Collisions and drag in debris discs with eccentric parent belts

Löhne, T.; Krivov, A. V.; Kirchschlager, Florian; Sende, J. A.; Wolf, S.

doi:10.1051/0004-6361/201630297

Cited by 24 publications

(59 citation statements)

References 75 publications

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“…That interpretation is supported by ALMA imaging which showed that the opposite side of the disk is brighter as expected due to the slower orbital velocity at apocentre (Pan et al 2016). Subsequently scattered light imaging showed that the star is not exactly at the centre of the disk (Milli et al 2017), although the direction of the offset is not exactly that expected suggesting that there may be some additional density variations around the ring (see also Löhne et al 2017). Fomalhaut's disk (see Fig.…”

Section: Dynamical Structuresmentioning

confidence: 75%

Extrasolar Kuiper belts

Wyatt

2020

The Trans-Neptunian Solar System

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Extrasolar debris disks are the dust disks found around nearby main sequence stars arising from the break-up of asteroids and comets orbiting the stars. Far-IR surveys (e.g., with Herschel) showed that ∼ 20% of stars host detectable dust levels. While dust temperatures suggest a location at 10s of au comparable with our Kuiper belt, orders of magnitude more dust is required implying a planetesimal population more comparable with the primordial Kuiper belt. High resolution imaging (e.g., with ALMA) has mapped the nearest and brightest disks, providing evidence for structures shaped by an underlying planetary system. Some of these are analogous to structures in our own Kuiper belt (e.g., the hot and cold classical, resonant, scattered disk and cometary populations), while others have no Solar System counterpart. CO gas is seen in some debris disks, and inferred to originate in the destruction of planetesimals with a similar volatile-rich composition to Solar System comets. This chapter reviews our understanding of extrasolar Kuiper belts and of how our own Kuiper belt compares with those of neighbouring stars.

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Section: Dynamical Structuresmentioning

confidence: 75%

Extrasolar Kuiper belts

Wyatt

2020

The Trans-Neptunian Solar System

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“…For this purpose we generated models of fiducial discs of different radii around mainsequence stars of various spectral types covering a broad luminosity range. We used the ACE code (Löhne et al 2017) to follow the collisional evolution of discs and then created their thermal emission images and surface brightness profiles at different wavelengths from mm down to mid-infrared. For the reference model setup (excitation level of 0.1, a relative belt width of 10%, without Poynting-Robertson and stellar wind drag), we found that it is possible to trace the planetesimal belts of all radii tested (from 30 AU to 200 AU) around all host stars (from A to M) and at all wavelengths investigated (from 1 mm down to 23 µm).…”

Section: Discussionmentioning

confidence: 99%

“…For our analysis we use the modelling code "Analysis of Collisional Evolution" (ACE, see Löhne et al 2017, and references therein) which allows a full featured collisional modelling of debris discs. It produces spatial and size distributions of circumstellar material, sized between dwarf planets and dust particles, and evolves them over giga-year time spans.…”

Section: Modelling With Acementioning

confidence: 99%

Dust spreading in debris discs: do small grains cling on to their birth environment?

Pawellek

Moór

Pascucci

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Debris discs are dusty belts of planetesimals around main-sequence stars, similar to the asteroid and Kuiper belts in our solar system. The planetesimals cannot be observed directly, yet they produce detectable dust in mutual collisions. Observing the dust, we can try to infer properties of invisible planetesimals. Here we address the question of what is the best way to measure the location of outer planetesimal belts that encompass extrasolar planetary systems. A standard method is using resolved images at mm-wavelengths, which reveal dust grains with sizes comparable to the observational wavelength. Smaller grains seen in the infrared (IR) are subject to several non-gravitational forces that drag them away from their birth rings, and so may not closely trace the parent bodies. In this study, we examine whether imaging of debris discs at shorter wavelengths might enable determining the spatial location of the exo-Kuiper belts with sufficient accuracy. We find that around M-type stars the dust best visible in the mid-IR is efficiently displaced inward from their birth location by stellar winds, causing the discs to look more compact in mid-IR images than they actually are. However, around earlier-type stars where the majority of debris discs is found, discs are still the brightest at the birth ring location in the mid-IR regime. Thus, sensitive IR facilities with good angular resolution, such as MIRI on JWST, will enable tracing exo-Kuiper belts in nearby debris disc systems.

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“…Whilst the variations in spectral index across the disc seen in figure 7 are not found to be significant due to the low sensitivity of the band 3 and 7 data and the low resolution of the band 3 data, with deep resolved maps at multiple ALMA wavelengths, such methods could be used to determine such variations. Variations are expected, for instance, in the case of an eccentric disc, where a difference in size distribution is expected between the pericentre and apocentre due to it being easier to remove small grains by radiation pressure at the pericentre than at the apocentre (Löhne et al 2017;Kim et al 2018).…”

Section: Size Distributionmentioning

confidence: 99%

Deep ALMA search for CO gas in the HD 95086 debris disc

Booth

Matrà

et al. 2018

Monthly Notices of the Royal Astronomical Society

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One of the defining properties of debris discs compared to protoplanetary discs used to be their lack of gas, yet small amounts of gas have been found around an increasing number of debris discs in recent years. These debris discs found to have gas tend to be both young and bright. In this paper we conduct a deep search for CO gas in the system HD 95086 -a 17 Myr old, known planet host that also has a debris disc with a high fractional luminosity of 1.5×10 −3 . Using the Atacama Large Millimeter/submillimeter Array (ALMA) we search for CO emission lines in bands 3, 6 and 7. By implementing a spectro-spatial filtering technique, we find tentative evidence for CO J=2-1 emission in the disc located at a velocity, 8.5±0.2 km s −1 , consistent with the radial velocity of the star. The tentative detection suggests that the gas on the East side of the disc is moving towards us. In the same region where continuum emission is detected, we find an integrated line flux of 9.5±3.6 mJy km s −1 , corresponding to a CO mass of (1.4-13)×10 −6 M ⊕ . Our analysis confirms that the level of gas present in the disc is inconsistent with the presence of primordial gas in the system and is consistent with second generation production through the collisional cascade.

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Collisions and drag in debris discs with eccentric parent belts

Cited by 24 publications

References 75 publications

Extrasolar Kuiper belts

Extrasolar Kuiper belts

Dust spreading in debris discs: do small grains cling on to their birth environment?

Deep ALMA search for CO gas in the HD 95086 debris disc

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