Eccentric debris disc morphologies – I. Exploring the origin of apocentre and pericentre glows in face-on debris discs

Lynch, Elliot M; Lovell, Joshua B.

doi:10.1093/mnras/stab3566

Cited by 9 publications

(5 citation statements)

References 38 publications

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“…This is due to particles at the disk apocenter piling up because of their lower relative velocities. However, as noted in Marino et al (2019) and Lynch & Lovell (2022), the particles at apocenter are more spread out radially, so a well-resolved disk with a constant eccentricity would have no obvious apocenter glow effect. The apocenter glow can still be observed, however, if the disk width is poorly resolved or if the disk eccentricity decreases with distance.…”

Section: Planetary Parametersmentioning

confidence: 88%

Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628

Brady,

Faramaz-Gorka,

Bryden

et al. 2023

ApJ

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We present the results of N-body simulations meant to reproduce the long-term effects of mutually inclined exoplanets on debris disks, using the HD 202628 system as a proxy. HD 202628 is a Gyr-old solar-type star that possesses a directly observable, narrow debris ring with a clearly defined inner edge and nonzero eccentricity, hinting at the existence of a sculpting exoplanet. The eccentric nature of the disk leads us to examine the effect on it over Gyr timescales from an eccentric and inclined planet, placed on its orbit through scattering processes. We find that, in systems with dynamical timescales akin to that of HD 202628, a planetary companion is capable of completely tilting the debris disk. This tilt is preserved over the Gyr age of the system. Simulated observations of our models show that an exoplanet around HD 202628 with an inclination misalignment ≳10° would cause the disk to be observably diffuse and broad, which is inconsistent with Atacama Large Millimeter Array (ALMA) observations. With these observations, we conclude that, if there is an exoplanet shaping this disk, it likely had a mutual inclination of less than 5° with the primordial disk. The conclusions of this work can be applied either to debris disks appearing as narrow rings (e.g., Fomalhaut and HR 4796) or to disks that are vertically thick at ALMA wavelengths (e.g., HD 110058).

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Section: Planetary Parametersmentioning

confidence: 88%

Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628

Brady,

Faramaz-Gorka,

Bryden

et al. 2023

ApJ

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“…At longer millimeter wavelengths, observations are more sensitive to surface density and apocenter glow can be seen. Lynch & Lovell (2022) argue that the interpretation from Pan et al (2016) fails to account for the greater area over which dust is spread at the apocenter position and that debris disks might exhibit either pericenter or apocenter glow at longer wavelengths depending on the resolution of the observations. We note, however, that the spread in orbits at apocenter versus pericenter also depends on the free eccentricity, which is not included in these new models so further investigation is needed to fully explore this effect.…”

Section: Eccentric Structurementioning

confidence: 97%

“…Because the HD 53143 disk does not appear to have this feature, we exclude this extra parameter in our models for simplicity. Similarly, Lynch & Lovell (2022) allow the forced eccentricity to vary with the semimajor axis, which we also do not include here but could impact the derived parameter constraints.…”

Section: Modeling Approachmentioning

confidence: 99%

ALMA Images the Eccentric HD 53143 Debris Disk

MacGregor

Hurt

Stark

et al. 2022

ApJL

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We present ALMA 1.3 mm observations of the HD 53143 debris disk—the first infrared or millimeter image produced of this ∼1 Gyr old solar analog. Previous HST STIS coronagraphic imaging did not detect flux along the minor axis of the disk, which could suggest a face-on geometry with two clumps of dust. These ALMA observations reveal a disk with a strikingly different structure. In order to fit models to the millimeter visibilities and constrain the uncertainties on the disk parameters, we adopt a Markov Chain Monte Carlo approach. This is the most eccentric debris disk observed to date with a forced eccentricity of 0.21 ± 0.02, nearly twice that of the Fomalhaut debris disk, and also displays an apocenter glow. Although this eccentric model fits the outer debris disk well, significant interior residuals remain, which may suggest a possible edge-on inner disk, which remains unresolved in these observations. Combined with the observed structure difference between HST and ALMA, these results suggest a potential previous scattering event or dynamical instability in this system. We also note that the stellar flux changes considerably over the course of our observations, suggesting flaring at millimeter wavelengths. Using simultaneous TESS observations, we determine the stellar rotation period to be 9.6 ± 0.1 days.

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“…At longer millimeter wavelengths, observations are more sensitive to surface density and apocenter glow can be seen. Lynch & Lovell (2022) argue that the interpretation from Pan et al (2016) fails to account for the greater area over which dust is spread at apocenter, and that debris disks might exhibit either pericenter or apocenter glow at longer wavelengths depending on the resolution of the observations. We note, however, that the spread in orbits at apocenter vs. pericenter also depends on the free eccentricity, which is not included in these new models so further investigation is needed to fully explore this effect.…”

Section: Eccentric Structurementioning

confidence: 98%

“…Since the HD 53143 disk does not appear to have this feature, we exclude this extra parameter in our models for simplicity. Similarly, Lynch & Lovell (2022) allow the forced eccentricity to vary with semi-major axis, which we also do not include here but could impact the derived parameter constraints.…”

Section: Modeling Approachmentioning

confidence: 99%

ALMA Images the Eccentric HD 53143 Debris Disk

MacGregor,

Hurt,

Stark

et al. 2022

Preprint

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We present ALMA 1.3 mm observations of the HD 53143 debris disk -the first infrared or millimeter image produced of this ∼ 1 Gyr-old solar-analogue. Previous HST STIS coronagraphic imaging did not detect flux along the minor axis of the disk which could suggest a face-on geometry with two 'clumps' of dust. These ALMA observations reveal a disk with a strikingly different structure. In order to fit models to the millimeter visibilities and constrain the uncertainties on the disk parameters, we adopt an MCMC approach. This is the most eccentric debris disk observed to date with a forced eccentricity of 0.21 ± 0.02, nearly twice that of the Fomalhaut debris disk, and also displays apocenter glow. Although this eccentric model fits the outer debris disk well, there are significant interior residuals remaining that may suggest a possible edge-on inner disk, which remains unresolved in these observations. Combined with the observed structure difference between HST and ALMA, these results suggest a potential previous scattering event or dynamical instability in this system. We also note that the stellar flux changes considerably over the course of our observations, suggesting flaring at millimeter wavelengths. Using simultaneous TESS observations, we determine the stellar rotation period to be 9.6 ± 0.1 days.

show abstract

Eccentric debris disc morphologies – I. Exploring the origin of apocentre and pericentre glows in face-on debris discs

Cited by 9 publications

References 38 publications

Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628

Long-term Evolution of Warps in Debris Disks—Application to the Gyr-old System HD 202628

ALMA Images the Eccentric HD 53143 Debris Disk

ALMA Images the Eccentric HD 53143 Debris Disk

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