Evolution of binary seeds in collapsing protostellar gas clouds

Satsuka, Tatsuya; Tsuribe, Toru; Tanaka, Shunya; Nagamine, Kentaro

doi:10.1093/mnras/stw2709

Cited by 16 publications

(17 citation statements)

References 41 publications

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“…In the core accretion model (Safronov 1972;Goldreich & Ward 1973;Mizuno 1980;Bodenheimer & Pollack 1986;Pollack et al 1996) the cores of giant planets form in circumstellar discs by coagulation of dust particles to progressively larger objects, until a core with a few Earth masses has formed. Such a ⋆ E-mail: dstamatellos@uclan.ac.uk core subsequently accretes an envelop of gas from the disc.…”

Section: Introductionmentioning

confidence: 99%

The diverse lives of massive protoplanets in self-gravitating discs

Stamatellos

Inutsuka

2018

Monthly Notices of the Royal Astronomical Society

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Gas giant planets may form early-on during the evolution of protostellar discs, while these are relatively massive. We study how Jupiter-mass planet-seeds (termed protoplanets) evolve in massive, but gravitationally stable (Q > ∼ 1.5), discs using radiative hydrodynamic simulations. We find that the protoplanet initially migrates inwards rapidly, until it opens up a gap in the disc. Thereafter, it either continues to migrate inwards on a much longer timescale or starts migrating outwards. Outward migration occurs when the protoplanet resides within a gap with gravitationally unstable edges, as a high fraction of the accreted gas is high angular momentum gas from outside the protoplanet's orbit. The effect of radiative heating from the protoplanet is critical in determining the direction of the migration and the eccentricity of the protoplanet. Gap opening is facilitated by efficient cooling that may not be captured by the commonly used β-cooling approximation. The protoplanet initially accretes at a high rate (∼ 10 −3 M J yr −1 ), and its accretion luminosity could be a few tenths of the host star's luminosity, making the protoplanet easily observable (albeit only for a short time). Due to the high gas accretion rate, the protoplanet generally grows above the deuterium-burning mass-limit. Protoplanet radiative feedback reduces its mass growth so that its final mass is near the brown dwarf-planet boundary. The fate of a young planet-seed is diverse and could vary from a gas giant planet on a circular orbit at a few AU from the central star to a brown dwarf on an eccentric, wide orbit.

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Section: Introductionmentioning

confidence: 99%

The diverse lives of massive protoplanets in self-gravitating discs

Stamatellos

Inutsuka

2018

Monthly Notices of the Royal Astronomical Society

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“…Numerical simulation studies for circumstellar disks indeed reproduce such substructures (e.g. Bate & Bonnell 1997;Fateeva et al 2011;Satsuka et al 2017;Price et al 2018;Matsumoto et al 2019). Both the observational and theoretical researches suggest a spatial gap of the gas distribution between the circumbinary disk and the circumstellar disks.…”

Section: Substructures Of the 13 MM Continuum Emissionmentioning

confidence: 80%

“…On the other hand, theoretical simulations show a gap of the gas distribution between a circumbinary disk and circumstellar disks (e.g. Bate & Bonnell 1997;Fateeva et al 2011;Satsuka et al 2017;Price et al 2018;Matsumoto et al 2019). At the first glance, such a gap/hole structure would not be the case of the C 17 O emission in IRAS 16293-2422 Source A; in the C 17 O deficient area, the dust is not expected to be so optically thick as to significantly suppress the molecular emission enough, because the H 2 CS emission is observed there (Figure 3).…”

Section: Circummultiple Structurementioning

confidence: 99%

“…Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases both in observations (Tokuda et al 2014;Dutrey et al 2014;Takakuwa et al 2014Takakuwa et al , 2017Tobin et al 2016a,b;Boehler et al 2017;Artur de la Villarmois et al 2018;Alves et al 2019) and numerical simulations (e.g. Bate & Bonnell 1997;Kratter et al 2008;Fateeva et al 2011;Shi et al 2012;Ragusa et al 2017;Satsuka et al 2017;Price et al 2018;Matsumoto et al 2019). For instance, circumbinary/circummultiple disk structures with a spiral structure as well as a circumstellar disk for each component are reported (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Substructures in the Disk-Forming Region of the Class 0 Low-Mass Protostellar Source IRAS 16293-2422 Source A on a 10 au Scale

