Revealing the dynamics of Class 0 protostellar discs with ALMA

Seifried, D.; Sánchez-Monge, Á.; Walch, Stefanie; Banerjee, Rinti

doi:10.1093/mnras/stw785

Cited by 55 publications

(71 citation statements)

References 65 publications

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“…This also applies to previous studies of the detectability of GI clumps for ALMA, such as in 3D MHD protostellar disk collapse simulations (Seifried et al 2016) and in 2D massive embedded disks fragmenting predominantly into brown-dwarf-sized objects (Vorobyov et al 2013). Also, Stamatellos et al (2011) included an approximate treatment of radiative transfer and focused on detectability by IRAM.…”

Section: Introductionsupporting

confidence: 60%

Direct Detection of Precursors of Gas Giants Formed by Gravitational Instability With the Atacama Large Millimeter/Submillimeter Array

Mayer

Peters

Pineda

et al. 2016

ApJL

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Phases of gravitational instability are expected in the early phases of disk evolution, when the disk mass is still a substantial fraction of the mass of the star. Disk fragmentation into sub-stellar objects could occur in the cold exterior part of the disk. Direct detection of massive gaseous clumps on their way to collapse into gas giant planets would offer an unprecedented test of the disk instability model. Here we use state-of-the-art 3D radiation-hydro simulations of disks undergoing fragmentation into massive gas giants, post-processed with RADMC-3D to produce dust continuum emission maps. These are then fed into the Common Astronomy Software Applications (CASA) ALMA simulator. The synthetic maps show that both overdense spiral arms and actual clumps at different stages of collapse can be detected with the Atacama Large Millimeter/submillimeter Array (ALMA) in the full configuration at the distance of the Ophiuchus star forming region (125 pc). The detection of clumps is particularly effective at shorter wavelengths (690 GHz) combining two resolutions with multi-scale clean. Furthermore, we show that a flux-based estimate of the mass of a protoplanetary clump can be comparable to a factor of three higher than the gravitationally bound clump mass. The estimated mass depends on the assumed opacity, and on the gas temperature, which should be set using the input of radiation-hydro simulations. We conclude that ALMA has the capability to detect "smoking gun" systems that are a signpost of the disk instability model for gas giant planet formation.

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Section: Introductionsupporting

confidence: 60%

Direct Detection of Precursors of Gas Giants Formed by Gravitational Instability With the Atacama Large Millimeter/Submillimeter Array

Mayer

Peters

Pineda

et al. 2016

ApJL

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“…We see that the velocity curves provide a good fit to the emission peak in each velocity channel. For each diagram, we also plot the outermost Keplerian curve that is tangential to the first emission contour, with a 6σ threshold 8 (see Seifried et al 2016;Ginsburg et al 2018, for a justification of the method). We obtain M (sin i) 2 = 0.7 M , 0.6 M and 0.4 M for the 13 CO (2 − 1), C 18 O (2 − 1), and SO (5 6 − 4 5 ) lines, respectively.…”

Section: Sourcementioning

confidence: 99%

Searching for kinematic evidence of Keplerian disks around Class 0 protostars with CALYPSO

Maret

Maury

Беллоче

et al. 2020

A&A

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The formation of protoplanetary disks is not well understood. To understand how and when these disks are formed, it is crucial to characterize the kinematics of the youngest protostars at a high angular resolution. Here we study a sample of 16 Class 0 protostars to measure their rotation profile at scales from 50 to 500 au and search for Keplerian rotation. We used high-angular-resolution line observations obtained with the Plateau de Bure Interferometer as part of the CALYPSO large program. From 13 CO (J = 2 − 1), C 18 O (J = 2 − 1) and SO (N j = 5 6 − 4 5 ) moment maps, we find that seven sources show rotation about the jet axis at a few hundred au scales: SerpS-MM18, L1448-C, L1448-NB, L1527, NGC1333-IRAS2A, NGC1333-IRAS4B, and SVS13-B. We analyzed the kinematics of these sources in the uv plane to derive the rotation profiles down to 50 au scales. We find evidence for Keplerian rotation in only two sources, L1527 and L1448-C. Overall, this suggests that Keplerian disks larger than 50 au are uncommon around Class 0 protostars. However, in some of the sources, the line emission could be optically thick and dominated by the envelope emission. Due to the optical thickness of these envelopes, some of the disks could have remained undetected in our observations.

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“…We note that there is also significant red/blueshifted emission in the SW/NE side of the disk. This could be an indication of infall motions, although MHD simulation of disk formation and evolution shows that this can be also a projection effect for significant inclinations (e.g., Seifried et al 2016). In order to constrain the dynamical mass from these PV maps, we followed the procedure given by Seifried et al (2016).…”

Section: The Ggd 27-mm1 Disk-jet Systemmentioning

confidence: 99%

Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

Añez-López

Osorio

Busquet

et al. 2020

ApJ

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Recent high-angular resolution ( 40 mas) ALMA observations at 1.14 mm resolve a compact (R 200 au) flattened dust structure perpendicular to the HH 80-81 jet emanating from the GGD 27-MM1 high-mass protostar, making it a robust candidate for a true accretion disk. The jet/disk system (HH 80-81/GGD 27-MM1) resembles those found in association with low-and intermediate-mass protostars. We present radiative transfer models that fit the 1.14 mm ALMA dust image of this disk which allow us to obtain its physical parameters and predict its density and temperature structure.Our results indicate that this accretion disk is compact ( R disk 170 au) and massive ( 5 M ), about 20% of the stellar mass of 20 M . We estimate the total dynamical mass of the star-disk system from the molecular line emission finding a range between 21 and 30 M , which is consistent with our model. We fit the density and temperature structures found by our model with power law functions. These results suggest that accretion disks around massive stars are more massive and hotter than their low-mass siblings, but they still are quite stable. We also compare the temperature distribution in the GGD 27-MM1 disk with that found in low-and intermediate-mass stars and discuss possible implications on the water snow line. We have also carried out a study of the distance based on Gaia DR2 data and the population of young stellar objects (YSOs) in this region, and from the extinction maps. We conclude that the source distance is within 1.2 and 1.4 kpc, closer than what was derived in previous studies (1.7 kpc).

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Revealing the dynamics of Class 0 protostellar discs with ALMA

Cited by 55 publications

References 65 publications

Direct Detection of Precursors of Gas Giants Formed by Gravitational Instability With the Atacama Large Millimeter/Submillimeter Array

Direct Detection of Precursors of Gas Giants Formed by Gravitational Instability With the Atacama Large Millimeter/Submillimeter Array

Searching for kinematic evidence of Keplerian disks around Class 0 protostars with CALYPSO

Modeling the Accretion Disk around the High-mass Protostar GGD 27-MM1

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