Choked accretion: from radial infall to bipolar outflows by breaking spherical symmetry

Alejandro Aguayo-Ortiz; Emilio Tejeda; X. Hernandez

REVIEW 2 major objections 5 minor 1 cited by

Choked accretion: from radial infall to bipolar outflows by breaking spherical symmetry

T0 review · 2 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read A small equatorial-polar density imbalance makes steady hydrodynamic accretion onto a point mass saturate at the Bondi rate and eject all surplus matter in bipolar outflows.

desk verdict A clean numerical demonstration of a new accretion-flow morphology, with the strong universal choking claim outrunning the parameter space actually explored. read the letter →

arxiv 1909.00884 v2 pith:3QWNIHQQ submitted 2019-09-02 astro-ph.HE

Alejandro Aguayo-Ortiz , Emilio Tejeda , X. Hernandez This is my paper · ORCID

classification astro-ph.HE

keywords accretionBondibipolaroutflowsaxisymmetrichydrodynamicssphericalsymmetrybreakingastrophysicaljetsnumericalsimulations

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Spherically symmetric accretion has a canonical steady solution, Bondi accretion, but real infall is never perfectly spherical. This paper asks what happens when the equatorial plane is slightly denser than the poles, and finds that the flow reorganizes into a steady pattern of equatorial infall plus bipolar outflows, while the mass flux actually reaching the central object saturates at essentially the Bondi value. The excess injected material is expelled even for density contrasts as small as $0.1\%$, and for a $10\%$ contrast the ejected gas leaves faster than the local escape speed. The result matters because it shows that bipolar ejection can arise from pure hydrodynamics, without rotation or magnetic fields, and it suggests a universal ceiling on steady spherical accretion.

What carries the argument

The central object is a named mechanism, choked accretion, produced by an equatorial-to-polar density contrast at the outer injection sphere. The analytic backbone is the incompressible, irrotational velocity potential $\Phi = \alpha/r\left[1 + r^3/(4S^3)(3\cos^2\theta - 1)\right]$, a Laplace-equation solution with a monopole term for Bondi inflow and a quadrupole term; its stagnation points at $(S,0)$ and $(S,\pi)$ mark the transition from equatorial infall to polar outflow. In the numerical simulations, the same morphology emerges: a pressure gradient from the density inhomogeneity redirects streamlines, and because the flow becomes quasi-spherical at small radii, the inner accretion rate locks onto the Bondi value. The quantity $S$, the stagnation-point radius, controls the geometry and shrinks as $\delta$ or $\gamma$ grow.

What would settle it

Run the same hydrodynamic problem with the inner boundary changed from free outflow to a hard absorbing surface, or with the outer injection sphere moved inward from $10\,r_\mathrm{B}$ to a few $r_\mathrm{B}$, and measure the steady-state accretion rate; a value that departs from $\dot{M}_B$ by more than a few per cent, or a flow that never reaches a stationary state, would falsify the choking claim.

Watch

Extended reading notes

Core claim

The paper claims that a steady, non-rotating, purely hydrodynamic accretion flow onto a Newtonian point mass does not simply pass through the spherical Bondi solution when the inflow is axisymmetrically over-dense at the equator. The density contrast generates a pressure gradient that deflects part of the infall, producing a bipolar outflow, while the inner flow re-converges toward the Bondi solution and the total accretion rate across the inner boundary 'chokes' at a value within a few per cent of the Bondi rate. In the simulations this holds for adiabatic indices $\gamma = 1$, $4/3$, $7/5$ and for equatorial-to-polar contrasts of $0.1$, $1$ and $10$ per cent; the ejected fraction grows with the contrast, reaching $94\%$ at $\delta = 10\%$ with outflow speeds above the local escape velocity. The authors therefore propose the choked accretion mechanism as a hydrodynamical bridge between purely radial accretion and jet-generating disc models.

Load-bearing premise

The claim that the accretion rate saturates at the Bondi value rests on the particular numerical setup — a free-outflow inner boundary at $0.1\,r_\mathrm{B}$ and a cosine-squared density excess injected at $10\,r_\mathrm{B}$ — and the paper itself reports that larger contrasts or smaller outer radii become unstable, so the choke could be a property of that setup rather than a general law.

