The effect of large-scale magnetic field on outflow in ADAFs: an odd symmetry configuration

Samadi, Maryam; Abbassi, Shahram

doi:10.1093/mnras/stv2466

Cited by 21 publications

(29 citation statements)

References 61 publications

(58 reference statements)

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“…The magnetic field plays a crucial role in the dynamical structure and the observational properties of accretion disc. Kaburaki (2000), Abbassi et al (2010 ), Ghasemnezhad et al(2012), , Samadi & Abbassi (2016), and Samadi et al (2014) studied the effect of magnetic field on hot accretion flow (ADAF) in the recent years. But the magnetized slim disc model has been less studied.…”

Section: Introductionmentioning

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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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: Introductionmentioning

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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“…In the one-dimensional works, the existence of wind is often an assumption (e.g. Blandford & Begelman 1999;Akizuki & Fukue 2006;Abbassi et al 2008;Zhang & Dai 2008;Bu et al 2009 Mosallanezhad et al 2014;Gu 2015;Samadi & Abbassi 2016 ) but not all (e.g., Narayan & Yi 1995 and references therein). In all these works magnetic field is not included.…”

Section: Introductionmentioning

confidence: 99%

Two-dimensional inflow-wind solution of black hole accretion with an evenly symmetric magnetic field

Mosallanezhad

Yuan

2015

Mon. Not. R. Astron. Soc.

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We solve the two-dimensional magnetohydrodynamic (MHD) equations of black hole accretion with the presence of magnetic field. The field includes a turbulent component, whose role is represented by the viscosity, and a large-scale ordered component. The latter is further assumed to be evenly symmetric with the equatorial plane. The equations are solved in the r − θ plane of a spherical coordinate by assuming timesteady and radially self-similar. An inflow-wind solution is found. Around the equatorial plane, the gas is inflowing; while above and below the equatorial plane at a certain critical θ angle, θ ∼ 47 • , the inflow changes its direction of radial motion and becomes wind. The driving forces are analyzed and found to be the centrifugal force and the gradient of gas and magnetic pressure. The properties of wind are also calculated. The specific angular momentum of wind is found to be significantly larger than that of inflow, thus wind can transfer angular momentum outward. These analytical results are compared to those obtained by the trajectory analysis based on MHD numerical simulation data and good agreements are found.

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“…Figure 6 displays isodensity contours for the asymmetric configuration of disk which is caused by asymmetric poloidal magnetic field. In the reflection symmetry of quantities, isodensity contours usually make close shapes such as Fig.2 of Samadi et al (2016). But here, non-zero B r in the mid-plane makes isodensity contour to be different in upper and lower sides of the disk.…”

Section: Vertical Structurementioning

confidence: 95%

“…the above equation is the result of ∂B r /∂t = 0 and ∂B θ /∂t = 0 (for more details refer to Samadi & Abbassi 2016). To satisfy ∇ · B = 0 we can express the poloidal magnetic field in terms of a flux function ψ(r, θ) (Lovelace et al 1987),…”

Section: Equationsmentioning

confidence: 99%

“…Some of them (e.g. Shadmehri 2004, Ghanbari et al 2007, Shaghaghian 2011, 2016) studied purely poloidal magnetic fields and many concentrated only toroidal fields (Akizuki & Fukue 2006, Khesali & Faghei 2008, Mosallanezhad et al 2014, 2016, Sarkar & Das 2016) and a few theoritical works have been recently done with the global magnetic field (Samadi & Abbassi 2016, Mosallanezhad et al 2016, Samadi et al 2017.…”

Section: Introductionmentioning

confidence: 99%

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Anchoring Polar Magnetic Field in a Stationary Thick Accretion Disk

Samadi

Abbassi

2017

ApJ

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We investigate the properties of a hot accretion flow bathed in a poloidal magnetic field. We consider an axisymmetric viscous resistive flow in the steady state configuration. We assume the dominant mechanism of energy dissipation is due to turbulence viscosity and magnetic diffusivity. A certain fraction of that energy can be advected towards the central compact object. We employ self-similar method in the radial direction to find a system of ODEs with just one varible, θ in the spherical coordinates. For the existence and maintaining of a purely poloidal magnetic in a rotating thick disk, we find the necessary condition is a constant value of angular velocity along a magnetic field line. We obtain an analytical solution for the poloidal magnetic flux. We explore possible changes in the vertical structure of the disk under the influences of even symmetric and asymmetric magnetic fields. Our results reveal that a polar magnetic field with even symmetry about the equatorial plane makes the disk vertically thin. Moreover, the accretion rate decreases when we consider a strong magnetic field. Finally, we notice hot magnetized accretion flows can be fully advected even in a slim shape.

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The effect of large-scale magnetic field on outflow in ADAFs: an odd symmetry configuration

Cited by 21 publications

References 61 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

Two-dimensional inflow-wind solution of black hole accretion with an evenly symmetric magnetic field

Anchoring Polar Magnetic Field in a Stationary Thick Accretion Disk

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