Standing Solitary Waves as Transitions to Spiral Structures in Gravitationally Unstable Accretion Disks

Deng, Hongping; Ogilvie, Gordon I.

doi:10.3847/2041-8213/ac81c0

Cited by 3 publications

(3 citation statements)

References 17 publications

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“…(Boley et al 2010) estimated fg ≈ 1.8Q. This is compatible with the considerations in Deng & Ogilvie (2022) where they suggested a solitary ring structure as a transitory state in which spiral density waves would emerge, and then collapse would eventually ensue in the flow entrained by them. Measuring Q in our simulations by tracing back the clump's particles in time leads to values of Q ≈ 1.15 in the early phases of the simulation.…”

Section: Predicted Mass Scalessupporting

confidence: 70%

“…Deng et al (2017)). With this in mind, Deng & Ogilvie (2022) instead of a smooth disk, considered an already nonlinear ring-like structure as the background state, described by solitary waves. Then, they studied the growth of nonaxisymmetric perturbations to the solitary modes, identifying fast growth, which would result in the development of a spiral structure.…”

Section: Summary and Concluding Discussionmentioning

confidence: 99%

“…Traditional disk instability, neglecting magnetic fields, is thought to be only relevant for gas giants and thus cannot provide an explanation for intermediate-mass planets. However, young gravitationally unstable disks exhibit spiral structures (Toomre 1964;Deng & Ogilvie 2022), such as observed in Elias 2-27 (Meru et al 2017;Veronesi et al 2021;Pérez et al 2016), suggesting some role of disk instability.…”

Section: Introductionmentioning

confidence: 99%

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Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary disks

Kubli¹,

Mayer²,

Hu³

2023

Preprint

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We study the initial development, structure and evolution of protoplanetary clumps formed in 3D resistive MHD simulations of self-gravitating disks. The magnetic field grows by means of the recently identified gravitational instability dynamo (Riols & Latter 2018;Deng et al. 2020). Clumps are identified and their evolution is tracked finely both backward and forward in time. Their properties and evolutionary path is compared to clumps in companion simulations without magnetic fields. We find that magnetic and rotational energy are important in the clumps' outer regions, while in the cores, despite appreciable magnetic field amplification, thermal pressure is most important in counteracting gravity. Turbulent kinetic energy is of a smaller scale than magnetic energy in the clumps. Compared to non-magnetized clumps, rotation is less prominent, which results in lower angular momentum in much better agreement with observations. In order to understand the very low sub-Jovian masses of clumps forming in MHD simulations, we revisit the perturbation theory of magnetized sheets finding support for a previously proposed magnetic destabilization in low-shear regions. This can help explaining why fragmentation ensues on a scale more than an order of magnitude smaller than that of the Toomre mass. The smaller fragmentation scale and the high magnetic pressure in clumps' envelopes explain why clumps in magnetized disks are typically in the super-Earth to Neptune mass regime rather than Super-Jupiters as in conventional disk instability. Our findings put forward a viable alternative to core accretion to explain widespread formation of intermediate-mass planets.

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Section: Predicted Mass Scalessupporting

confidence: 70%

Section: Summary and Concluding Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary disks

Kubli¹,

Mayer²,

Hu³

2023

Preprint

View full text Add to dashboard Cite

show abstract

Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary discs

Kubli,

Mayer,

Deng

2023

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We study the initial development, structure and evolution of protoplanetary clumps formed in 3D resistive MHD simulations of self-gravitating disks. The magnetic field grows by means of the recently identified gravitational instability dynamo. Clumps are identified and their evolution is tracked finely both backward and forward in time. Their properties and evolutionary path is compared to clumps in companion simulations without magnetic fields. We find that magnetic and rotational energy are important in the clumps’ outer regions, while in the cores, despite appreciable magnetic field amplification, thermal pressure is most important in counteracting gravity. Turbulent kinetic energy is of a smaller scale than magnetic energy in the clumps. Compared to non-magnetized clumps, rotation is less prominent, which results in lower angular momentum in much better agreement with observations. In order to understand the very low sub-Jovian masses of clumps forming in MHD simulations, we revisit the perturbation theory of magnetized sheets finding support for a previously proposed magnetic destabilization in low-shear regions. This can help explaining why fragmentation ensues on a scale more than an order of magnitude smaller than that of the Toomre mass. The smaller fragmentation scale and the high magnetic pressure in clumps’ envelopes explain why clumps in magnetized disks are typically in the super-Earth to Neptune mass regime rather than Super-Jupiters as in conventional disk instability. Our findings put forward a viable alternative to core accretion to explain widespread formation of intermediate-mass planets.

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SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B

Lewis,

Li,

Gibbs

et al. 2024

ApJ

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Brown dwarfs with measured dynamical masses and spectra from direct imaging are benchmarks that anchor substellar atmosphere cooling and evolution models. We present Subaru SCExAO/CHARIS infrared spectroscopy of HIP 93398 B, a brown dwarf companion recently discovered by Y. Li et al. (2023), as part of an informed survey using the Hipparcos–Gaia Catalog of Accelerations. This object was previously classified as a T6 dwarf based on its luminosity, with its independently derived age and dynamical mass in tension with existing models of brown dwarf evolution. Spectral typing via empirical standard spectra, temperatures derived by fitting substellar atmosphere models, and J − H, J − K and H − L ′ colors all suggest that this object has a substantially higher temperature and luminosity, consistent with classification as a late-L dwarf near the L/T transition (T = 1200 − 119 + 140 K) with moderate to thick clouds possibly present in its atmosphere. When compared with the latest generation of evolution models that account for clouds with our revised luminosity and temperature for the object, the tension between the model-independent mass/age and model predictions is resolved.

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Standing Solitary Waves as Transitions to Spiral Structures in Gravitationally Unstable Accretion Disks

Cited by 3 publications

References 17 publications

Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary disks

Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary disks

Characterizing fragmentation and sub-Jovian clump properties in magnetized young protoplanetary discs

SCExAO/CHARIS Spectroscopic Characterization of Cloudy L/T Transition Companion Brown Dwarf HIP 93398 B

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