Editorial extensions

If this is right

A density contrast as small as $0.1\%$ between equator and poles is enough to switch the flow from purely radial Bondi infall to a steady inflow/outflow morphology.
The accretion rate onto the central object saturates at approximately $\dot{M}_B$ regardless of the injection rate at the outer boundary; extra mass is ejected rather than accreted.
For a $10\%$ contrast the ejected matter exceeds the local escape speed and carries up to $94\%$ of the injected mass, so the mechanism can in principle launch unbound outflows.
The same qualitative result is obtained for isothermal ($\gamma=1$), radiation-dominated ($\gamma=4/3$) and diatomic-gas ($\gamma=7/5$) equations of state, suggesting the mechanism is not tied to a specific thermodynamics.
Order-of-magnitude estimates place the mechanism's characteristic scale $S$ within reach of young-stellar-object molecular outflows and long-GRB collapsar conditions, though not of X-ray binaries or AGN as-is.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If the choke is a general property of subsonic outer-injection flows, the Bondi rate acts as a strict upper bound on steady non-rotating, non-magnetic accretion; any observed super-Bondi accretion would then be a signature of rotation, magnetic stresses, or time dependence.
A natural numerical test would replace the free-outflow inner boundary with a hard absorbing surface (e.g. a star) or place the outer boundary closer than $10\,r_\mathrm{B}$; the paper notes the latter regime becomes unsteady, so the plateau may be restricted to gently perturbed, large-box configurations.
The equatorial-overdense boundary condition is the axisymmetric cousin of the transverse density gradient in Bondi-Hoyle-Lyttleton accretion; choked accretion might be the zero-relative-velocity limit of a larger family of gradient-driven outflows.
Observational extension: if molecular outflows in young stellar objects are choked-accretion driven, their mass-loss rates should track infall rates above a threshold set by the Bondi rate, a correlation that could be searched for in protostellar cores.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Colleague,

Read Aguayo-Ortiz et al. The paper is worth your time: it shows numerically that a steady, non-rotating, axisymmetric accretion flow with a mild equatorial over-density develops a bipolar outflow while the net accretion onto the central object stays at roughly the Bondi rate. The choking effect—inner Mdot saturating near Mdot_B while excess supply is ejected—is new relative to the earlier isothermal perturbation work. The simulations are careful: Bondi validation at sub-percent level, second-order convergence, three adiabatic indices, and a consistent morphology across the board.

What I find genuinely useful: the idea that spherical symmetry breaking alone can produce an in/outflow geometry, without rotation or magnetic fields, and that the inner flow converges to a quasi-Bondi configuration. The authors are also honest about where the model strains, and they don't oversell the astrophysical applicability—they explicitly note that S is large and that radiation/MHD effects would shrink it.

The soft spots are real but not fatal. The strongest claim—that there is a maximum achievable accretion rate equal to the Bondi value regardless of supply—is not as controlled as it sounds. The outer boundary fixes density and pressure but lets velocity float, so the injection rate Mdot_in is part of the solution, not an externally imposed control parameter. Varying delta changes both the supply and the driving pressure gradient simultaneously. The authors themselves report that larger density contrasts or outer boundaries smaller than rB go unstable and never reach steady state, and they concede that very different boundary conditions may produce very different solutions. So the "universal" part is an extrapolation from a single family of self-selected steady branches. The free-outflow inner boundary also means the sink itself imposes no limiting rate; the plateau is a property of the flow, which is interesting, but the parameter space tested is narrow (delta up to 10%, Mdot_in up to about 17 Mdot_B). Table 1 has no error bars, though the convergence test mitigates that.

The analytic model in Section 2 is explicitly a toy: alpha is set to the Bondi rate by hand, so it doesn't independently support the choking claim. That's fine as motivation, and the simulations are the real evidence.

Net: this is a solid, well-executed numerical study of a plausible new mechanism. It deserves a serious referee and a thoughtful revision that either narrows the claims or expands the boundary-condition study. I'd bring it to group.

