J/A+A/673/A78 1D disc evolution models (Emsenhuber+, 2023)
Towards a population synthesis of discs and planets.
II. Confronting disc models and observations at the population level.
Emsenhuber A., Burn R., Weder J., Monsch K., Picogna G., Ercolano B.,
Preibisch T.
<Astron. Astrophys. 673, A78 (2023)>
=2023A&A...673A..78E 2023A&A...673A..78E (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Stars, double and multiple ; Exoplanets
Keywords: protoplanetary disk - methods: numerical
Abstract:
We want to find the distribution of initial conditions that best
reproduces disc observations at the population level.
We first run a parameter study using a 1D model that includes the
viscous evolution of a gas disc, dust, and pebbles, coupled with an
emission model to compute the mm flux observable with ALMA. This is
used to train a machine learning surrogate model, which can compute
the relevant quantity for comparison with observations in seconds.
This surrogate model is used to perform parameter studies and
synthetic disc populations.
Performing parameter study, we find that internal photoevaporation
lead to lower dependency of disc lifetimes on stellar mass than
external photoevaporation. This dependence should be investigated in
the future. Performing population synthesis, we find that under the
combined losses of internal and external photoevaporation, discs are
too short lived.
To match observational constraints, future models of disc evolution
need to include either or all of the following processes: infall of
material to replenish the discs, shielding of the disc from internal
photoevaporation due to magnetically-driven disc winds, and extinction
of external high-energy radiation. Nevertheless, disc properties in
low-external photoevaporation regions can be reproduced by having more
massive and compact discs. Here, the optimum values of the alpha
viscosity parameter lie between 3*10-4 and 10-3 and with internal
photoevaporation being the main mode of disc dispersal.
Description:
A set of 119999 1D radial disc evolution models are presented. The
models include viscous evolution of the gas, dust growth into pebbles,
drift and advection of dust and pebbles caused by the gas, and losses
by internal and external photoevaporation.
Two parameter studies with initial conditions selected using Latin
hypercube sampling (LHS) were performed. For each model, the initial
conditions and the corresponding results are given. Outcomes include
disc lifetime, measured either on a critical mass and surface density
criterion, or based on the observability in the near-IR. Also, the
results contain two sets, one at 105 and one at 2*106yr of stellar
accretion rate, observable dust disc masses, and radii.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 301 100000 Training and validation data
table4.dat 301 19999 Testing data
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Byte-by-byte Description of file: table3.dat table4.dat
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Bytes Format Units Label Explanations
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1- 3 F3.1 Msun Mstar Mass of the central star
6- 19 E14.8 --- Mdiskf Gas disc-to-star initial mass ratio
22- 35 E14.8 --- expo Power-law index of the initial profile
38- 51 E14.8 d Period Orbital period at the inner edge
54- 67 E14.8 AU aout Charateristic radius of the
initial profile
70- 83 E14.8 --- alpha Turbulent viscosity parameter
86- 99 E14.8 --- fpg Initial dust-to-gas mass ratio
in the disc
102-115 E14.8 cm/s Vfrag Fragmentation velocity
118-131 E14.8 --- peff Planetesimals formation efficiency
134-147 E14.8 --- fdrift Drift efficiency factor
150-163 E14.8 10+23W LX Stellar X-ray luminosity
166-179 E14.8 1.6x10-6kg/s3 UVfs Ambient UV field strength
182-192 E11.8 yr dltMass Disc lifetime based on mass criterion (1)
195-205 E11.8 yr dltNIR Disc lifetime based on near-IR
criterion (2)
208-221 E14.8 Msun/yr Acc1e5 Stellar accretion rate at 100kyr (3)
224-237 E14.8 Msun Mobs1e5 Observable dust mass at 100kyr (3)
240-253 E14.8 AU r681e5 Radius containing 68% of the flux
at 100kyr (3)
256-269 E14.8 Msun/yr Acc2e6 Stellar accretion rate at 2Myr (3)
272-285 E14.8 Msun Mobs2e6 Observable dust mass at 2Myr (3)
288-301 E14.8 AU r68e6 Radius containing 68% of the flux at
2Myr (3)
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Note (1): Value is set to zero if the disc lifetime is longer than 100Myr
(maximum simulation time)
Note (2): Value is set to zero if the near-IR observability criterion is
fulfilled until dispersal based on the mass criterion
Note (3): Value is set to zero if the disc lifetime (based on the mass
criterion) is is shorter than the epoch
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Acknowledgements:
Alexandre Emsenhuber, emsenhuber(at)usm.lmu.de
(End) Patricia Vannier [CDS] 12-Dec-2022