Special Relativistic Simulations of Magnetically Dominated Jets in Collapsing Massive Stars

Takiwaki, Tomoya; Kotake, Kei; Sato, Katsuhiko

doi:10.1088/0004-637x/691/2/1360

Cited by 168 publications

(179 citation statements)

References 105 publications

(133 reference statements)

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“…Because the disc occupies only a small solid angle, much of the energy will escape into the other directions, especially if the energy release occurs in the form of jets, which might be the case for fast-rotating massive stars (e.g. Bisnovatyi-Kogan & Moiseenko 2008; Takiwaki et al 2009;Dessart et al 2012), and ablate only the surface of the disc. At this point (4.5 Myr for the 60 M star) we might expect that a large fraction of the inner disc gas has already accreted onto the newly formed stars.…”

Section: Effect Of Supernovae On the Associated Star-forming Discmentioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause

Charbonnel

Decressin

et al. 2013

A&A

134

155

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Context. The self-enrichment scenario for globular clusters (GC) requires large amounts of residual gas after the initial formation of the first stellar generation. Recently, we found that supernovae may not be able to expel that gas, as required to explain their presentday gas-free state, and suggested that a sudden accretion onto the dark remnants at a stage when type II supernovae have ceased may plausibly lead to fast gas expulsion. Aims. Here, we explore the consequences of these results for the self-enrichment scenario via fast-rotating massive stars (FRMS). Methods. We analysed the interaction of FRMS with the intra-cluster medium (ICM), in particular where, when, and how the second generation of stars may form. From the results, we developed a timeline of the first ≈40 Myr of GC evolution. Results. Our previous results imply three phases during which the ICM is in a fundamentally different state, namely the wind bubble phase (lasting 3.5 to 8.8 Myr), the supernova phase (lasting 26.2 to 31.5 Myr), and the dark remnant accretion phase (lasting 0.1 to 4 Myr): (i) Quickly after the first-generation massive stars have formed, stellar wind bubbles compress the ICM into thin filaments. No stars may form in the normal way during this phase because of the high Lyman-Werner flux density. If the first-generation massive stars have equatorial ejections however, as we proposed in the FRMS scenario, accretion may resume in the shadow of the equatorial ejecta. The second-generation stars may then form due to gravitational instability in these disc, which are fed by both the FRMS ejecta and pristine gas. (ii) In the supernova phase the ICM develops strong turbulence, with characteristic velocities below the escape velocity. The gas does not accrete either onto the stars or onto the dark remnants in this phase because of the high gas velocities. The strong mass loss associated with the transformation of the FRMS into dark remnants then leads to the removal of the secondgeneration stars from the immediate vicinity of the dark remnants. (iii) When the supernovae have ceased, turbulence quickly decays, and the gas can once more accrete, now onto the dark remnants. As discussed previously, this may release sufficient energy to unbind the gas, and may happen fast enough so that a large fraction of less tightly bound first-generation stars are lost. Conclusions. Studying the FRMS scenario for the self-enrichment of GCs in detail reveals the important role of the physics of the ICM for our understanding of the formation and early evolution of GCs. Depending on the level of mass segregation, this sets constraints on the orbital properties of the stars, in particular high orbital eccentricities, which likely has implications on the GC formation scenario.

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Section: Effect Of Supernovae On the Associated Star-forming Discmentioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause

Charbonnel

Decressin

et al. 2013

A&A

134

155

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“…Core-collapse supernovae (CC-SNe) driven by rotation and magnetic fields, so-called magneto-rotational supernovae (MR-SNe), are a promising mechanism for several high-energy astronomical phenomena, e.g., magnetar formation, gravitational waves and hypernovae, and gamma-ray bursts (e.g., Yamada & Sawai 2004;Shibata et al 2006;Takiwaki et al 2009;Mösta et al 2014). Jet-like explosions in CCSNe are expected to eject very neutron-rich matter, appropriate for the r-process (e.g., Cameron 2003;Papish & Soker 2012).…”