Referee Report

2 major / 5 minor

Summary. This paper investigates the effect of a small axisymmetric density contrast between the equatorial plane and the poles on steady-state hydrodynamic accretion onto a Newtonian point mass. The authors first present an analytic potential-flow toy model for an incompressible fluid (Section 2) that produces an inflow/outflow geometry with polar stagnation points, and then perform axisymmetric hydrodynamic simulations for adiabatic indices γ = 1, 4/3, and 7/5 using the aztekas code (Section 3). The outer boundary imposes a density profile ρ(θ)=ρ0(1−δ cos²θ) and the corresponding pressure, while velocities evolve freely; the inner boundary is a free-outflow sphere at 0.1 rB. The simulations are validated against the Bondi solution to within 1% and show second-order convergence. For δ = 0.1%, 1%, and 10%, the authors find steady-state flows in which the polar regions become underdense and drive a bipolar outflow, while the mass accretion rate through the inner boundary saturates at approximately the Bondi rate, with the ratio Mdot/Mdot_B within 5% of unity. The injection rate Mdot_in/Mdot_B increases with δ up to ~17, and the ratio of ejected to injected mass approaches ~94% at δ = 10%. The paper interprets this as evidence for a 'choked accretion' mechanism that limits the accretion rate to the Bondi value and ejects all excess mass.

Significance. If the choking phenomenon were shown to be independent of the specific boundary setup, it would constitute a new, purely hydrodynamical mechanism for producing bipolar outflows from quasi-spherical accretion, complementing magneto-rotational jet models. The paper has notable strengths: the numerical code is benchmarked against the analytic Bondi solution to better than 1% for three equations of state, and a self-convergence test demonstrates second-order convergence. The analytic toy model transparently illustrates the inflow/outflow geometry, and the numerical results show a consistent trend across γ and δ. However, the central claim of a maximum accretion rate is only established within a narrow parameter window (δ ≤ 10%, R = 10 rB, steady flow); the paper itself notes that larger contrasts or smaller outer radii produce non-steady solutions. The generality of the 'choked accretion' mechanism therefore remains a hypothesis, not a demonstrated theorem.

major comments (2)

[Section 4 (and abstract)] The claim that the inner accretion rate chokes at the Bondi value 'regardless of how large the injected mass rate is' is not supported by the present simulations, which cover only the steady-state regime with density contrasts δ ≤ 10% and an outer boundary at R = 10 rB (Section 3.1). The paper explicitly reports that larger δ or outer boundaries smaller than rB lead to 'rather unstable, highly dynamic accretion flows that do not seem to relax to steady state configurations.' Since the choking behavior is demonstrated only for the steady subset, the universal statement in the abstract ('any extra material being ejected') is not established. The authors should either extend the analysis into the non-steady regime (e.g., by time-averaging the accretion rate and outflow) or explicitly restrict the conclusion to the parameter range explored.
[Section 3.1, Figure 8] The injection rate Mdot_in is not an independent control parameter in these experiments. At the outer boundary the authors impose only the density profile (3.2) and the corresponding pressure, while allowing free evolution of both velocity components; consequently Mdot_in and Mdot_ej are emergent properties of the steady solution, not externally imposed mass supplies. Figure 8 thus demonstrates a correlation between Mdot_in/Mdot_B and Mdot_ej/Mdot_in as δ is varied, but it does not test the physical prediction that a prescribed super-Bondi mass supply would be diverted into the outflow while the inner rate stays fixed at Mdot_B. A test that controls the supply rate independently (e.g., by imposing a radial velocity profile at R) is needed to validate the 'maximum achievable accretion rate' interpretation.

minor comments (5)

[Table 1] The reported rates are given to two decimal places without error bars; since the key claim is that Mdot/Mdot_B is close to unity (within a few percent), the numerical uncertainty from the convergence study should be quantified so that the reader can assess the significance of the deviations.
[Section 2, Eq. (2.7)] The analytic model sets the accretion rate to the Bondi value by hand in Eq. (2.7); the paper should state more explicitly that this is an assumed input for the toy model rather than a derived consequence, to avoid any appearance of circularity in the analytic motivation.
[Section 3.1] The phrase 'free (as free-outflow condition) evolution' for the velocity components at the outer boundary is ambiguous; a zero-gradient copied ghost-cell condition permits both inflow and outflow, so the authors should specify the exact implementation and verify that it does not artificially constrain the diagnosed injection rate.
[Section 3.3] Equation (2.5) is introduced in the context of the incompressible analytic model; the numerical computation of Mdot should instead be stated directly as the surface integral of ρ v_r over a sphere, to avoid confusion about which equations are used in the simulations.
[Throughout] There are several typographical artifacts, including a stray backslash character in 'i.e.⃗ v= ∇Φ' in Section 2 and the appearance of '/Slash1s' in the axis label of Figure 1; these should be corrected in the final version.

