Evidence for a correlation between mass accretion rates onto young stars and the mass of their protoplanetary disks

Manara, C. F.; Rosotti, Giovanni; Testi, L.; Natta, A.; Alcalá, J. M.; Williams, Jonathan P.; Ansdell, Megan; Miotello, A.; Marel, Nienke van der; Tazzari, Marco; Carpenter, John M.; Guidi, Greta; Mathews, Geoffrey S.; Oliveira, I.; Prusti, T.; Dishoeck, E. F. van

doi:10.1051/0004-6361/201628549

Cited by 192 publications

(253 citation statements)

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“…For simple evolving disk models treated with an exponentially declining accretion rate, we require IOPF to be completed within this decay time, ∼1 Myr, in order to preserve the observed relatively flat scaling of planet mass with orbital radius. We note that IOPF's apparent preference for accretion rates of~-- m M 10 yr 9 1 is quite consistent with the observed accretion rates of young stellar objects, including transition disk systems (e.g., Williams & Cieza 2011;Manara et al 2014Manara et al , 2016. At even lower accretion rates, the rate of photoevaporation of the disk may become comparable, potentially terminating or greatly reducing the supply of gas to the inner disk (e.g., Ercolano et al 2009;Owen et al 2012;Ercolano et al 2014).…”

Section: Discussionsupporting

confidence: 75%

Inside-out Planet Formation. IV. Pebble Evolution and Planet Formation Timescales

Tan

Zhu

et al. 2018

ApJ

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Systems with tightly packed inner planets (STIPs) are very common. Chatterjee & Tan proposed Inside-out Planet Formation (IOPF), an in situ formation theory, to explain these planets. IOPF involves sequential planet formation from pebble-rich rings that are fed from the outer disk and trapped at the pressure maximum associated with the dead zone inner boundary (DZIB). Planet masses are set by their ability to open a gap and cause the DZIB to retreat outwards. We present models for the disk density and temperature structures that are relevant to the conditions of IOPF. For a wide range of DZIB conditions, we evaluate the gap-opening masses of planets in these disks that are expected to lead to the truncation of pebble accretion onto the forming planet. We then consider the evolution of dust and pebbles in the disk, estimating that pebbles typically grow to sizes of a few centimeters during their radial drift from several tens of astronomical units to the inner, 1 au scale disk. A large fraction of the accretion flux of solids is expected to be in such pebbles. This allows us to estimate the timescales for individual planet formation and the entire planetary system formation in the IOPF scenario. We find that to produce realistic STIPs within reasonable timescales similar to disk lifetimes requires disk accretion rates of ∼10 −9 M e yr −1 and relatively low viscosity conditions in the DZIB region, i.e., a Shakura-Sunyaev parameter of α∼10 .

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Section: Discussionsupporting

confidence: 75%

Inside-out Planet Formation. IV. Pebble Evolution and Planet Formation Timescales

Tan

Zhu

et al. 2018

ApJ

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“…All observational data used in this analysis were previously published; the ALMA data surveys of disk masses were presented by Ansdell et al (2016) and Pascucci et al (2016); the X-Shooter surveys of mass accretion rates were presented by Alcalá et al (2014Alcalá et al ( , 2017 and Manara et al (2014Manara et al ( , 2016aManara et al ( , 2017. The dust mass and mass accretion in Lupus were jointly analyzed by Manara et al (2016b).…”

Section: Homogeneous Analysis Of Stellar and Disk Propertiesmentioning

confidence: 99%

“…Using a stellar-mass-independent temperature avoids introducing a correlated error between dust mass and stellar mass. While a disk temperature that decreases with stellar mass flattens the M dust - M relation (e.g., Pascucci et al 2016) and weakens the M dust -Ṁ acc relation (Manara et al 2016b), the intrinsic scatter around the M dust -Ṁ acc relation remains unchanged. Hence, we focus our analysis on understanding the scatter more than the slope of the M dust -Ṁ acc relation.…”

