2019
DOI: 10.1093/mnrasl/slz160 View full text |Buy / Rent full text
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Abstract: We study the gravitational instability and fragmentation of primordial protostellar discs by using high-resolution cosmological hydrodynamics simulations. We follow the formation and evolution of spiral arms in protostellar discs, examine the dynamical stability, and identify a physical mechanism of secondary protostar formation. We use linear perturbation theory based on the spiral-arm instability (SAI) analysis in our previous studies. We improve the analysis by incorporating the effects of finite thickness … Show more

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“…Whereas Takahashi et al (2016) specifically consider the fragmentation of a non-accreting massive protoplanetary disc, Inoue & Yoshida (2018) show that the similar concept is applicable for the galaxy-formation simulations in 3D. Inoue & Yoshida (2020) further apply the analyses to the cosmological simulation of the primordial star formation performed by Greif et al (2012). They show that the fragmentation of a rapidly accreting circumstellar disc demonstrated by Greif et al (2012) is essentially the same process.…”
Section: Role Of Spiral Arm Fragmentationmentioning
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“…Whereas Takahashi et al (2016) specifically consider the fragmentation of a non-accreting massive protoplanetary disc, Inoue & Yoshida (2018) show that the similar concept is applicable for the galaxy-formation simulations in 3D. Inoue & Yoshida (2020) further apply the analyses to the cosmological simulation of the primordial star formation performed by Greif et al (2012). They show that the fragmentation of a rapidly accreting circumstellar disc demonstrated by Greif et al (2012) is essentially the same process.…”
Section: Role Of Spiral Arm Fragmentationmentioning
“…Then, the locally estimated Q is below 0.6; the dense region grows to a separate protostar PS3. DF through interaction of spiral arms are studied by Inoue & Yoshida (2020). They perform detailed analysis of time evolution of spiral arms using an analytic model and direct simulations, to define the conditions for fragmentation.…”
Section: A13 Interaction Of Spiral Armsmentioning
“…An accretion disc forming around the core is in general gravitationally unstable. Several authors reported that low-mass secondary protostars with masses ∼ 0.1-1 M form both in primordial discs (Clark et al 2011;Greif et al 2012;Susa et al 2014;Hirano & Bromm 2017;Inoue & Yoshida 2020) and in low-metallicity discs with 10 −6 -10 −3 Z (Machida & Nakamura 2015; Chiaki et al 2016).…”
Section: Introductionmentioning
“…It has been believed that the first stars are largely massive (∼ 10-1000 M ) due to inefficient cooling in the primordial gas clouds (Omukai & Nishi 1998;Yoshida et al 2008). However, recent numerical studies have revealed that the fragmentation of accretion disks can lead less massive stars (∼ 1 M ) to form (Clark et al 2011b;Greif et al 2011Greif et al , 2012Susa 2013;Susa et al 2014;Stacy et al 2016;Hirano & Bromm 2017;Susa 2019;Inoue & Yoshida 2020;Chiaki & Yoshida 2020). In addition, turbulence can either promote (Clark et al 2011a;Riaz et al 2018;Wollenberg et al 2020), or suppresses fragmentation due to the amplification of magnetic fields (Sur et al 2010(Sur et al , 2012Federrath et al 2011;Turk et al 2012;Machida & Doi 2013;Sharda et al 2020).…”
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