The Influences of Outflow on the Dynamics of Inflow

Xie, Fu-Guo; Yuan, Feng

doi:10.1086/588522

Cited by 55 publications

(70 citation statements)

References 26 publications

(38 reference statements)

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“…It was assumed that outflow contributes to loss of mass, angular momentum, and thermal energy from accretion discs. By using the method presented by Bu et al (2009) andXi &Yuan (2008) we consider the discontinuity between mass, momentum (radial and azimuthal components of momentum) and energy outflow and inflow. Also simulations have indicated that the large scale ordered magnetic field exists in the accretion disc and can produce outflow in both cold and hot accretion flow.…”

Section: Discussionmentioning

confidence: 99%

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The influence of large-scale magnetic field in the structure of supercritical accretion flow with outflow

Ghasemnezhad

Abbassi

2017

Monthly Notices of the Royal Astronomical Society

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We present the effects of ordered large scale magnetic field on the structure of supercritical accretion flow in the presence of outflow. In the cylindrical coordinates (r, ϕ, z), We write the 1.5 dimensional, the steady state ( ∂ ∂t = 0) and axisymmetric ( ∂ ∂ϕ = 0) inflow-outflow equations by using the self similar solutions. Also a model for radiation pressure supported accretion flow threaded by both toroidal and vertical components of magnetic field has been formulated. For studying the outflows, we adopt a radius dependent mass accretion rate aṡ M =Ṁ out ( . Also by following the previous works, we have considered the interchange of mass, radial and angular momentum and the energy between inflow and outflow. we have found numerically that two components of magnetic field have the opposite effects on the thickness of the disc and similar effects on the radial and angular velocities of the flow. We have found that the existence of the toroidal component of magnetic field will lead to increasing of radial and azimuthal velocities as well as the relative thickness of the disc, which is increased . Moreover, the thickness of the disc will decrease when the vertical component of magnetic field becomes important in magnetized flow. The solutions indicated that the mass inflow rate, the specific energy of outflow affect strongly on the advection parameter.We have shown that by increasing the two components of magnetic field, the temperature of the accretion flow will decrease significantly. On the other hand we have shown the bolometric luminosity of the slim discs for high values ofṁ(ṁ >> 1) is not sensitive to mass accretion rate and is kept constant (L ≈ 10L E ).

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Section: Discussionmentioning

confidence: 99%

“…Apparently, it is almost impossible to solve the equations directly. We therefore, following Xie & Yuan (2008), we introduce the parameters ζ1 and ζ2 to evaluate radial and angular velocities of outflow in terms of inflow: vr,w = ζ1vr, vϕ,w = ζ2vϕ.…”

Section: Basic Equationsmentioning

confidence: 99%

The influence of large-scale magnetic field in the structure of supercritical accretion flow with outflow

Ghasemnezhad

Abbassi

2017

Monthly Notices of the Royal Astronomical Society

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“…Recent development in observations has shown more and more evidence of outflows in accretion systems, such as Sgr A* (Marrone et al 2006;Xie & Yuan 2008), soft Xray transients (Loeb et al 2001) and quasars with blueshifted absorption lines (e.g., PG1115+80; Chartas et al 2003). Many two-or three-dimensional numerical simulations of accretion disks have also found outflow in their results (e.g.…”

Section: Introductionmentioning

confidence: 99%

Outflows from Accretion Disks around Compact Objects

Jiao¹,

Wu²

2012

Proc. IAU

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Abstract. We solve the set of hydrodynamic equations for accretion disks in the spherical coordinates (rθφ) to obtain the explicit structure along the θ direction. The results display thinner, quasi-Keplerian disks for Shakura-Sunyaev Disks (SSDs) and thicker, sub-Keplerian disks for Advection Dominated Accretion Flows (ADAFs) and slim disks, which are consistent with previous popular analytical models, while an inflow region and an outflow region always exist, which supports the results of some recent numerical simulation works. Our results indicate that the outflows should be common in various accretion disks and stronger in slim disks and ADAFs.

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“…It is noted that the initial specific angular momentum of outflow matter is no greater than that of the accreting matter on the disc. Outflow can contribute to the overall equilibrium, provided that there exists some interaction between the outflow and the disc [19].(5) Large-scale magnetic field. Analogous to the MC process, angular momentum can be taken away very efficiently by virtue of some "open" magnetic field lines anchored in the accretion disc in either Poynting or hydromagnetic fluxes, e.g., the BP process [11,[20][21][22].…”

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confidence: 99%

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Energy dissipation and angular momentum transfer within a magnetically torqued accretion disc

Gan

Wang

Lei

et al. 2010

Sci. China Phys. Mech. Astron.

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We discuss transportation and redistribution of energy and angular momentum in the magnetic connection (MC) process and Blandford-Payne (BP) process. The MC results in readjusting the interior viscous torque, and its effects are operative not only in but also beyond the MC region. The BP process is invoked to transfer the "excessive" angular momentum from an accretion disc. In addition, we derive a criterion for the interior viscous torque to resolve the puzzle of the overall equilibrium of angular momentum in disc accretion. It turns out that the BP efficiency of extracting angular momentum and the intensity of the outflow are required to be greater than some critical values.accretion: accretion discs, black hole physics, magnetic field, angular momentum transfer Disc accretion is widely regarded as an effective energy mechanism of high-energy phenomena in AGNs, X-ray binaries and some other compact objects. The interior viscous torque due to differential rotation transfers angular momentum outward to make accreting matter fall inward, and energy of disc radiation arises from dissipation of gravitational binding energy [1][2][3][4].Rotating energy of a fast spinning black hole is another energy source for disc radiation. A black hole can exert a significant torque at its surrounding disc via large-scale magnetic field, and this mechanism is referred to as the magnetic connection (MC) process. The Poynting flux is injected into the inner disc in the MC process, resulting in the enhanced dissipation more concentrated in the inner disc [5,6]. This feature can be used to interpret the very steep emissivity index of MCG-6-30-15 required by the observed Fe Kα line [7][8][9][10].On the other hand, large-scale magnetic fields also play an important role in jet production, e.g. via BlandfordPayne (BP) process [11][12][13][14]. Recently, Miller et al. pointed out that the X-ray-absorbing wind discovered in the observation of GRO J1655-40 must be powered by a magnetic process, by which angular momentum can also be transferred efficiently out of the disc [15].It is well known that angular momentum transfer is of fundamental importance in disc accretion. A potential barrier arising from continuous transfer of "excessive" angular momentum outward by the interior viscous torque blocks accretion at outer disc, and this problem is referred to as a puzzle of overall equilibrium of angular momentum of accretion discs. The following processes could be invoked to remove the "excessive" angular momentum from the disc:(1) Tidal interaction. It has been argued that the tidal interaction with the companion star can exert a decelerating torque on the outer boundary, and transfer the excessive angular momentum of accretion disc to the bulk revolution of a binary system [16].(2) Radiation. Angular momentum can be taken away from the disc by radiation. However, the efficiency is very low as argued in the next section of this paper. Probably, angular momentum can be carried away by gravitational wave in a very violent burst.(3) Exterior str...

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The Influences of Outflow on the Dynamics of Inflow

Cited by 55 publications

References 26 publications

The influence of large-scale magnetic field in the structure of supercritical accretion flow with outflow

The influence of large-scale magnetic field in the structure of supercritical accretion flow with outflow

Outflows from Accretion Disks around Compact Objects

Energy dissipation and angular momentum transfer within a magnetically torqued accretion disc

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