A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION

By Ilaria Pascucci, L. Testi, G. Herczeg, F. Long, C. Manara, Nathanial P. Hendler, G. Mulders, S. Krijt, F. Ciesla, Th. Henning and 6 more. 2016

225 citations recorded by the source corpus.

The disk mass is among the most important input parameter for every planet formation model to determine the number and masses of the planets that can form. We present an ALMA 887 μm survey of the disk population around objects from ∼2 to 0.03 M⊙ in the nearby ∼2 Myr old Chamaeleon I star-forming region. We detect thermal dust emission from 66 out of 93 disks, spatially resolve 34 of them, and identify two disks with large dust cavities of about 45 au in radius. Assuming isothermal and optically thin emission, we convert the 887 μm flux densities into dust disk masses, hereafter Mdust. We find that the relation is steeper than linear and of the form Mdust ∝ (M*)1.3–1.9, where the range in the power-law index reflects two extremes of the possible relation between the average dust temperature and stellar luminosity. By reanalyzing all millimeter data available for nearby regions in a self-consistent way, we show that the 1–3 Myr old regions of Taurus, Lupus, and Chamaeleon I share the same relation, while the 10 Myr old Upper Sco association has a steeper relation. Theoretical models of grain growth, drift, and fragmentation reproduce this trend and suggest that disks are in the fragmentation-limited regime. In this regime millimeter grains will be located closer in around lower-mass stars, a prediction that can be tested with deeper and higher spatial resolution ALMA observations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e600a3fdfc6678436e95e74da5b6c2d06251e648

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Citations in the corpus

Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, methodology): “On the contrary, the highest measured dust masses of protoplanetary disks at ∼1–3 Myr are ∼0.5–1 MJ around solar mass stars, and 0.01 MJ , ∼3 M⊕, around brown dwarfs (see also discussion by Pascucci et al. 2016).”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, methodology): “…observed 106 disks in the more evolved Upper Sco region (∼5–10 Myr at 145 pc; Preibisch et al. 2002; Pecaut et al. 2012) with sensitivities of Mdust∼0.1 M⊕; and Pascucci et al. (2016), who surveyed 93 protoplanetary disks in the young Chamaeleon I region (∼2–3 Myr at 160 pc; Luhman 2008) with…”
On the diversity and statistical properties of protostellar discs (2018, background): “Pascucci et al. (2016) deriveMd ∝M1.”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “If true, this rules out one of the scenarios proposed by Pascucci et al. (2016) to explain the steepening of the Mdust–”
A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, background): “…et al. 2016), environment (Jensen et al. 1994, 1996; Harris et al. 2012; Akeson & Jensen 2014; Mann & Williams 2009, 2010; Mann et al. 2014), and stellar host mass (Andrews et al. 2013; Mohanty et al. 2013; Carpenter et al. 2014; Ansdell et al. 2016; Barenfeld et al. 2016; Pascucci et al. 2016).”
One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering (2019, background): “Andrews et al. (2018a) also confirm the disk luminosity and stellar luminosity relationship found in Andrews et al. (2013); Ansdell et al. (2016); Pascucci et al. (2016).”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, methodology): “The stellar masses are then calculated from the Baraffe et al. (2015) and nonmagnetic Feiden (2016) evolutionary tracks, following Pascucci et al. (2016).”