Structure of advection-dominated accretion discs with outflows: the role of toroidal magnetic fields
文献类型：期刊论文
| 作者 | Mosallanezhad, A.1,2; Abbassi, S.3,4; Beiranvand, N.5 |
| 刊名 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
 |
| 出版日期 | 2014-02-01 |
| 卷号 | 437期号:4页码:3112-3123 |
| 关键词 | accretion accretion discs black hole physics MHD stars: winds outflows |
| 英文摘要 | The main aim of this article is to study the effect of toroidal magnetic fields on the structure of advection-dominated accretion flows (ADAFs) in the presence of turbulence viscosity and diffusivity due to viscosity and magnetic field respectively. We use the self-similar assumption in the radial direction to solve the magnetohydrodynamic equations for a hot accretion disc. We use spherical coordinates (r, theta, phi) to solve our equation. The toroidal component of magnetic field is considered and all three components of the velocity field v equivalent to (v(r),v(o), v(psi)) are present in our work. We reduce the equations to a set of differential equations in theta and apply a symmetric boundary condition at the equatorial plane of the disc. Our results indicate that the outflow region, where the radial velocity becomes positive at a certain inclination angle theta(0), always exists. The results illustrate that the stronger the magnetic field, the smaller the inclination angle theta(0) becomes. This means that a magnetized disc is thinner compared with a non-magnetized disc. According to the work of Jiao & Wu, we can define three regions. The first is called the inflow region, which starts from the disc mid-plane and extends to a certain inclination theta(0) where v(r)(theta(0)) = 0. In this region, the velocity has a negative value and the accretion material moves towards the central object. The outflow region, where v(r)(theta) > 0, is placed between theta(0) and the surface of the disc, theta(0) < theta < theta(s). In this area, the accretion flow moves away from the central object. The third region, which is located between the surface of the disc and the polar axis, is called the wind region. This area is very narrow and material is blown out from the surface in the form of wind. In this article, we consider two parameters to illustrate the magnetic field effects. These parameters are the ratio of gas pressure to magnetic pressure in the equatorial plane of the disc, beta(0), and also the magnetic diffusivity parameter, eta(0). Numerical calculations with our model have revealed that the toroidal component of magnetic field has a significant effect on the vertical structure of an accretion disc. |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | SELF-SIMILAR SOLUTIONS ; BLACK-HOLE ACCRETION ; THERMAL CONDUCTION ; NUMERICAL-SIMULATION ; DRIVEN ACCRETION ; SAGITTARIUS-A ; 2 DIMENSIONS ; RADIO JETS ; FLOWS ; DISKS |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000329177100008 |
| 源URL | [http://119.78.226.72/handle/331011/18172]  |
| 专题 | 上海天文台_星系宇宙学重点实验室 |
| 作者单位 | 1.Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China 2.Univ Chinese Acad Sci, Beijing 100049, Peoples R China 3.Ferdowsi Univ Mashhad, Sch Sci, Dept Phys, Mashhad 917751436, Iran 4.Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran 5.Damghan Univ, Sch Phys, Damghan, Iran |
| 推荐引用方式 GB/T 7714 | Mosallanezhad, A.,Abbassi, S.,Beiranvand, N.. Structure of advection-dominated accretion discs with outflows: the role of toroidal magnetic fields[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2014,437(4):3112-3123. |
| APA | Mosallanezhad, A.,Abbassi, S.,&Beiranvand, N..(2014).Structure of advection-dominated accretion discs with outflows: the role of toroidal magnetic fields.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,437(4),3112-3123. |
| MLA | Mosallanezhad, A.,et al."Structure of advection-dominated accretion discs with outflows: the role of toroidal magnetic fields".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 437.4(2014):3112-3123. |
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来源：上海天文台
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