Oya,

Yamamoto

2020

Preprint

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We have observed the Class 0 protostellar source IRAS 16293−2422 A in the C 17 O and H 2 CS lines as well as the 1.3 mm dust continuum with the Atacama Large Millimeter/submillimeter Array at an angular resolution of ∼0. 1 (14 au).The continuum emission of the binary component, Source A, reveals the substructure consisting of 5 intensity peaks within 100 au from the protostar. The C 17 O emission mainly traces the circummultiple structure on a 300 au scale centered at the intensity centroid of the continuum, while it is very weak within the radius of 50 au from the centroid. The H 2 CS emission, in contrast, traces the rotating disk structure around one of the continuum peaks (A1). Thus, it seems that the rotation centroid of the circummultiple structure is slightly different from that of the disk around A1. We derive the rotation temperature by using the multiple lines of H 2 CS. As approaching to the protostar A1, the rotation temperature steeply rises up to 300 K or higher at the radius of 50 au from the protostar. It is likely due to a local accretion shock and/or the preferential protostellar heating of the transition zone from the circummultiple structure to the disk around A1. This position corresponds to the place where the organic molecular lines are reported to be enhanced. Since the rise of the rotation temperature of H 2 CS most likely represents the rise of the gas and dust temperatures, it would be related to the chemical characteristics of this prototypical hot corino.

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“…In the star formation process, angular momentum is naturally introduced into the system by mass accretion during the main accretion phase, because the infalling gas possesses angular momentum. It can be expected that the separation of the protobinary system will gradually widen over time, because parcels of gas with large angular momentum will later accrete onto the system, as shown in Satsuka et al (2017). However, many observations of (high-mass) close binary systems in various star-forming regions (Duchêne & Kraus 2013) indicate that there is likely to be a mechanism to efficiently remove angular momentum from the system in the binary formation process.…”

Section: Introductionmentioning

confidence: 99%

Impact of Magnetic Braking on High-mass Close Binary Formation

Harada,

Hirano,

Machida

et al. 2021

Preprint

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Combining numerical simulations and analytical modeling, we investigate whether close binary systems form by the effect of magnetic braking. Using magnetohydrodynamics simulations, we calculate the cloud evolution with a sink, for which we do not resolve the binary system or binary orbital motion to realize long-term time integration. Then, we analytically estimate the binary separation using the accreted mass and angular momentum obtained from the simulation. In unmagnetized clouds, wide binary systems with separations of > 100 au form, in which the binary separation continues to increase during the main accretion phase. In contrast, close binary systems with separations of < 100 au can form in magnetized clouds. Since the efficiency of magnetic braking strongly depends on both the strength and configuration of the magnetic field, they also affect the formation conditions of a close binary.In addition, the protostellar outflow has a negative impact on close binary formation, especially when the rotation axis of the prestellar cloud is aligned with the global magnetic field. The outflow interrupts the accretion of gas with small angular momentum, which is expelled from the cloud, while gas with large angular momentum preferentially falls from the side of the outflow onto the binary system and widens the binary separation. This study shows that a cloud with a magnetic field that is not parallel to the rotation axis is a favorable environment for the formation of close binary systems.

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Evolution of binary seeds in collapsing protostellar gas clouds

Cited by 16 publications

References 41 publications

The diverse lives of massive protoplanets in self-gravitating discs

The diverse lives of massive protoplanets in self-gravitating discs

Substructures in the Disk-Forming Region of the Class 0 Low-Mass Protostellar Source IRAS 16293-2422 Source A on a 10 au Scale

Impact of Magnetic Braking on High-mass Close Binary Formation

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