Circularity Check

1 steps flagged · score 2.0 of 10

The illustrative analytic model presets the Bondi rate; the numerical choke is emergent.

self definitional [Section 2, Eqs. (2.5)-(2.7)]
"At this point ˙M can have any arbitrary value. For the choked accretion model, we shall assume that ˙M is given by the Bondi accretion rate, i.e. α = ˙MB 4πρ = 1 4 (GM)2 a∞3 ( 2 5− 3γ ) 5−3 γ 2(γ−1) , (2.7)"

Equation (2.5) defines the central accretion rate as ˙M = 4πρα, so α = ˙M/(4πρ). Equation (2.7) then sets α = ˙MB/(4πρ), which makes ˙M = ˙MB in the analytic model by construction. Any choking of the accretion rate in Eqs. (2.8)-(2.10) is therefore an input of the toy model, not a derived prediction. The paper is transparent about this ('we shall assume') and uses it only to illustrate the in/outflow geometry; the numerical simulations do not impose ˙MB and their measured plateau is an emergent output, so this step is not load-bearing for the main claim.

full rationale

The central claim is supported by the finite-volume simulations of Section 3, which are initialized with uniform density and velocity and only impose the equatorial density contrast at the outer boundary; the inner accretion rate is measured, not prescribed, and the δ = 0 runs independently recover the Bondi solution to <1% error. The only place where the Bondi rate enters by hand is the incompressible analytic model of Section 2, where Eq. (2.7) is explicitly labelled as an assumption and later justified a posteriori from the simulations ('This justifies our choice in equation (2.7)'). Self-citations to Hernandez et al. (2014) and Tejeda (2018) supply the motivating perturbation and the irrotational ansatz, but the numerical validation and the measured flux plateau are self-contained and do not reduce to these citations. The paper also honestly discloses boundary-condition limitations ('very distinct boundary conditions may very well lead to substantially different solutions', and larger δ or smaller outer radii fail to reach steady state), which are robustness concerns rather than circularity. Hence the only circular element is the illustrative analytic model's preset Bondi rate, giving a low overall score.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The paper introduces the named mechanism 'choked accretion' and the in/outflow geometry, but no new physical entity such as a particle, force, or field. No independent evidence is needed for an invented entity because none is postulated.

free parameters (2)

density contrast delta = 0.001, 0.01, 0.1 for the three simulation series
The amplitude of the equatorial-to-polar density asymmetry in the boundary profile rho(theta) = rho0(1 - delta cos^2(theta)) is chosen by hand, not derived from a physical model. The paper explicitly states it is a convenient first-order parametrization of departures from spherical symmetry.
stagnation radius S = varies per run; e.g., 5.10 rB for gamma=1, delta=0.1% and 2.55 rB for gamma=1, delta=10%
In the analytic model (Section 2), S is introduced as the length scale in the velocity potential and is not fixed by the equations. In the simulations, S is measured as an output, so it functions as a free parameter in the analytic construction.

assumptions (5)

domain assumption Steady, axisymmetric accretion flow onto a Newtonian point mass is a valid representation of the astrophysical settings considered.
The entire paper assumes steady state and axisymmetry from the outset (Section 1 and Section 3), and the discussion of applications to YSOs, AGNs, and GRBs relies on this idealization.
domain assumption The boundary density profile rho(theta) = rho0(1 - delta cos^2(theta)) captures the essential departure from spherical symmetry.
Section 3.1 imposes this profile at the outer boundary. The authors admit in Section 4 that it is not intended as a physical model and that distinct boundary conditions may lead to substantially different solutions, making this a load-bearing modeling choice.
domain assumption The free-outflow inner boundary at Racc = 0.1 rB adequately represents accretion onto a featureless Keplerian potential.
Section 3.1 sets the inner boundary to free-outflow and notes that modeling the accretor as a star would require different boundary conditions. The choking value depends on this choice, as the paper itself acknowledges.
domain assumption The fluid is ideal and polytropic with P = K rho^gamma, with no viscosity, magnetic fields, rotation, radiation, or cooling.
The Euler equations in Section 3 and the equation of state in Eq. (3.1) omit these physical ingredients, and Section 4 explicitly discusses their likely effects but does not include them in the simulations.
standard math For the analytic model, the flow is incompressible and irrotational, so the velocity potential satisfies the Laplace equation.
Section 2 uses the standard potential-flow solution expanded in Legendre polynomials, a standard mathematical result from potential theory (Currie 2003).

