A Quasi-static Hyper-resistive Model of Ultra-high-energy Cosmic-ray Acceleration by Magnetically Collimated Jets Created by Active Galactic Nuclei
Abstract
This is the fourth in a series of companion papers showing that when an efficient dynamo can be maintained by accretion disks around supermassive black holes in active galactic nuclei, it will lead to the formation of a powerful, magnetically collimated helix that could explain the observed jet/radiolobe structures on very large scales. In this work, we present a hyper-resistive kinetic theory that shows how different instabilities can cause the slowly evolving magnetically collimated jets to accelerate ions and electrons in different regions of jets and lobes. In particular, we propose that the Drift Cyclotron Loss Cone instability at the ends of jets can accelerate ions up to the observed ultra-high-energy cosmic rays with energies ≈1020 eV. Based on this jet/lobe structure model and its associated acceleration processes, we estimate cosmic-ray intensities and likely radiative signatures and compare them with observations.
- Authors:
-
- Univ. of California, Berkeley, CA (United States)
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Univ. of California, Berkeley, CA (United States); Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
- Publication Date:
- Research Org.:
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- USDOE Laboratory Directed Research and Development (LDRD) Program
- OSTI Identifier:
- 1764229
- Report Number(s):
- LA-UR-20-28592
Journal ID: ISSN 1538-4357; TRN: US2206156
- Grant/Contract Number:
- 89233218CNA000001
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 885; Journal Issue: 1; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; cosmic ray acceleration; accretion disks; jets; hyper-resistivity
Citation Formats
Fowler, T. Kenneth, Li, Hui, and Anantua, Richard. A Quasi-static Hyper-resistive Model of Ultra-high-energy Cosmic-ray Acceleration by Magnetically Collimated Jets Created by Active Galactic Nuclei. United States: N. p., 2019.
Web. doi:10.3847/1538-4357/ab44bc.
Fowler, T. Kenneth, Li, Hui, & Anantua, Richard. A Quasi-static Hyper-resistive Model of Ultra-high-energy Cosmic-ray Acceleration by Magnetically Collimated Jets Created by Active Galactic Nuclei. United States. https://doi.org/10.3847/1538-4357/ab44bc
Fowler, T. Kenneth, Li, Hui, and Anantua, Richard. Thu .
"A Quasi-static Hyper-resistive Model of Ultra-high-energy Cosmic-ray Acceleration by Magnetically Collimated Jets Created by Active Galactic Nuclei". United States. https://doi.org/10.3847/1538-4357/ab44bc. https://www.osti.gov/servlets/purl/1764229.
@article{osti_1764229,
title = {A Quasi-static Hyper-resistive Model of Ultra-high-energy Cosmic-ray Acceleration by Magnetically Collimated Jets Created by Active Galactic Nuclei},
author = {Fowler, T. Kenneth and Li, Hui and Anantua, Richard},
abstractNote = {This is the fourth in a series of companion papers showing that when an efficient dynamo can be maintained by accretion disks around supermassive black holes in active galactic nuclei, it will lead to the formation of a powerful, magnetically collimated helix that could explain the observed jet/radiolobe structures on very large scales. In this work, we present a hyper-resistive kinetic theory that shows how different instabilities can cause the slowly evolving magnetically collimated jets to accelerate ions and electrons in different regions of jets and lobes. In particular, we propose that the Drift Cyclotron Loss Cone instability at the ends of jets can accelerate ions up to the observed ultra-high-energy cosmic rays with energies ≈1020 eV. Based on this jet/lobe structure model and its associated acceleration processes, we estimate cosmic-ray intensities and likely radiative signatures and compare them with observations.},
doi = {10.3847/1538-4357/ab44bc},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 885,
place = {United States},
year = {Thu Oct 24 00:00:00 EDT 2019},
month = {Thu Oct 24 00:00:00 EDT 2019}
}
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