ii) depletion of mm-sized dust in the outer disk, where it is noted that it is of critical importance to ascertain whether this mass ends up in larger planetesimals or is collisionally depleted; (iii) final clearing of inner regions, where it is noted that multiple debris-like mechanisms exist to replenish moderate levels of hot dust atInstitute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK later phases, and that these likely also operate in protoplanetary disks; (iv) disappearence of the gas, noting the recent discoveries of both primordial and secondary gas in debris disks which highlight our ignorance in this area and its impending enlightenment by ALMA; (v) formation of ring-like structure of planetesimals, noting that these are shaped by interactions with planets, and that the location of the planetesimals in protoplanetary disks may be unrelated to that of dust concentrations therein that are set by gas interactions.

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“…These discoveries show HD 169142 to be among the first objects in which multiple gaps have been found. A point-like IR source, possibly a brown dwarf or a forming planet, was found at ∼23 au from the central star, that is, just at the inner rim of the outer disk (Biller et al 2014;Reggiani et al 2014). With radio observations at 7 mm, Osorio et al (2014) confirmed that the second gap is likely to be caused by a dip in surface density profile, and found a possible point source in this gap region.…”

Section: Introductionmentioning

confidence: 99%

A study of dust properties in the inner sub-au region of the Herbig Ae star HD 169142 with VLTI/PIONIER

Chen

Kóspál

Ábrahám

et al. 2018

A&A

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Context. An essential step to understanding protoplanetary evolution is the study of disks that contain gaps or inner holes. The pretransitional disk around the Herbig star HD 169142 exhibits multi-gap disk structure, differentiated gas and dust distribution, planet candidates, and near-infrared fading in the past decades, which make it a valuable target for a case study of disk evolution. Aims. Using near-infrared interferometric observations with VLTI/PIONIER, we aim to study the dust properties in the inner sub-au region of the disk in the years 2011-2013, when the object is already in its near-infrared faint state. Methods. We first performed simple geometric modeling to characterize the size and shape of the NIR-emitting region. We then performed Monte-Carlo radiative transfer simulations on grids of models and compared the model predictions with the interferometric and photometric observations. Results. We find that the observations are consistent with optically thin gray dust lying at R in ∼ 0.07 au, passively heated to T ∼ 1500 K. Models with sub-micron optically thin dust are excluded because such dust will be heated to much higher temperatures at similar distance. The observations can also be reproduced with a model consisting of optically thick dust at R in ∼ 0.06 au, but this model is plausible only if refractory dust species enduring ∼2400 K exist in the inner disk.

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An Enigmatic Point-Like Feature Within the Hd 169142 Transitional Disk,

Cited by 139 publications

References 45 publications

Characterization of exoplanets from their formation

Characterization of exoplanets from their formation

Five steps in the evolution from protoplanetary to debris disk

A study of dust properties in the inner sub-au region of the Herbig Ae star HD 169142 with VLTI/PIONIER

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