A Deep Search for Five Molecules in the 49 Ceti Debris Disk

Klusmeyer, Jessica; Hughes, A. Meredith; Matrà, Luca; Flaherty, Kevin; Kóspál, Á.; Moór, A.; Roberge, Aki; Öberg, Karin I.; Boley, Aaron C.; White, Jacob Aaron; Wilner, David J.; Ábrahám, P.

doi:10.3847/1538-4357/ac1583

Cited by 7 publications

(5 citation statements)

References 59 publications

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“…Not only CO (or isotopes of CO) have been detected, but also O (Riviere-Marichalar et al 2012, Brandeker et al 2016, Kral et al 2016, C (Cataldi et al 2018, Kral et al 2019, and C (Cataldi et al 2014), at far-infrared or sub-mm wavelengths. Nonetheless, other molecules such as HCN or HCO + seem to be largely absent in CO-rich debris disks (Matrà et al 2018, Smirnov-Pinchukov et al 2021, Klusmeyer et al 2021 ). More stochastic events such as falling evaporating bodies (Beust et al 2001) can be detected using optical spectroscopic observations, tracing other lines (in absorption) such as Ca or Na , if the gas is in the line of sight of the star (e.g., Kiefer et al 2014, Rebollido et al 2018, Iglesias et al 2018, Rebollido et al 2020.…”

Section: Introductionmentioning

confidence: 99%

The vertical structure of debris disks and the impact of gas

Olofsson,

Thébault,

Kral

et al. 2022

Preprint

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The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate of the unseen planetesimals. Thanks to the ever-increasing angular resolution of contemporary instruments and facilities, we are beginning to constrain the scale height of a handful of debris disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here the geometric modeling of eight disks close to edge-on, all observed with the same instrument (SPHERE) and using the same mode (dual-beam polarimetric imaging). Motivated by the presence of CO gas in two out of the eight disks, we then investigate the impact that gas can have on the scale height by performing N-body simulations including gas drag and collisions. We show that gas can quickly alter the dynamics of particles (both in the radial and vertical directions), otherwise governed by gravity and radiation pressure. We find that, in the presence of gas, particles smaller than a few tens of microns can efficiently settle toward the midplane at the same time as they migrate outward beyond the birth ring. For second generation gas (𝑀 gas ≤ 0.1 𝑀 ⊕ ), the vertical settling should be best observed in scattered light images compared to observations at millimeter wavelengths. But if the gas has a primordial origin (𝑀 gas ≥ 1 𝑀 ⊕ ), the disk will appear very flat both at near-infrared and sub-mm wavelengths. Finally, far beyond the birth ring, our results suggest that the surface brightness profile can be as shallow as ∼ −2.25.

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Section: Introductionmentioning

confidence: 99%

The vertical structure of debris disks and the impact of gas

Olofsson,

Thébault,

Kral

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Not only CO (or isotopes of CO) have been detected, but also O I (Riviere-Marichalar et al 2012 ;Brandeker et al 2016 ;Kral et al 2016 ), C I (Cataldi et al 2018, Kral et al 2019, and C II (Cataldi et al 2014 ), at farinfrared or sub-mm wavelengths. None the less, other molecules such as HCN or HCO + seem to be largely absent in CO-rich debris discs (Matr à et al 2018 ;Klusmeyer et al 2021 ;Smirno v-Pinchuko v et al 2021 ). More stochastic events such as falling evaporating bodies (Beust, Karmann & Lagrange 2001 ) can be detected using optical spectroscopic observations, tracing other lines (in absorption) such as Ca II or Na I , if the gas is in the line of sight of the star (e.g.…”

Section: Introductionmentioning

confidence: 99%

The vertical structure of debris discs and the impact of gas

Olofsson

Thébault

Kral

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate of the unseen planetesimals. Thanks to the ever-increasing angular resolution of contemporary instruments and facilities, we are beginning to constrain the scale height of a handful of debris disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here the geometric modeling of eight disks close to edge-on, all observed with the same instrument (SPHERE) and using the same mode (dual-beam polarimetric imaging). Motivated by the presence of CO gas in two out of the eight disks, we then investigate the impact that gas can have on the scale height by performing N-body simulations including gas drag and collisions. We show that gas can quickly alter the dynamics of particles (both in the radial and vertical directions), otherwise governed by gravity and radiation pressure. We find that, in the presence of gas, particles smaller than a few tens of microns can efficiently settle toward the midplane at the same time as they migrate outward beyond the birth ring. For second generation gas (Mgas ≤ 0.1 M⊕), the vertical settling should be best observed in scattered light images compared to observations at millimeter wavelengths. But if the gas has a primordial origin (Mgas ≥ 1 M⊕), the disk will appear very flat both at near-infrared and sub-mm wavelengths. Finally, far beyond the birth ring, our results suggest that the surface brightness profile can be as shallow as ∼−2.25.

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“…The edge-on, gas-rich debris disk around 49 Ceti has been the subject of multiple detailed studies over the past years (some of the more recent work includes Higuchi et al 2019aHiguchi et al , 2019bHiguchi et al , 2020Moór et al 2019;Pawellek et al 2019;Klusmeyer et al 2021). Hughes et al (2017) presented two non-LTE models of the CO disk around 49 Ceti with CO/H 2 abundances of 10 −4 (representing a primordial gas) and 1 (representing a secondary gas).…”

Section: Appendix a Continuum Fluxesmentioning

confidence: 99%

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Cataldi

Aikawa

Iwasaki

et al. 2023

ApJ

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The origin and evolution of gas in debris disks are still not well understood. Secondary gas production from cometary material or a primordial origin have been proposed. So far, observations have mostly concentrated on CO, with only a few C observations available. We overview the C and CO content of debris disk gas and test state-of-the-art models. We use new and archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO and C i emission, complemented by C ii data from Herschel, for a sample of 14 debris disks. This expands the number of disks with ALMA measurements of both CO and C i by 10 disks. We present new detections of C i emission toward three disks: HD 21997, HD 121191, and HD 121617. We use a simple disk model to derive gas masses and column densities. We find that current state-of-the-art models of secondary gas production overpredict the C0 content of debris disk gas. This does not rule out a secondary origin, but might indicate that the models require an additional C removal process. Alternatively, the gas might be produced in transient events rather than a steady-state collisional cascade. We also test a primordial gas origin by comparing our results to a simplified thermochemical model. This yields promising results, but more detailed work is required before a conclusion can be reached. Our work demonstrates that the combination of C and CO data is a powerful tool to advance our understanding of debris disk gas.

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A Deep Search for Five Molecules in the 49 Ceti Debris Disk

Cited by 7 publications

References 59 publications

The vertical structure of debris disks and the impact of gas

The vertical structure of debris disks and the impact of gas

The vertical structure of debris discs and the impact of gas

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

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