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Pith. "Pith review of Choked accretion: from radial infall to bipolar outflows by breaking spherical symmetry." pith.science (2026). https://pith.science/paper/3QWNIHQQ

@misc{pith2026190900884,
  author       = {Pith},
  title        = {Pith review of: Choked accretion: from radial infall to bipolar outflows by breaking spherical symmetry},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3QWNIHQQ}},
  note         = {Machine review of arXiv:1909.00884}
}

abstract

Steady state, spherically symmetric accretion flows are well understood in terms of the Bondi solution. Spherical symmetry however, is necessarily an idealized approximation to reality. Here we explore the consequences of deviations away from spherical symmetry, first through a simple analytic model to motivate the physical processes involved, and then through hydrodynamical, numerical simulations of an ideal fluid accreting onto a Newtonian gravitating object. Specifically, we consider axisymmetric, large-scale, small amplitude deviations in the density field such that the equatorial plane is over dense as compared to the polar regions. We find that the resulting polar density gradient dramatically alters the Bondi result and gives rise to steady state solutions presenting bipolar outflows. As the density contrast increases, more and more material is ejected from the system, attaining speeds larger than the local escape velocities for even modest density contrasts. Interestingly, interior to the outflow region, the flow tends locally towards the Bondi solution, with a resulting total mass accretion rate through the inner boundary $choking$ at a value very close to the corresponding Bondi one. Thus, the numerical experiments performed suggest the appearance of a maximum achievable accretion rate, with any extra material being ejected, even for very small departures from spherical symmetry.

Figures

Figures reproduced from arXiv: 1909.00884 by the authors.

**Figure 1.** Streamlines of the incompressible analytic model showing an inner quasi-spherical accretion region, and polar stagnation points beyond which a polar outflow solution results. The red dots indicate the location of the stagnation points along the symmetry axis. The axes correspond to the usual cylindrical coordinates R = r sin θ, z = r cos θ. which leads to the velocity field dr dt = − α r 2 1 − r 3 2 S3 [PITH_FUL… view at source ↗

**Figure 2.** Mass accretion rate as a function of time for the four values of the density contrast δ in the case γ = 4/3 (similar results were obtained for the other two values of γ). There is a clear convergence towards a steady state solution. set free-outflow5 from the grid at Racc (i.e. free inflow towards the central object) and reflection conditions at both polar boundaries. At the outer boundary, at R = 10 rB, we impose … view at source ↗

**Figure 3.** Comparison of the spherically symmetric numerical simulations performed with aztekas and the Bondi accretion solution corresponding to the adiabatic indices γ = 1, 4/3, 7/5. The figure shows the Mach number versus radius for the three cases. Solid, coloured lines correspond to the Bondi solution while dashed, black lines correspond to the numerical results. The vertical dashed lines indicate the position of the so… view at source ↗

Figures from the paper (5 more)

**Figure 4.** Figure 4: Resulting steady state flow configurations for the numerical simulations for a fluid with equation of state γ = 1 accreting onto a point mass. The different values of the density contrast δ used in each case are indicated on the top-left corner of each panel. The first…

**Figure 5.** Figure 5: Resulting steady state flow configurations for the numerical simulations with γ = 4/3. The meaning of the different lines is the same as in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]

**Figure 6.** Figure 6: Resulting steady state flow configurations for the numerical simulations with γ = 7/5. The meaning of the different lines is the same as in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]

