The temporal requirements of directly observing self-gravitating spiral waves in protoplanetary discs with ALMA

Abstract

We investigate how the detectability of signatures of self-gravity in a protoplanetary disc depends on its temporal evolution. We run a one-dimensional model for secular timescales to follow the disc mass as a function of time. We then combine this with three-dimensional global hydrodynamics simulations that employ a hybrid radiative transfer method to approximate realistic heating and cooling. We simulate ALMA continuum observations of these systems, and find that structures induced by the gravitational instability (GI) are readily detectable when $q=M_{\mathrm{disc}}/M_{\ast }\gtrsim 0.25$ and $R_{\mathrm{outer}}\lesssim 100$ au. The high accretion rate generated by gravito-turbulence in such a massive disc drains its mass to below the detection threshold in $\sim 10^4$ years, or approximately 1 % of the typical disc lifetime. Therefore, discs with spiral arms detected in ALMA dust observations, if generated by self-gravity, must either be still receiving infall to maintain a high $q$ value, or have just emerged from their natal envelope. Detection of substructure in systems with lower $q$ is possible, but would require a specialist integration with the most extended configuration over several days. This disfavours the possibility of GI-caused spiral structure in systems with $q<0.25$ being detected in relatively short integration times, such as those found in the DSHARP ALMA survey (Andrews et al. 2018; Huang et al. 2018). We find no temporal dependence of detectability on dynamical timescales

13 pages, 6 figures

References in corpus (24)

• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Protoplanetary Disk Structures in Ophiuchus
• X-Shooter spectroscopy of young stellar objects in Lupus: Accretion properties of class II and transitional objects
• Spiral Density Waves in a Young Protoplanetary Disk
• Asymmetric features in the protoplanetary disk MWC758
• Direct Imaging of Fine Structures in Giant Planet Forming Regions of the Protoplanetary Disk around AB Aurigae
• A Triple Protostar System Formed via Fragmentation of a Gravitationally Unstable Disk
• The Coupled Physical Structure of Gas and Dust in the IM Lup Protoplanetary Disk
• Fragmentation of gravitationally unstable gaseous protoplanetary disks with radiative transfer
• The Disk Substructures at High Angular Resolution Project (DSHARP): III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
• Why Do T Tauri Disks Accrete?
• The minimum mass for star formation, and the origin of binary brown dwarfs
• Radiative transfer and the energy equation in SPH simulations of star formation
• The Disk Substructures at High Angular Resolution Project (DSHARP): IV. Characterizing substructures and interactions in disks around multiple star systems
• On the Distance to the Ophiuchus Star-Forming Region
• Grand Design Spiral Arms in A Young Forming Circumstellar Disk
• Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: The effect of fragment-fragment interactions
• Introducing a Hybrid Method of Radiative Transfer for Smoothed Particle Hydrodynamics
• On the reliability of protostellar disc mass measurements and the existence of fragmenting discs
• The chemistry of protoplanetary fragments formed via gravitational instabilities
• Identifying and Analysing Protostellar Disc Fragments in Smoothed Particle Hydrodynamics Simulations
• How to Detect the Signatures of Self-Gravitating Circumstellar Discs with the Atacama Large Millimetre/sub-millimetre Array
• Grand challenges in protoplanetary disc modelling
• Gravitational instabilities in a protosolar-like disc II: continuum emission and mass estimates

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• Gravitoviscous Protoplanetary Discs with a Dust Component. IV. Disc Outer Edges, Spectral Indices, and Opacity Gaps
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• The observational impact of dust trapping in self-gravitating discs
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• Testing velocity kinks as a planet-detection method: Do velocity kinks in surface gas emission trace planetary spiral wakes in the midplane continuum?
• Global Spiral Density Wave Modes in Protoplanetary Disks: Morphology of Spiral Arms
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• Winding Motion of Spirals in a Gravitationally Unstable Protoplanetary Disk
• Observational Signatures of Planets in Protoplanetary Disks: Temperature structures in spiral arms
• Constraining protoplanetary disc mass using the GI wiggle
• Evolution of the Accretion Rate of Young Intermediate Mass Stars: Implications for Disk Evolution and Planet Formation