臺灣博碩士論文加值系統

觀測上黑洞吸積系統(accreting black hole systems)的光度(Luminosity),L,與電波輻射(radio emission)的互相關聯暗示了黑洞吸積盤(accretion disk)與噴流有偶合關係。假設黑洞相對論性噴流(relativistic jets)是藉由旋轉黑洞的轉動動能提供能量，我們檢視了當黑洞吸積盤隨其光度(以愛丁頓光度(Eddington Liminosity)，LEdd，為單位)變化而改變種類時，黑洞的能量是否能被抽取出來(產生噴流)。在此論文中，我們主要討論相對論性噴流為何能夠在吸積盤成為薄盤狀前產生(當L/LEdd 漸漸接近約0.01前)。經由相對論性流體力學(general relativistic magnetohydrodynamics)的討論，我們發現黑洞轉動能量容易在黑洞被一種混合外部薄盤(thin disk)及內部水平對流主導吸積流(advection-dominated accretion flow)的吸積盤所包圍時,經由"磁流體Penrose過程(MHD Penrose Process)"被抽取出來。這類混合薄盤與水平對流主導吸積流的吸積盤曾經被用來解釋黑洞X射線雙星(black hole X-ray binaries)和活躍星系核(active galactic nuclei)的光譜表現。我們的模型也解釋了為何射電光度與噴流速度兩者皆隨著X射線光度上升而增加。此外，我們提出關於為何當L/LEdd約等於0.01時噴流被抑制，以及為何在L/LEdd 大於 0.01和 L/LEdd 小於0.01時產生的噴流有不同的功率(power)和速度的可能解釋。我們建議，對於不同種類的吸積盤，在黑洞視像地平面(event horizon)附近，當吸積流速度從次音速到超音速時的吸積流幾何形狀(transonic flow geometry)，以及被吸積盤束縛的大尺度磁場兩者對抽取黑洞轉動動能及噴流的產生有重要的影響。

Observed correlations between the disk luminosity (L) and radio emission from accreting black hole (BH) systems indicate underlying couplings between BH accretion disk and jet. Assuming relativistic jets are launched at the expense of the rotational energy of spinning BHs, we examine whether the BH energy can be extracted outward when the accretion disk type varies with L/LEdd, where LEdd
is the Eddingtion luminosity. In this thesis, we mainly focus on why relativistic jet is launched before the disk is dominated by the thin disk type (before L/LEdd approaches the value ∼ 0.01), as inferred from observation. Considering the general relativistic magnetohydrodynamics (MHD), we found the extraction of BH energy via the “MHD Penrose process” (and hence the relativistic jet)can preferentially take place when the BH is surrounded by a disk which consists a (outer) thin disk
and an (inner) advection-dominated flow. Such combined disk has been inferred from the spectra of both BH X-ray binaries and active galactic nuclei. Our model also consistently explains why both the radio luminosity and jet speed increase with increasing X-ray luminosity. In addition, we propose possible explanations why jet are quenched at when L/LEdd ∼ 0.01 and why the jets launched when L/LEdd > 0.01 has different jet power and jet speed than those launched when L/LEdd < 0.01. It is suggested that, for different types of accretion disks, both the transonic flow geometry near the horizon, and the large–scale magnetic field confined by the disk, play essential roles in affecting the extraction of BH rotational energy and hence the jet formation.

1 Introduction
1.1 Black Hole Disk-Jet Coupling: Observation
1.2 Overview of Black Hole Accretion Disk Theories
1.3 Overview of Relativistic Jet Formation Theories
1.4 The Transonic Nature of the Accretion Flow
1.5 MHD Flows around a Rotating Black Hole
1.5.1 The Relativistic Bernoulli Equation
1.5.2 The Cold Limit
1.5.3 Separation Point
1.5.4 Light Surfaces
1.5.5 Critical Points
1.5.6 Negative Energy Flow
1.5.7 Outward Energy Flux
1.5.8 Relativistic Jet Formation Theories– Revisit

2 Formation of Relativistic Jet at Low Accretion Rate
2.1 Overview of the Model
2.2 Assumptions
2.3 Method
2.3.1 Estimating the Field Strength and the Mass Loading
2.3.2 Solving the Relativistic Bernoulli Equation for the Location of the Alfven Point
2.4 Results and Discussion
2.4.1 Results
2.4.2 Universal Paradigm of Black Hole Disk-Jet Coupling at Low Accretion Rate
2.4.3 Universal Paradigm of Black Hole Disk-Jet Coupling at Low Accretion Rate
2.4.4 The Estimated Speed of Ergospheric Jet
2.4.5 Validity of the Model

3 Outlook
3.1 Quenching of Black Hole relativistic Jet: a Possible Reason
3.1.1 The Transonic Flow Geometry of a Thin Disk
3.1.2 Universal Paradigm of Black Hole Disk-Jet Coupling at Low Accretion Rate– Revisited
3.2 Two Types of Ergospheric Jet
3.2.1 Jet Power
3.2.2 Jet Speed
3.2.3 The Dichotomy of Fanaroff-Riley I and Fanaroff-Riley II Galaxies

4 Summary

A Electromagnetic Counter Torque induced by the Frame Dragging Effect

B Analytical Solution of the Accretion Disks

C Parameterized the Large-Scale Magnetic Field Strength

D Unifying the Disk Solutions on the aurface density – accretion rate Plane
D.1 Optically Thick Solutions
D.1.1 Assumptions
D.1.2 The Energy Equation
D.1.3 Solving the “S” curve
D.2 Optically Thin Solutions

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