**Figure 8.** Figure 8: Ratio between the ejected and injected mass rates versus the injected mass rate in units of M˙ B (see equation 2.7) for all of the simulations reported in this work. The solid line represents the case where the accretion rate onto the central object M˙ is equal to the…

**Figure 7.** Figure 7: Close up of the inner region of the simulations with δ = 10% for the three values of γ. In the three panels we show the location of the sonic surface as extracted from the numerical simulations (dashed lines) together with the one corresponding to the Bondi solution (s…

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Choked accretion onto a Schwarzschild black hole: A hydrodynamical jet-launching mechanism
astro-ph.HE 2019-09 conditional novelty 6.0 of 10

An equatorial overdense, polar underdense accretion flow onto a Schwarzschild black hole leads to a black-hole accretion rate of about the Michel value, with the excess mass ejected as a bipolar outflow.

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Works this paper leans on

43 extracted references · 22 canonical work pages · cited by 1 Pith paper

[1]

Aguayo-Ortiz A., Mendoza S., Olvera D., 2018, PLoS ONE, 13, e0195494

2018
[2]

J., Adams C

Awe T. J., Adams C. S., Davis J. S., Hanna D. S., Hsu S. C., Cassibry J. T., 2011, Physics of Plasmas, 18, 072705

work page 2011
[3]

Bachiller R., 1996, , 34, 111

work page 1996
[4]

A., Hawley J

Balbus S. A., Hawley J. F., 1991, Astrophysical Journal, 376, 214

1991
[5]

D., 1976, Monthly Notices of the Royal Astronomical Society, 176, 465

Blandford R. D., 1976, Monthly Notices of the Royal Astronomical Society, 176, 465

work page 1976
[6]

D., Payne D

Blandford R. D., Payne D. G., 1982, Monthly Notices of the Royal Astronomical Society, 199, 883

1982
[7]

D., Rees M

Blandford R. D., Rees M. J., 1974, Monthly Notices of the Royal Astronomical Society, 169, 395

work page 1974
[8]

D., Znajek R

Blandford R. D., Znajek R. L., 1977, Monthly Notices of the Royal Astronomical Society, 179, 433

1977

Show all 43 references

[9]

Bondi H., 1952, Monthly Notices of the Royal Astronomical Society, 112, 195+

1952
[10]

F., 1980, Astrophysical Journal, 239, 982

Canto J., Rodriguez L. F., 1980, Astrophysical Journal, 239, 982

1980
[11]

Casse F., Keppens R., 2002, , 581, 988

2002
[12]

G., 2003, Fundamental mechanics of fluids , 3rd edn

Currie I. G., 2003, Fundamental mechanics of fluids , 3rd edn. New York: Marcel Dekker

2003
[13]

M., Loska Z., Zycki P

Czerny B., Niko ajuk M., R \'o \.z a \'n ska A., Dumont A. M., Loska Z., Zycki P. T., 2003, , 412, 317

2003
[14]

Del Zanna L., Velli M., Londrillo P., 1998, , 330, L13

1998
[15]

D., Leer B., 1983, SIAM Review, 25

Harten A., Lax P. D., Leer B., 1983, SIAM Review, 25

1983
[16]

F., Fendt C., Hardcastle M., Nokhrina E., Tchekhovskoy A., 2015, , 191, 441

Hawley J. F., Fendt C., Hardcastle M., Nokhrina E., Tchekhovskoy A., 2015, , 191, 441

2015
[17]

L., Rodr \' guez-Mota R

Hernandez X., Rend \'o n P. L., Rodr \' guez-Mota R. G., Capella A., 2014, Revista Mexicana de Astronom\'ia y Astrof\'isica, 50, 23

2014
[18]

arXiv:1904.09677

Jafari A., 2019, arXiv e-prints, p. arXiv:1904.09677

2019 arXiv
[19]

P., 2017, , 55, 303

Kaaret P., Feng H., Roberts T. P., 2017, , 55, 303

2017
[20]

N., Fiege J

Lery T., Henriksen R. N., Fiege J. D., Ray T. P., Frank A., Bacciotti F., 2002, , 387, 187

2002
[21]

Liska M., Tchekhovskoy A., Ingram A., van der Klis M., 2019, , 487, 550

2019
[22]

