Wakefield Acceleration Towards ZeV from a Black Hole Emanating Astrophysical Jets

Hydromagnetic disk winds have great potential as a general theory for the production and collimation of astrophysical jets in both protostellar and black hole environments. We first review the analytic stationary theory of these outflows as well as recent numerical simulations of MHD disk winds. We then focus on simulations that we have done on winds from magnetized disks using the ZEUS 2-D code of Stone and Norman. We treat the Keplerian disk as a fixed platform throughout the simulations. We show that both stationary and episodic, jet-like outflows are driven from disks depending upon their magnetic structure and mass loss rates.

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Wakefield acceleration towards ZeV from a black hole emanating astrophysical jets

International Journal of Modern Physics A ◽

10.1142/s0217751x19430188 ◽

2019 ◽

Vol 34 (34) ◽

pp. 1943018

Author(s):

T. Ebisuzaki ◽

T. Tajima

Keyword(s):

Particle Interaction ◽

Cosmic Ray ◽

High Energy ◽

Rotational Instability ◽

Astrophysical Jets ◽

Electromagnetic Pulses ◽

High Energy Cosmic Rays ◽

Acceleration Mechanism ◽

Wakefield Acceleration ◽

Pondermotive Force

We consider that electromagnetic pulses produced in the jets of this innermost part of the accretion disk accelerate charged particles (protons, ions, electrons) to very high energies via wakefield acceleration, including energies above 10[Formula: see text] eV for the case of protons and nucleus and 10[Formula: see text] eV for electrons by electromagnetic wave-particle interaction. Thereby, the wakefield acceleration mechanism supplements the pervasive Fermi’s stochastic acceleration mechanism (and overcomes its difficulties in the highest energy cosmic ray generation). The episodic eruptive accretion in the disk by the magneto-rotational instability gives rise to the strong Alfvenic pulses, which acts as the driver of the collective accelerating pondermotive force. This pondermotive force drives the wakes. The accelerated hadrons (protons and nuclei) are released to the intergalactic space to be ultra-high energy cosmic rays. The high-energy electrons, on the other hand, emit photons to produce various non-thermal emissions (radio, IR, visible, UV, and gamma-rays) of active galactic nuclei in an episodic manner, giving observational telltale signatures.

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Inherent and Local Magnetic Field Structures in Jets from Active Galactic Nuclei

Galaxies ◽

10.3390/galaxies9030058 ◽

2021 ◽

Vol 9 (3) ◽

pp. 58

Author(s):

Denise C. Gabuzda

Keyword(s):

Black Hole ◽

Active Galactic Nuclei ◽

Accretion Disk ◽

Field Component ◽

Galactic Nuclei ◽

Intrinsic Property ◽

Theoretical Models ◽

Local Magnetic Field ◽

Astrophysical Jets ◽

Wide Range

In theoretical models for the electromagnetic launching of astrophysical jets, a helical magnetic (B)-field component is generated through the winding up of an initial longitudinal field component by the rotation of the cental black hole and accretion disk. This helical field component travels outward with the jet plasma. There is now abundant evidence that the jets of active galactic nuclei carry helical B fields, and the presence of such fields has been invoked to explain a wide range of phenomena observed in these jets. However, distinguishing between features associated with this inherent jet B field and with B fields generated by local phenomena such as shocks and shear can be challenging. There is now evidence that the field that is accreted is dipolar like, giving rise to a current distribution with inward currents along both jet axes and outward currents in a more extended region around the jets. Striking limb brightening has been observed for several relatively nearby active galactic nuclei; it is argued that this must be due to some intrinsic property of the jet, which is independent of the viewing angle, such as its helical B field, or mass loading and/or particle acceleration at the jet edges. Circular-polarization observations may make it possible to reconstruct the full three-dimensional B field of jets carrying a helical B-field component, and to correctly infer the direction of rotation of the central black hole and its accretion disk.

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Sweeping-Magnetic-Twist Mechanism and Molecular Bipolar Flows

Symposium - International Astronomical Union ◽

10.1017/s0074180900096029 ◽

1987 ◽

Vol 115 ◽

pp. 385-387

Author(s):

Kazunari SHIBATA ◽

Yutaka UCHIDA

Keyword(s):

Magnetic Field ◽

Black Hole ◽

Active Galactic Nuclei ◽

Accretion Disks ◽

Large Scale ◽

Galactic Nuclei ◽

Main Mechanism ◽

Astrophysical Jets ◽

Centrifugal Effect ◽

Poloidal Magnetic Field

Uchida and Shibata have proposed the “sweeping-magnetic-twist” mechanism for the formation of astrophysical jets in relation to the accretion disks (disks around protostars, around black hole in the center of active galactic nuclei, and so on) in which a jet is accelerated by thejxBforce in the relaxing magnetic twist created in the winding-up of the poloidal magnetic field by the rotation of the contracting disk (Uchida and Shibata 1985a, b; Shibata and Uchida 1986a, b; Uchidaet al.1985). In this mechanism, a jet is collimated also by thejxBforce due to the large scale poloidal magnetic field whose footpoints are squeezed in the contracting disk. The main mechanism involved is different from that of centrifugal wind models (Blandford and Payne 1982, Pudritz and Norman 1983) and worked out indepentently, but the centrifugal effect itself is automatically built-in.

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Simulations of Neutrino and Gamma-Ray Production from Relativistic Black-Hole Microquasar Jets

Galaxies ◽

10.3390/galaxies9030067 ◽

2021 ◽

Vol 9 (3) ◽

pp. 67

Author(s):

Theodora Papavasileiou ◽

Odysseas Kosmas ◽

Ioannis Sinatkas

Keyword(s):

Black Hole ◽

Electromagnetic Radiation ◽

Binary Systems ◽

Gamma Ray ◽

Large Magellanic Cloud ◽

High Energy ◽

X Rays ◽

Fermi Acceleration ◽

Astrophysical Jets ◽

Model Calculations

Recently, microquasar jets have aroused the interest of many researchers focusing on the astrophysical plasma outflows and various jet ejections. In this work, we concentrate on the investigation of electromagnetic radiation and particle emissions from the jets of stellar black hole binary systems characterized by the hadronic content in their jets. Such emissions are reliably described within the context of relativistic magneto-hydrodynamics. Our model calculations are based on the Fermi acceleration mechanism through which the primary particles (mainly protons and electrons) of the jet are accelerated. As a result, a small portion of thermal protons of the jet acquire relativistic energies, through shock-waves generated into the jet plasma. From the inelastic collisions of fast (non-thermal) protons with the thermal (cold) ones, secondary charged and neutral particles (pions, kaons, muons, η-particles, etc.) are created, as well as electromagnetic radiation from the radio wavelength band to X-rays and even very high energy gamma-rays. One of our main goals is, through the appropriate solution of the transport equation and taking into account the various mechanisms that cause energy losses to the particles, to study the secondary particle concentrations within hadronic astrophysical jets. After assessing the suitability and sensitivity of the derived (for this purpose) algorithms on the Galactic MQs SS 433 and Cyg X-1, as a concrete extragalactic binary system, we examine the LMC X-1 located in the Large Magellanic Cloud, a satellite galaxy of our Milky Way Galaxy. It is worth mentioning that, for the companion O star (and its extended nebula structure) of the LMC X-1 system, new observations using spectroscopic data from VLT/UVES have been published a few years ago.

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