ALMA Images the Eccentric HD 53143 Debris Disk

MacGregor, Meredith A.; Hurt, Spencer A.; Stark, Christopher C.; Howard, Ward S.; Weinberger, Alycia J.; Ren, Bin; Schneider, Glenn; Choquet, Élodie; Mawet, Dimitri

doi:10.3847/2041-8213/ac7729

Cited by 12 publications

(1 citation statement)

References 40 publications

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“…The study of gas can help us better understand the evolution of debris disks and the formation of planets, as well as the study of debris disk structure. Disk structure can be seen clearly from images of resolved disks such as the two-belt systems (Boley et al 2012;Matthews et al 2014b;Rajan et al 2015;Desgrange et al 2022;MacGregor et al 2022). MacGregor et al (2019 found gap structure in HD 15115 through direct imaging and thought it might be caused by planet sculpting.…”

Section: Introductionmentioning

confidence: 99%

A Catalog of Collected Debris Disks: Properties, Classifications and Correlations between Disks and Stars/Planets

Cao

Liu

Liao

et al. 2023

Res. Astron. Astrophys.

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1. We have collected a catalog of 1095 debris disks with properties and classification (resolved, planet, gas) information. From the catalog, we defined a less biased sample with 612 objects and presented the distributions of their stellar and disk properties to search for correlations between disks and stars. We found debris disks were widely distributed from B to M-type stars while planets were mostly found around solar-type stars, gases were easier to detect around early-type stars and resolved disks were mostly distributed from A to G- type stars. The fractional luminosity dropped off with stellar age and planets were mostly found around old stars while gas-detected disks were much younger. The dust temperature of both one-belt systems and cold components in two-belt systems increased with distance while decreased with stellar age. In addition, we defined a less biased planet sample with 211 stars with debris disks but no planets and 35 stars with debris disks and planets and found the stars with debris disks and planets had higher metallicities than stars with debris disks but no planets. Among the 35 stars with debris disks and planets, we found the stars with disks and cool Jupiters were widely distributed with age from 10 Myr to 10 Gyr and metallicity from -1.56 to 0.28 while the other three groups tended to be old (> 4Gyr) and metal-rich (> -0.3). Besides, the eccentricities of cool Jupiters are distributed from 0 to 0.932 wider than the other three types of planets (< 0.3).

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Section: Introductionmentioning

confidence: 99%

A Catalog of Collected Debris Disks: Properties, Classifications and Correlations between Disks and Stars/Planets

Cao

Liu

Liao

et al. 2023

Res. Astron. Astrophys.

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Development and suborbital validation of technologies for direct imaging of nearby exoplanetary systems in reflected visible wavelengths

Chakrabarti,

Mendillo,

Hewawasam

et al. 2023

Acta Astronautica

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Using debris disk observations to infer substellar companions orbiting within or outside a parent planetesimal belt

Stuber

Löhne

Wolf

2022

A&A

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Context. Alongside a debris disk, substellar companions often exist in the same system. The companions influence the dust dynamics via their gravitational potential. Aims. We analyze whether the effects of secular perturbations, originating from a substellar companion, on the dust dynamics can be investigated with spatially resolved observations. Methods. We numerically simulated the collisional evolution of narrow and eccentric cold planetesimal belts around a star of spectral type A3 V that are secularly perturbed by a substellar companion that orbits either closer to or farther from the star than the belt. Our model requires a perturber on an eccentric orbit (𝑒 0.3) that is both far from and more massive than the collisionally dominated belt around a luminous central star. Based on the resulting spatial dust distributions, we simulated spatially resolved maps of their surface brightness in the 𝐾, 𝑁, and 𝑄 bands and at wavelengths of 70 µm and 1300 µm. Results. Assuming a nearby debris disk seen face-on, we find that the surface brightness distribution varies significantly with observing wavelength, for example between the 𝑁 and 𝑄 band. This can be explained by the varying relative contribution of the emission of the smallest grains near the blowout limit. The orbits of both the small grains that form the halo and the large grains close to the parent belt precess due to the secular perturbations induced by a substellar companion orbiting inward of the belt. The halo, being composed of older grains, trails the belt. The magnitude of the trailing decreases with increasing perturber mass and hence with increasing strength of the perturbations. We recovered this trend in synthetic maps of their surface brightness by fitting ellipses to lines of constant brightness. Systems with an outer perturber do not show a uniform halo precession since the orbits of small grains are strongly altered. We identified features of the brightness distributions suitable for distinguishing between systems with a potentially detectable inner or outer perturber, especially with a combined observation with JWST/MIRI in the 𝑄 band tracing small grain emission and with ALMA at millimeter wavelengths tracing the position of the parent planetesimal belt.

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ALMA Images the Eccentric HD 53143 Debris Disk

Cited by 12 publications

References 40 publications

A Catalog of Collected Debris Disks: Properties, Classifications and Correlations between Disks and Stars/Planets

A Catalog of Collected Debris Disks: Properties, Classifications and Correlations between Disks and Stars/Planets

Development and suborbital validation of technologies for direct imaging of nearby exoplanetary systems in reflected visible wavelengths

Using debris disk observations to infer substellar companions orbiting within or outside a parent planetesimal belt

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