D., Guzm \'a n F

Lora-Clavijo F. D., Guzm \'a n F. S., 2013, Monthly Notices of the Royal Astronomical Society, 429, 3144

2013
[23]

Lovelace R. V. E., 1976, , 262, 649

1976
[24]

Mendoza S., Tejeda E., Nagel E., 2009, Monthly Notices of the Royal Astronomical Society, 393, 579

2009
[25]

C., 1972, Astrophysics and Space Science, 15, 153

Michel F. C., 1972, Astrophysics and Space Science, 15, 153

1972
[26]

F., Rodr \' guez L

Mirabel I. F., Rodr \' guez L. F., 1994, , 371, 46

1994
[27]

Mori S., Bai X.-N., Okuzumi S., 2019, , 872, 98

2019
[28]

30 of EAS Publications Series, A GPL Relativistic Hydrodynamical Code

Olvera D., Mendoza S., 2008, in Oscoz A., Mediavilla E., Serra-Ricart M., eds, EAS Publications Series Vol. 30 of EAS Publications Series, A GPL Relativistic Hydrodynamical Code . pp 399--400

2008
[29]

I., Shapiro S

Petrich L. I., Shapiro S. L., Teukolsky S. A., 1988, Physical Review Letters, 60, 1781

1988
[30]

E., Ouyed R., Fendt C., Brandenburg A., 2007, Protostars and Planets V, pp 277--294

Pudritz R. E., Ouyed R., Fendt C., Brandenburg A., 2007, Protostars and Planets V, pp 277--294

2007
[31]

Qian Q., Fendt C., Vourellis C., 2018, , 859, 28

2018
[32]

E., Boettcher M., Markoff S., Tavecchio F., 2017, , 207, 5

Romero G. E., Boettcher M., Markoff S., Tavecchio F., 2017, , 207, 5

2017
[33]

Semenov V., Dyadechkin S., Punsly B., 2004, Science, 305, 978

2004
[34]

I., Sunyaev R

Shakura N. I., Sunyaev R. A., 1973, Astronomy and Astrophysics, 24, 337

1973
[35]

Sheikhnezami S., Fendt C., 2018, , 861, 11

2018
[36]

Shu C.-W., Osher S., 1988, Journal of Computational Physics, 77, 439

1988
[37]

Tchekhovskoy A., 2015, 414

2015
[38]

Tejeda E., 2018, Revista Mexicana de Astronom\'ia y Astrof\'isica, 54, 171

2018
[39]

Tejeda E., Aguayo-Ortiz A., 2019, , 487, 3607

2019
[40]

arXiv:1909.01527

Tejeda E., Aguayo-Ortiz A., Hernandez X., 2019, arXiv e-prints, p. arXiv:1909.01527

2019 arXiv
[41]

Velli M., 1994, , 432, L55

1994
[42]

E., Bloom J

Woosley S. E., Bloom J. S., 2006, Annual Review of Astronomy and Astrophysics, 44, 507

2006
[43]

write newline

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Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.

[1] [1]

Aguayo-Ortiz A., Mendoza S., Olvera D., 2018, PLoS ONE, 13, e0195494

2018

[2] [2]

J., Adams C

Awe T. J., Adams C. S., Davis J. S., Hanna D. S., Hsu S. C., Cassibry J. T., 2011, Physics of Plasmas, 18, 072705

work page 2011

[3] [3]

Bachiller R., 1996, , 34, 111

work page 1996

[4] [4]

A., Hawley J

Balbus S. A., Hawley J. F., 1991, Astrophysical Journal, 376, 214

1991

[5] [5]

D., 1976, Monthly Notices of the Royal Astronomical Society, 176, 465

Blandford R. D., 1976, Monthly Notices of the Royal Astronomical Society, 176, 465

work page 1976

[6] [6]

D., Payne D

Blandford R. D., Payne D. G., 1982, Monthly Notices of the Royal Astronomical Society, 199, 883

1982

[7] [7]

D., Rees M

Blandford R. D., Rees M. J., 1974, Monthly Notices of the Royal Astronomical Society, 169, 395

work page 1974

[8] [8]

D., Znajek R

Blandford R. D., Znajek R. L., 1977, Monthly Notices of the Royal Astronomical Society, 179, 433

1977