| DOI | Resolve DOI: https://doi.org/10.1093/mnras/stab1901 |
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| Author | Search for: Norfolk, Brodie J.; Search for: Maddison, Sarah T.; Search for: Marshall, Jonathan P.; Search for: Kennedy, Grant M.ORCID identifier: https://orcid.org/0000-0001-6831-7547; Search for: Duchêne, Gaspard; Search for: Wilner, David J.; Search for: Pinte, ChristopheORCID identifier: https://orcid.org/0000-0001-5907-5179; Search for: Moór, Attila; Search for: Matthews, Brenda1; Search for: Ábrahám, Péter; Search for: Kóspál, Ágnes; Search for: Van der Marel, Nienke1 |
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| Affiliation | - National Research Council of Canada. Herzberg Astronomy and Astrophysics
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| Funder | Search for: Royal Society; Search for: Ministry of Science and Technology of Taiwan; Search for: Academia Sinica; Search for: NKFIH; Search for: CSIRO; Search for: NASA; Search for: National Science Foundation |
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| Format | Text, Article |
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| Subject | techniques: interferometric; planets and satellites: dynamical evolution and stability; circumstellar matter; planetary systems |
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| Abstract | Millimetre continuum observations of debris discs can provide insights into the physical and dynamical properties of the unseen planetesimals that these discs host. The material properties and collisional models of planetesimals leave their signature on the grain size distribution, which can be traced through the millimetre spectral index. We present 8.8 mm observations of the debris discs HD 48370, CPD-72 2713, HD 131488, and HD 32297 using the Australian Telescope Compact Array (ATCA) as part of the PLanetesimals Around TYpical Pre-main-seqUence Stars (PLATYPUS) survey. We detect all four targets with a characteristic beam size of 5 arcsec and derive a grain size distribution parameter that is consistent with collisional cascade models and theoretical predictions for parent planetesimal bodies where binding is dominated by self-gravity. We combine our sample with 19 other millimetre-wavelength-detected debris discs from the literature and calculate a weighted mean grain size power-law index that is close to analytical predictions for a classical steady-state collisional cascade model. We suggest the possibility of two distributions of q in our debris disc sample; a broad distribution (where q ∼ 3.2–3.7) for ‘typical’ debris discs (gas-poor/non-detection), and a narrow distribution (where q < 3.2) for bright gas-rich discs. Or alternatively, we suggest that there exists an observational bias between the grain size distribution parameter and absolute flux that may be attributed to the detection rates of faint debris discs at ∼ cm wavelengths. |
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| Publication date | 2021-07-06 |
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| Publisher | Oxford Academic
Royal Astronomical Society |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 87ca0b13-376e-4df2-ba80-c98cb5bbdf7d |
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| Record created | 2023-01-17 |
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| Record modified | 2023-01-17 |
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