Critical phenomena in the aspherical gravitational collapse of radiation fluids

Baumgarte, Thomas W.; Montero, Pedro J.

doi:10.1103/physrevd.92.124065

Cited by 21 publications

(56 citation statements)

References 42 publications

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“…10. We should be able to predict how much better the constraints can be satisfied as we increase the resolution; specifically, as we double the number of points on a side, we should see the ratio of errors be O(∆x 6 )/O(∆x 6 /2 6 ) ∼ 2 6 . We have implemented a number of finite-differencing stencils, seeing reduced error for higher-order stencils as expected.…”

Section: Varying the Resolutionmentioning

confidence: 99%

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Integration of inhomogeneous cosmological spacetimes in the BSSN formalism

2016

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We present cosmological-scale numerical simulations of an evolving universe in full general relativity (GR) and introduce a new numerical tool, CosmoGRaPH, which employs the BaumgarteShapiro-Shibata-Nakamura (BSSN) formalism on a 3-dimensional grid. Using CosmoGRaPH, we calculate the effect of an inhomogeneous matter distribution on the evolution of a spacetime. We also present the results of a set of standard stability tests to demonstrate the robustness of our simulations.

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Section: Varying the Resolutionmentioning

confidence: 99%

“…This formalism is most often applied in regimes of strong gravity -compact object dynamics. However, it has also been applied to cosmological problems in the early universe, such as critical collapse in a radiation fluid [5,6], black hole lattices (eg. [7]), and more (for a recent review, see [8]).…”

Section: Introductionmentioning

confidence: 99%

Integration of inhomogeneous cosmological spacetimes in the BSSN formalism

2016

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“…In particular, despite the tremendous recent progress in numerical relativity, only few numerical simulations of aspherical critical collapse have been performed (e.g. [5,[9][10][11][12][13][14]). This is even more surprising as several interesting questions cannot be addressed in spherical symmetry.…”

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confidence: 99%

“…The code makes no symmetry assumptions, but we run it here assuming both axisymmetry and a symmetry across the equatorial plane. In [14] we used this code to study critical phenomena in the aspherical collapse of a radiation fluid; those calculations also serve as a calibration of our code for the calculations presented here. We use a logarithmic grid in the radial direction (see App.…”

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confidence: 99%

Critical Collapse of Rotating Radiation Fluids

Baumgarte

Gundlach

2016

Phys. Rev. Lett.

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We present results from the first fully relativistic simulations of the critical collapse of rotating radiation fluids. We observe critical scaling both in subcritical evolutions, in which case the fluid disperses to infinity and leaves behind flat space, and in supercritical evolutions that lead to the formation of black holes. We measure the mass and angular momentum of these black holes, and find that both show critical scaling with critical exponents that are consistent with perturbative results. The critical exponents are universal; they are not affected by angular momentum, and are independent of the direction in which the critical curve, which separates subcritical from supercritical evolutions in our two-dimensional parameter space, is crossed. In particular, these findings suggest that the angular momentum decreases more rapidly than the square of the mass, so that, as criticality is approached, the collapse leads to the formation of a non-spinning black hole. We also demonstrate excellent agreement of our numerical data with new closed-form extensions of power-law scalings that describe the mass and angular momentum of rotating black holes formed close to criticality.

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“…In [30] the authors studied tri-axial collapse of black holes and critical collapse in a way which is relevant also for primordial black-hole formation, and in [31] a non-spherical critical collapse was considered. The authors of [32][33][34] discussed effects of non-spherical geometry in the formation of primordial black holes if it occurred during an intermediate phase of matter domination due to a superheavy unified field theory particle in the very early universe.…”

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Ellipsoidal collapse and primordial black hole formation

Kühnel

Sandstad

2016

Phys. Rev. D

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We reinvestigate gravitational ellipsoidal collapse with special focus on its impact on primordial black-hole formation. For a generic model we demonstrate that the abundance and energy density of the produced primordial black holes will be significantly decreased when the non-sphericity of the overdensities is taken into account.The process of gravitational collapse is of utmost importance to our understanding of the Universe. From the formation of galaxies [1,2], clusters of galaxies [3,4], haloes [5][6][7][8][9] (for a recent review see [10]) or even to the possible formation of primordial black holes [11][12][13], the nature of the collapse is crucial in determining characteristics like abundance, mass or shape.In many cases, both for its calculational simplicity as well as being a reasonable first approximation, spherical symmetry has been an integral assumption to investigate gravitational collapse processes [14][15][16]. Although in most cases initial non-sphericity is either small or eventually leads to (approximately) spherical objects, its effect might nevertheless be consequential. For instance, estimates of the abundance of small galactic haloes receive considerable corrections [17], the formation of space-time singularities might be very different [18], or, the precise geometric way in which collapse proceeds may lead to major intermediate deformations [19,20].The space of all possible shapes a collapsing overdensitiy might have is enormously large. Hence, one needs to focus on the most relevant structures. One of the simplest and most studied, deviating from spherical symmetry, is an ellipsoidal one, also because it gives a fairly good approximation to objects of many shapes. This has been and still is the focus of a vast amount of literature (cf. [17, 21-27]), including the seminal work of Sheth, Mo and Tormen [17] who obtained a fitting formula for the mentioned collapse threshold which they found to be supported by numerical evidence. More recent evidence for the improvement of fits with an ellipsoidal collapse model can be found for instance in [28,29].While most of the quoted references on ellipsoidal collapse deal with the formation of dark-matter haloes, the investigation of how the shape distribution of initial overdensities may affect the formation of primordial black holes is relatively modest. In [30] the authors studied tri-axial collapse of black holes and critical collapse in a way which is relevant also for primordial black-hole formation, and in [31] a non-spherical critical collapse was considered. The authors of [32][33][34] discussed effects of non-spherical geometry in the formation of primordial black holes if it occurred during an intermediate phase of matter domination due to a superheavy unified field theory particle in the very early universe. However, to the best of our knowledge, there has not been a thorough investigation of the effect of the abundance, or, the energy density of primordial back holes when lifting the spherical assumption on the overdensities in a genera...

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Critical phenomena in the aspherical gravitational collapse of radiation fluids

Cited by 21 publications

References 42 publications

Integration of inhomogeneous cosmological spacetimes in the BSSN formalism

Integration of inhomogeneous cosmological spacetimes in the BSSN formalism

Critical Collapse of Rotating Radiation Fluids

Ellipsoidal collapse and primordial black hole formation

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