The unseen planets of double belt debris disc systems

Shannon, Andrew; Bonsor, Amy; Kral, Quentin; Matthews, Elisabeth C.

doi:10.1093/mnrasl/slw143

Cited by 68 publications

(85 citation statements)

References 57 publications

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“…To clear a gap between 10 and 80 au over 16 Myr, we find that two planets of > 0.65 M Jup are needed. Shannon et al (2016) assume equal-mass planets separated by 20 mutual Hill radii (i.e., the typical separation between planets in Kepler multi-planet systems). Using the planet mass upper limits from this paper together with the lower limit that we have just derived, we find that the potential planet able to warp the inner cold disc would have a mass of between 0.65 and 2 M Jup .…”

Section: Discussionmentioning

confidence: 99%

Two cold belts in the debris disk around the G-type star NZ Lupi

Boccaletti

Thébault

Pawellek

et al. 2019

A&A

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Context. Planetary systems hold the imprint of the formation and of the evolution of planets especially at young ages, and in particular at the stage when the gas has dissipated leaving mostly secondary dust grains. The dynamical perturbation of planets in the dust distribution can be revealed with high-contrast imaging in a variety of structures. Aims. SPHERE, the high-contrast imaging device installed at the VLT, was designed to search for young giant planets in long period, but is also able to resolve fine details of planetary systems at the scale of astronomical units in the scattered-light regime. As a young and nearby star, NZ Lup was observed in the course of the SPHERE survey. A debris disk had been formerly identified with HST/NICMOS. Methods. We observed this system in the near-infrared with the camera in narrow and broad band filters and with the integral field spectrograph. High contrasts are achieved by the mean of pupil tracking combined with angular differential imaging algorithms. Results. The high angular resolution provided by SPHERE allows us to reveal a new feature in the disk which is interpreted as a superimposition of two belts of planetesimals located at stellocentric distances of ∼85 and ∼115 au, and with a mutual inclination of about 5 • . Despite the very high inclination of the disk with respect to the line of sight, we conclude that the presence of a gap, that is, a void in the dust distribution between the belts, is likely. Conclusions. We discuss the implication of the existence of two belts and their relative inclination with respect to the presence of planets.

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Section: Discussionmentioning

confidence: 99%

Two cold belts in the debris disk around the G-type star NZ Lupi

Boccaletti

Thébault

Pawellek

et al. 2019

A&A

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“…The positions of the inner and outer debris belts are indicated in grey, with the regions inside the inner and beyond the outer shaded. Our direct imaging contrast limits based on SPHERE/IRDIS are shown in orange, with the region above this shaded, and dynamical mass constraints from Shannon et al (2016) are indicated in green, with masses below this value shaded. The uncertainty on this lower limit is calculated based on the age of host and the uncertainty in debris belt temperature, and indicated with hatching.…”

Section: Discussionmentioning

confidence: 99%

“…In a small number of cases, the planet masses inferred from Shannon et al (2016) are sufficiently high that the value of R H approaches a significant fraction of the starplanet spacing. In this case, for planets to be spaced by K R H , the second planet will be at semi-major axis a 2 = a 1 + K R H .…”

Section: Datementioning

confidence: 97%

“…As well as using disk structure to predict the locations of planets, it is possible to use dynamical arguments to constrain exoplanet masses. By assuming several equal mass planets spread across a debris gap, Shannon et al (2016) found that the clearing time scales with the planet mass and the width of the debris gap. For a system with widely spaced debris belts and giant planets, this timescale is of order millions of years, and as such is similar to the lifetime of the system.…”

Section: Introductionmentioning

confidence: 99%

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Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments

Matthews

Hinkley

Vigan

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR 8799 and HD 95086 systems, and even the solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disk, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical timescales to clear debris. The typical dynamical lower limit is ∼0.2M J in this work, and in some cases exceeds 1M J . Direct imaging data, meanwhile, is typically sensitive to planets down to ∼3.6M J at 1", and 1.7M J in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers.

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“…Even the gap between two components debris disks is suspected to be carved by intervening planets scattering away the remnant planetesimals (Su & Rieke 2014;Shannon et al 2016) and a survey based on direct imaging is searching for planets in systems with double debris disks (Meshkat et al 2015). In addition to these direct effects, a planet also perturbs the planetesimal belt stirring up their orbits and affecting the collision probability and impact velocity (Mustill & Wyatt 2009).…”

Section: Introductionmentioning

confidence: 99%

Collisional parameters of planetesimal belts, precursor of debris discs, perturbed by a nearby giant planet

Marzari

Dell’Oro

2016

Mon. Not. R. Astron. Soc.

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Planetesimal belts are invoked to explain the prolonged existence of debris disks. Important parameters to model their collisional evolution and to compute the dust production rate are the intrinsic probability of collision P i and the mean impact velocity U c . If a planet orbits close to the belt, the values of both these parameters are affected by its secular perturbations yielding a strong correlation between eccentricity e and pericentre longitude ̟. We adopt a new algorithm to compute both P i and U c in presence of various levels of secular correlation due to different ratios between proper and forced eccentricity. We tested this algorithm in a standard case with a Jupiter-sized planet orbiting inside a putative planetesimal belt finding that it is less collisionally active compared to a self-stirred belt because of the e − ̟ coupling. The eccentricity of the planet is an important parameter in determining the amount of dust production since the erosion rate is 10 times faster when the planet eccentricity increases from 0.1 to 0.6. Also the initial conditions of the belt (either warm or cold) and its average inclination strongly affects P i and U c and then its long term collisional evolution in presence of the planet. We finally apply our method to the planetesimal belts supposedly refilling the dust disks around HD 38529 and ǫ Eridani. In the most collisionally active configurations, only a small fraction of bodies smaller than 100 km are expected to be fragmented over a time-span of 4 Gyr.

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The unseen planets of double belt debris disc systems

Cited by 68 publications

References 57 publications

Two cold belts in the debris disk around the G-type star NZ Lupi

Two cold belts in the debris disk around the G-type star NZ Lupi

Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments

Collisional parameters of planetesimal belts, precursor of debris discs, perturbed by a nearby giant planet

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