Section: Chamaeleon Imentioning

confidence: 99%

“…Recent surveys of nearby star-forming regions are enabling us for the first time to test this prediction on statistically significant samples where mass accretion rates and disk masses are available for the same objects. Manara et al (2016b) used 66 objects from the ∼1-3 Myr old Lupus star-forming region with mass accretion rates homogeneously computed from VLT/XShooter spectra and disk masses from submillimeter continuum emission from the Atacama Large Millimeter/submillimeter Array (ALMA). The relation between mass accretion rates and dust disk masses is found to be roughly consistent with viscously evolved disks.…”

Section: Introductionmentioning

confidence: 99%

“…Here, we expand on this study by combining the ALMA and X-Shooter surveys of disks in the Lupus and Chamaeleon I star-forming regions, thus more than doubling the sample of Manara et al (2016b) (Section 2). First, we investigate the relation between dust mass, mass accretion rate, and stellar mass (Section 3).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Constraints from Dust Mass and Mass Accretion Rate Measurements on Angular Momentum Transport in Protoplanetary Disks

Mulders

Pascucci

Manara

et al. 2017

ApJ

123

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In this paper, we investigate the relation between disk mass and mass accretion rate to constrain the mechanism of angular momentum transport in protoplanetary disks. We find a correlation between dust disk mass and mass accretion rate in Chamaeleon I with a slope that is close to linear, similar to the one recently identified in Lupus. We investigate the effect of stellar mass and find that the intrinsic scatter around the best-fit M dust - M andṀ acc - M relations is uncorrelated. We simulate synthetic observations of an ensemble of evolving disks using a Monte Carlo approach and find that disks with a constant α viscosity can fit the observed relations between dust mass, mass accretion rate, and stellar mass but overpredict the strength of the correlation between disk mass and mass accretion rate when using standard initial conditions. We find two possible solutions. In the first one, the observed scatter in M dust andṀ acc is not primordial, but arises from additional physical processes or uncertainties in estimating the disk gas mass. Most likely grain growth and radial drift affect the observable dust mass, while variability on large timescales affects the mass accretion rates. In the second scenario, the observed scatter is primordial, but disks have not evolved substantially at the age of Lupus and Chamaeleon I owing to a low viscosity or a large initial disk radius. More accurate estimates of the disk mass and gas disk sizes in a large sample of protoplanetary disks, through either direct observations of the gas or spatially resolved multiwavelength observations of the dust with ALMA, are needed to discriminate between both scenarios or to constrain alternative angular momentum transport mechanisms such as MHD disk winds.

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Planetary Population Synthesis

Mordasini¹

2018

Handbook of Exoplanets

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In stellar astrophysics, the technique of population synthesis has been successfully used for several decades. For planets, it is in contrast still a young method which only became important in recent years because of the rapid increase of the number of known extrasolar planets, and the associated growth of statistical observational constraints. With planetary population synthesis, the theory of planet formation and evolution can be put to the test against these constraints. In this review of planetary population synthesis, we first briefly list key observational constraints. Then, the work flow in the method and its two main components are presented, namely global end-to-end models that predict planetary system properties directly from protoplanetary disk properties and probability distributions for these initial conditions. An overview of various population synthesis models in the literature is given. The sub-models for the physical processes considered in global models are described: the evolution of the protoplanetary disk, the planets' accretion of solids and gas, orbital migration, and N-body interactions among concurrently growing protoplanets. Next, typical population synthesis results are illustrated in the form of new syntheses obtained with the latest generation of the Bern model. Planetary formation tracks, the distribution of planets in the mass-distance and radius-distance plane, the planetary mass function, and the distributions of planetary radii, semimajor axes, and luminosities are shown, linked to underlying physical processes, and compared with their observational counterparts. We finish by highlighting the most important predictions made by population synthesis models and discuss the lessons learned from these predictions -both those later observationally confirmed and those rejected.

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Evidence for a correlation between mass accretion rates onto young stars and the mass of their protoplanetary disks

Cited by 192 publications

References 100 publications

Inside-out Planet Formation. IV. Pebble Evolution and Planet Formation Timescales

Inside-out Planet Formation. IV. Pebble Evolution and Planet Formation Timescales

Constraints from Dust Mass and Mass Accretion Rate Measurements on Angular Momentum Transport in Protoplanetary Disks

Planetary Population Synthesis

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