Dust mass in protoplanetary disks with porous dust opacities
arXiv:2411.00277 · doi:10.1051/0004-6361/202451981
Abstract
ALMA surveys have suggested that protoplanetary disks are not massive enough to form the known exoplanet population, under the assumption that the millimeter continuum emission is optically thin. In this work, we investigate how the mass determination is influenced when the porosity of dust grains is considered in radiative transfer models. The results show that disks with porous dust opacities yield similar dust temperature, but systematically lower millimeter fluxes compared to disks incorporating compact dust grains. Moreover, we recalibrate the relation between dust temperature and stellar luminosity for a wide range of stellar parameters, and calculate the dust masses of a large sample of disks using the traditionally analytic approach. The median dust mass from our calculation is about 6 times higher than the literature result, and this is mostly driven by the different opacities of porous and compact grains. A comparison of the cumulative distribution function between disk dust masses and exoplanet masses show that the median exoplanet mass is about 2 times lower than the median dust mass, if grains are porous, and there are no exoplanetary systems with masses higher than the most massive disks. Our analysis suggests that adopting porous dust opacities may alleviate the mass budget problem for planet formation. As an example illustrating the combined effects of optical depth and porous dust opacities on the mass estimation, we conduct new IRAM/NIKA-2 observations toward the IRAS 04370+2559 disk and perform a detailed radiative transfer modeling of the spectral energy distribution. The best-fit dust mass is roughly 100 times higher than the value from the traditionally analytic calculation. Future spatially resolved observations at various wavelengths are required to better constrain the dust mass.
11 pages, 7 figures, Accepted for publication in A&A
References in corpus (40)
- Gaia Data Release 3: Summary of the content and survey properties
- New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit
- Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores
- A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation
- A Millimeter Continuum Size-Luminosity Relationship for Protoplanetary Disks
- One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering
- Dust masses of young disks: constraining the initial solid reservoir for planet formation
- Four annular structures in a protostellar disk less than 500,000 years old
- Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results
- The anomalously low (sub)millimeter spectral indices of some protoplanetary disks may be explained by dust self-scattering
- Characterizing the dust content of disk substructures in TW Hya
- ALMA survey of Class II protoplanetary disks in Corona Australis: a young region with low disk masses
- Tracing water vapor and ice during dust growth
- The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks
- Distribution of solids in the rings of the HD 163296 disk: a multiwavelength study
- Far-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions
- Effect of dust size and structure on scattered light images of protoplanetary discs
- Protoplanetary Disk Masses from Radiative Transfer Modeling: A Case Study in Taurus
- The first ALMA survey of protoplanetary discs at 3 mm: demographics of grain growth in the Lupus region
- Reflections on nebulae around young stars: A systematic search for late-stage infall of material onto Class II disks
- Submillimeter Structure of the Disk of the Butterfly Star
- Fractal aggregates of sub-micron-sized grains in the young planet-forming disk around IM Lup
- Porous dust grains in debris disks
- Intrinsic polarisation of elongated porous dust grains
- Porous Dust Particles in Protoplanetary Disks: Application to the HL Tau Disk
- Effect of dust grain porosity on the appearance of protoplanetary disks
- The properties of the inner disk around HL Tau: Multi-wavelength modeling of the dust emission
- An ALMA Survey of Protoplanetary Disks in Lynds 1641
- Measuring the Dust Masses of Protoplanetary Disks in Lupus with ALMA: Evidence that Disks can be Optically Thick at 3 mm
- On the underestimation of dust mass in protoplanetary disks: Effects of disk structure and dust properties
- Support for fragile porous dust in a gravitationally self-regulated disk around IM Lup
- Dust mineralogy and variability of the inner PDS 70 disk
- Chemical evolution in ices on drifting, planet-forming pebbles
- Determining Dust Properties in Protoplanetary Disks: SED-derived Masses and Settling With ALMA
- Into the thick of it: ALMA 0.45 mm observations of HL Tau at 2 au resolution
- Observed polarized scattered light phase functions of planet-forming disks
- The circumstellar disk of FS Tau B - A self-consistent model based on observations in the mid-infrared with NACO -
- Compaction during fragmentation and bouncing produces realistic dust grain porosities in protoplanetary discs
- Self-scattering on large, porous grains in protoplanetary disks with dust settling
- Constraining Millimeter Dust Emission in Nearby Galaxies with NIKA2: the case of NGC2146 and NGC2976