The Dynamical Structure of HR 8799’s Inner Debris Disk

Contro, Bruna; Wittenmyer, R. A.; Horner, Jonathan; Marshall, Jonathan P.

doi:10.1007/s11084-015-9405-x

Cited by 7 publications

(4 citation statements)

References 25 publications

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“…The exoplanetary systems orbiting the A-type stars HR 8799, Vega, and Fomalhaut all appear to share this basic architecture (Su et al, 2009(Su et al, , 2013 with asteroid belt analogs located near (and interior to) their respective snow lines, and with (confirmed or inferred) giant planets just exterior. Early simulations demonstrate that the exoplanet HR 8799e will often perturb its exoasteroids towards the inner system (Contro et al, 2015), suggesting that a progenitor architecture of polluted white dwarf systems, one which is similar to the Solar System, is not unusual.…”

Section: Planetary System Possibilitiesmentioning

confidence: 99%

Circumstellar debris and pollution at white dwarf stars

Farihi

2016

New Astronomy Reviews

300

265

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Circumstellar disks of planetary debris are now known or suspected to closely orbit hundreds of white dwarf stars. To date, both data and theory support disks that are entirely contained within the preceding giant stellar radii, and hence must have been produced during the white dwarf phase. This picture is strengthened by the signature of material falling onto the pristine stellar surfaces; disks are always detected together with atmospheric heavy elements. The physical link between this debris and the white dwarf host abundances enables unique insight into the bulk chemistry of extrasolar planetary systems via their remnants. This review summarizes the body of evidence supporting dynamically active planetary systems at a large fraction of all white dwarfs, the remnants of first generation, main-sequence planetary systems, and hence provide insight into initial conditions as well as long-term dynamics and evolution.

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Section: Planetary System Possibilitiesmentioning

confidence: 99%

Circumstellar debris and pollution at white dwarf stars

Farihi

2016

New Astronomy Reviews

300

265

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“…Moreover, if one assumes circular and pole-on orbits, there will be no gain at combining all DI data. The intermediate cases between those extremes are more common, like HR8799 (25 ˝with respect to the plane of the sky, Contro et al 2015), TW Hydrae (7 ˝for the outer disk and 4.3 ˝for the inner disk, Setiawan et al 2008;Pontoppidan et al 2008) or HD141569 (51 ˝, van der Plas et al 2015). Fig.…”

Section: Concluding Remarks and Perspectivesmentioning

confidence: 99%

Combining direct imaging and radial velocity data towards a full exploration of the giant planet population

Lannier

Lagrange

Bonavita

et al. 2017

A&A

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Context. Thanks to the detections of more than 3000 exoplanets these last 20 years, statistical studies have already highlighted some properties in the distribution of the planet parameters. Nevertheless, few studies have yet investigated the planet populations from short to large separations around the same star since this requires the use of different detection techniques that usually target different types of stars. Aims. We wish to develop a tool that combines direct and indirect methods so as to correctly investigate the giant planet populations at all separations. Methods. We developed the MESS2 code, a Monte Carlo simulation code combining radial velocity and direct imaging data obtained at different epochs for a given star to estimate the detection probability of giant planets spanning a wide range of physical separations. It is based on the generation of synthetic planet populations. Results. We apply MESS2 on a young M1-type, the nearby star AU Mic observed with HARPS and NACO/ESO. We show that giant planet detection limits are significantly improved at intermediate separations («20 au in the case of AU Mic). We show that the traditional approach of analysing independently the RV and DI detection limits systematically overestimates the planet detection limits and hence planet occurrence rates. The use of MESS2 allows to obtain correct planet occurrence rates in statistical studies, making use of multi-epoch DI data and/or RV measurements. We also show that MESS2 can optimise the schedule of future DI observations.

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“…Their mass ratio with their host star and short projected separations (∼15-70 AU) distinguish them from the population of previously known planetary mass companions. The existence of a warm inner belt of debris and cold Kuiper belt bracketing the orbits of the planets (Su et al 2009;Hughes et al 2011;Matthews et al 2014;Contro et al 2015) indicates that the companions likely formed into a circumstellar disk.…”

Section: Introductionmentioning

confidence: 99%

First light of the VLT planet finder SPHERE

Bonnefoy¹,

Zurlo²,

Baudino³

et al. 2016

A&A

132

104

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Context. The system of four planets discovered around the intermediate-mass star HR8799 offers a unique opportunity to test planet formation theories at large orbital radii and to probe the physics and chemistry at play in the atmospheres of self-luminous young (∼30 Myr) planets. We recently obtained new photometry of the four planets and low-resolution (R ∼ 30) spectra of HR8799 d and e with the SPHERE instrument (Paper III). Aims. In this paper (Paper IV), we aim to use these spectra and available photometry to determine how they compare to known objects, what the planet physical properties are, and how their atmospheres work. Methods. We compare the available spectra, photometry, and spectral energy distribution (SED) of the planets to field dwarfs and young companions. In addition, we use the extinction from corundum, silicate (enstatite and forsterite), or iron grains likely to form in the atmosphere of the planets to try to better understand empirically the peculiarity of their spectrophotometric properties. To conclude, we use three sets of atmospheric models (BT-SETTL14, Cloud-AE60, Exo-REM) to determine which ingredients are critically needed in the models to represent the SED of the objects, and to constrain their atmospheric parameters (T eff , log g, M/H). Results. We find that HR8799d and e properties are well reproduced by those of L6-L8 dusty dwarfs discovered in the field, among which some are candidate members of young nearby associations. No known object reproduces well the properties of planets b and c. Nevertheless, we find that the spectra and WISE photometry of peculiar and/or young early-T dwarfs reddened by submicron grains made of corundum, iron, enstatite, or forsterite successfully reproduce the SED of these planets. Our analysis confirms that only the Exo-REM models with thick clouds fit (within 2σ) the whole set of spectrophotometric datapoints available for HR8799 d and e for T eff = 1200 K, log g in the range 3.0−4.5, and M/H = +0.5. The models still fail to reproduce the SED of HR8799c and b. The determination of the metallicity, log g, and cloud thickness are degenerate. Conclusions. Our empirical analysis and atmospheric modelling show that an enhanced content in dust and decreased CIA of H 2 is certainly responsible for the deviation of the properties of the planet with respect to field dwarfs. The analysis suggests in addition that HR8799c and b have later spectral types than the two other planets, and therefore could both have lower masses.

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The Dynamical Structure of HR 8799’s Inner Debris Disk

Cited by 7 publications

References 25 publications

Circumstellar debris and pollution at white dwarf stars

Circumstellar debris and pollution at white dwarf stars

Combining direct imaging and radial velocity data towards a full exploration of the giant planet population

First light of the VLT planet finder SPHERE

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