What Sets the Radial Locations of Warm Debris Disks?

Ballering, Nicholas P.; Rieke, G. H.; Su, K. Y. L.; Gáspár, András

doi:10.3847/1538-4357/aa8037

Cited by 45 publications

(24 citation statements)

References 110 publications

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“…Studies such as that of Ballering et al (2017) alleviate this effect by accounting for the dust's optical properties, assuming all belts share the same composition, and finding that the radial location of warm, inner belts increases around stars with increasing masses, once again with a large scatter. In addition, Herschel marginally resolved a considerable number of cold dust disks (e.g.…”

Section: Introductionmentioning

confidence: 99%

An Empirical Planetesimal Belt Radius–Stellar Luminosity Relation

Matrà¹,

Marino²,

Kennedy³

et al. 2018

ApJ

109

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Resolved observations of millimetre-sized dust, tracing larger planetesimals, have pinpointed the location of 26 Edgeworth-Kuiper belt analogs. We report that a belt's distance R to its host star correlates with the star's luminosity L , following R ∝ L 0.19 with a low intrinsic scatter of ∼17%. Remarkably, our Edgeworth-Kuiper belt in the Solar System and the two CO snow lines imaged in protoplanetary disks lie close to this R-L relation, suggestive of an intrinsic relationship between protoplanetary disk structures and belt locations. To test the effect of bias on the relation, we use a Monte Carlo approach and simulate uncorrelated model populations of belts. We find that observational bias could produce the slope and intercept of the R-L relation, but is unable to reproduce its low scatter. We then repeat the simulation taking into account the collisional evolution of belts, following the steady state model that fits the belt population as observed through infrared excesses. This significantly improves the fit by lowering the scatter of the simulated R-L relation; however, this scatter remains only marginally consistent with the one observed. The inability of observational bias and collisional evolution alone to reproduce the tight relationship between belt radius and stellar luminosity could indicate that planetesimal belts form at preferential locations within protoplanetary disks. The similar trend for CO snow line locations would then indicate that the formation of planetesimals and/or planets in the outer regions of planetary systems is linked to the volatility of their building blocks, as postulated by planet formation models.

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Section: Introductionmentioning

confidence: 99%

An Empirical Planetesimal Belt Radius–Stellar Luminosity Relation

Matrà¹,

Marino²,

Kennedy³

et al. 2018

ApJ

109

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“…Debris discs are thought to be the remains of the planet formation process (Wyatt et al 2012;Currie et al 2015;Booth et al 2017). They are observed to be common around unevolved stars (Moro-Martín et al 2010;Ballering et al 2017;Anglada et al 2017). Debris discs around white dwarfs have not been directly observed, but their existence is implied by the pollution of their atmospheres by asteroidal material, perhaps from a debris disc that survived stellar evolution (Gänsicke et al 2006;Kilic et al 2006;von Hippel et al 2007;Farihi et al 2009;Jura et al 2009;Farihi et al 2010;Melis et al 2010;Brown et al 2017;Bonsor et al 2017;Xu et al 2018;Smallwood et al 2018b).…”

Section: Introductionmentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

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The origin of fast radio bursts (FRBs) is still a mystery. One model proposed to interpret the only known repeating object, FRB 121102, is that the radio emission is generated from asteroids colliding with a highly magnetized neutron star (NS). With N -body simulations, we model a debris disc around a central star with an eccentric orbit intruding NS. As the NS approaches the first periastron passage, most of the comets are scattered away rather than being accreted by the NS. To match the observed FRB rate, the debris belt would have to be at least three orders of magnitude more dense than the Kuiper belt. We also consider the rate of collisions on to the central object but find that the density of the debris belt must be at least four orders of magnitude more dense than the Kuiper belt. These discrepancies in the density arise even if (1) one introduces a Kuiper-belt like comet belt rather than an asteroid belt and assume that comet impacts can also make FRBs; (2) the NS moves ∼ 2 orders of magnitude slower than their normal proper-motion velocity due to supernova kicks; and (3) the NS orbit is coplanar to the debris belt, which provides the highest rate of collisions.

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“…Sublimation and distruption cometary bodies -Comets transported from an outer reservoir into the inner regions are also widely considered as possible sources of warm debris material (e.g., Wyatt et al 2007;Morales et al 2011;Bonsor et al 2012;Ballering et al 2017;Marino et al 2017). Actually, in our solar system the zodiacal dust particles dominantly stem from comets (Nesvorný et al 2010;Rowan-Robinson & May 2013).…”

Section: Alternative Scenarios For the Formation Of Eddsmentioning

confidence: 99%

A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog

Moór

Ábrahám

Szabó

et al. 2021

ApJ

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Extreme debris disks (EDDs) are rare systems with peculiarly large amounts of warm dust that may stem from recent giant impacts between planetary embryos during the final phases of terrestrial planet growth. Here we report on the identification and characterization of six new EDDs. These disks surround F5-G9 type main-sequence stars with ages >100 Myr, have dust temperatures higher than 300 K and fractional luminosities between 0.01 and 0.07. Using time-domain photometric data at 3.4 and 4.6 µm from the WISE all sky surveys, we conclude that four of these disks exhibited variable mid-infrared emission between 2010 and 2019. Analyzing the sample of all known EDDs, now expanded to 17 objects, we find that 14 of them showed changes at 3-5 µm over the past decade suggesting that mid-infrared variability is an inherent characteristic of EDDs. We also report that wide-orbit pairs are significantly more common in EDD systems than in the normal stellar population. While current models of rocky planet formation predict that the majority of giant collisions occur in the first 100 Myr, we find that the sample of EDDs is dominated by systems older than this age. This raises the possibility that the era of giant impacts may be longer than we think, or that some other mechanism(s) can also produce EDDs. We examine a scenario where the observed warm dust stems from the disruption and/or collisions of comets delivered from an outer reservoir into the inner regions, and explore what role the wide companions could play in this process.

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What Sets the Radial Locations of Warm Debris Disks?

Cited by 45 publications

References 110 publications

An Empirical Planetesimal Belt Radius–Stellar Luminosity Relation

An Empirical Planetesimal Belt Radius–Stellar Luminosity Relation

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

A New Sample of Warm Extreme Debris Disks from the ALLWISE Catalog

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