THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS

By S. Andrews, K. Rosenfeld, A. Kraus, D. Wilner. 2013

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We present a substantial extension of the millimeter (mm) wave continuum photometry catalog for circumstellar dust disks in the Taurus star-forming region, based on a new “snapshot” λ = 1.3 mm survey with the Submillimeter Array. Combining these new data with measurements in the literature, we construct a mm-wave luminosity distribution, f(Lmm), for Class II disks that is statistically complete for stellar hosts with spectral types earlier than M8.5 and has a 3σ depth of roughly 3 mJy. The resulting census eliminates a longstanding selection bias against disks with late-type hosts, and thereby demonstrates that there is a strong correlation between Lmm and the host spectral type. By translating the locations of individual stars in the Hertzsprung–Russell diagram into masses and ages, and adopting a simple conversion between Lmm and the disk mass, Md, we confirm that this correlation corresponds to a statistically robust relationship between the masses of dust disks and the stars that host them. A Bayesian regression technique is used to characterize these relationships in the presence of measurement errors, data censoring, and significant intrinsic scatter: the best-fit results indicate a typical 1.3 mm flux density of ∼25 mJy for 1 M☉ hosts and a power-law scaling . We suggest that a reasonable treatment of dust temperature in the conversion from Lmm to Md favors an inherently linear Md∝M* scaling, with a typical disk-to-star mass ratio of ∼0.2%–0.6%. The measured rms dispersion around this regression curve is ±0.7 dex, suggesting that the combined effects of diverse evolutionary states, dust opacities, and temperatures in these disks imprint a full width at half-maximum range of a factor of ∼40 on the inferred Md (or Lmm) at any given host mass. We argue that this relationship between Md and M* likely represents the origin of the inferred correlation between giant planet frequency and host star mass in the exoplanet population, and provides some basic support for the core accretion model for planet formation. Moreover, we caution that the effects of incompleteness and selection bias must be considered in comparative studies of disk evolution, and illustrate that fact with statistical comparisons of f(Lmm) between the Taurus catalog presented here and incomplete subsamples in the Ophiuchus, IC 348, and Upper Sco young clusters.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/8b72078417ddb3de0b8a3e1f788fc65b55098aa0

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Citations in the corpus

Astrochemistry and compositions of planetary systems (2020, background): “A second possible explanation is that the observed chemistry depends on disk dynamics, which depends on disk mass, which in its turn correlates with stellar mass (Andrews et al. 2013).”
Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, background): “It has been shown that Article number, page 3 of 8 some dust mass can be confined into optically thick inner regions of disks (Tripathi et al. 2017; Ansdell et al. 2018) and that the opacity of disks and their temperature is still debatable (e.g., Andrews et al. 2013; Pascucci et al. 2016).”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, methodology): “For the old Baraffe et al. (1998) tracks, which in Andrews et al. (2013) are the most similar to the ones we use, the – *F Mmm slope in Taurus is 1.5±0.2, lower than but still marginally consistent with the one we find in ChamaeleonI.”
Dust Evolution and the Formation of Planetesimals (2016, background): “From these high angular resolution observations, the typical disk size is around 100AU, and the typical disk-to-host mass ratio is around 0.2–0.6% (Andrews et al. 2009, 2010, 2013).”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, methodology): “For example, as previously noted by Andrews et al. (2013), the Mdust–”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, positive): “The mass is also the fundamental parameter used in planet-formation synthesis (e.g. Mordasini et al. 2009a) since it is expected to scale with the mass of the disk, for the mass range considered here (Andrews et al. 2013).”
A STELLAR-MASS-DEPENDENT DROP IN PLANET OCCURRENCE RATES (2014, background): “…environments of planets— protoplanetary disks—show strong scaling with stellar mass for fundamental properties such as disk mass (Mohanty et al. 2013; Andrews et al. 2013), mass accretion rate (e.g., Hartmann et al. 2006; Alcalá et al. 2014), inner disk radius (Monnier & Millan-Gabet 2002;…”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “Although Andrews et al. (2013) derived the relation Tdust = 25K × (L?”
Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, background): “This trend would be the result of two competing factors: high-mass stars have more massive disks (e.g. Andrews et al. 2013), and so are more likely to form gas giants.”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, methodology): “The disk dust masses are calculated with updated Gaia DR2 distance for individual objects with millimeter fluxes adopted from our measurements for the 12 disks and adopted from Andrews et al. (2013) for the other Taurus members.”
BREEDING SUPER-EARTHS AND BIRTHING SUPER-PUFFS IN TRANSITIONAL DISKS (2015, background): “As for M dwarf disks, we posit that their surface densities are systematically lower than those of their FGK counterparts (see also Laughlin et al. 2004; Andrews et al. 2013; cf. Kornet et al. 2006), so much so that they almost never produce gas giants, but instead make super-Earths everywhere.”
Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “From mm-surveys it seems such disc masses for solar like stars show a large spread between 10−4–10−1 M (Andrews et al. 2013) and therefore the disc mas in our model lies in the higher end of this distribution.”
A PARAMETRIC MODELING APPROACH TO MEASURING THE GAS MASSES OF CIRCUMSTELLAR DISKS (2013, methodology): “Following Andrews et al. (2013) we scale the dust temperature with the stellar luminosity, Tdust = 25(Lstar/L ) 1/4 K.”
Gravitational Instabilities in Circumstellar Disks (2016, methodology): “The most comprehensive survey for disk masses at this time is that of Andrews et al. (2013), who survey all known members of the nearby star forming region Taurus.”
ALMA SURVEY OF LUPUS PROTOPLANETARY DISKS. I. DUST AND GAS MASSES (2016, methodology): “The first statistically robust confirmation of this correlation was by Andrews et al. (2013) for Class II disks in the young (∼1–2 Myr) Taurus region.”
Imaging Extrasolar Giant Planets (2016, background): “Brown Dwarfs Young brown dwarfs (≈13–75 MJup) have low circum-substellar disk masses (Mohanty et al. 2013; Andrews et al. 2013) and are not expected to host giant planets as frequently as stars.”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “We base that behavior on the analysis of a suite of radiative transfer models of representative disks by Andrews et al. (2013) and set Td(r) ≈ T10 ( L∗ L )1/4 ( r 10 AU )−1/2 (9) where T10 = 30±5 K is the temperature at 10 AU and L∗ is the stellar host luminosity.”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “The studies that provided those data are biased toward brighter continuum sources, which permeates to the host properties since the continuum luminosity scales steeply with M∗ (Andrews et al. 2013; Mohanty et al. 2013) and Ṁ∗ (Manara et al. 2016; Mulders et al. 2017).”