Section: Introductionmentioning

confidence: 99%

The Intermediate r-process in Core-collapse Supernovae Driven by the Magneto-rotational Instability

Nishimura

Sawai

Takiwaki

et al. 2017

ApJL

177

197

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We investigated r-process nucleosynthesis in magneto-rotational supernovae, based on a new explosion mechanism induced by the magneto-rotational instability (MRI). A series of axisymmetric magnetohydrodynamical simulations with detailed microphysics including neutrino heating is performed, numerically resolving the MRI. Neutrino-heating dominated explosions, enhanced by magnetic fields, showed mildly neutronrich ejecta producing nuclei up toÃ 130 (i.e., the weak r-process), while explosion models with stronger magnetic fields reproduce a solar-like r-process pattern. More commonly seen abundance patterns in our models are in between the weak and regular r-process, producing lighter and intermediate-mass nuclei. These intermediate r-processes exhibit a variety of abundance distributions, compatible with several abundance patterns in r-processenhanced metal-poor stars. The amount of Eu ejectain magnetically driven jets agrees with predicted values in the chemical evolution of early galaxies. In contrast, neutrino-heating dominated explosions have a significant amount of Fe ( Ni 56 ) and Zn, comparable to regular supernovae and hypernovae, respectively. These results indicate magneto-rotational supernovae can produce a wide range of heavy nuclei from iron-group to r-process elements, depending on the explosion dynamics.

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“…It accelerates to ultrarelativistic speeds (reaching Lorentz factors of ∼ 50 Aloy et al 2000) while, at the same time, interacts with the progenitor system. Alternatively, MHD process may tap a fraction of the rotational energy of the BH or of the accretion disk to form an outflow (Proga et al 2003;Mizuno et al 2004;McKinney 2006;Nagataki et al 2007;Komissarov & Barkov 2007;Takiwaki et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Angular Energy Distribution of Collapsar-Jets

Mizuta

Aloy

2009

ApJ

120

119

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Collapsars are fast-spinning, massive stars, whose core collapse liberates an energy, that can be channeled in the form of ultrarelativistic jets. These jets transport the energy from the collapsed core to large distances, where it is dissipated in the form of long-duration gamma-ray bursts. In this paper we study the dynamics of ultrarelativistic jets produced in collapsars. Also we extrapolate our results to infer the angular energy distribution of the produced outflows in the afterglow phase. Our main focus is to look for global energetical properties which can be imprinted by the different structure of different progenitor stars. Thus, we employ a number of pre-supernova, stellar models (with distinct masses and metallicities), and inject in all of them jets with fixed initial conditions. We assume that at the injection nozzle, the jet is mildly relativistic (Lorentz factor ∼ 5), has a finite half-opening angle (5 • ), and carries a power of 10 51 erg s −1 . In all cases, well collimated jets propagate through the progenitor, blowing a high pressure and high temperature cocoon. These jets arrive intact to the stellar surface and break out of it. A large Lorentz factor region Γ > ∼ 100 develops well before the jet reaches the surface of the star, in the unshocked part of the beam, located between the injection nozzle and the first recollimation shock. These high values of Γ are possible because the finite opening angle of the jet allows for free expansion towards the radial direction. We find a strong correlation between the angular energy distribution of the jet, after its eruption from the progenitor surface, and the mass of the progenitors. The angular energy distribution of the jets from light progenitor models is steeper than that of the jets injected in more massive progenitor stars. This trend is also imprinted in the angular distribution of isotropic equivalent energy.

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Special Relativistic Simulations of Magnetically Dominated Jets in Collapsing Massive Stars

Cited by 168 publications

References 105 publications

Superbubble dynamics in globular cluster infancy

Superbubble dynamics in globular cluster infancy

The Intermediate r-process in Core-collapse Supernovae Driven by the Magneto-rotational Instability

Angular Energy Distribution of Collapsar-Jets

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