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Abstract
Relativistic jets are collimated plasma outflows with relativistic speeds. Astrophysical objects involving relativistic jets are a system comprising a compact object such as a black hole, surrounded by rotating accretion flows, with the relativistic jets produced near the central compact object. The most accepted models explaining the origin of relativistic jets involve magnetohydrodynamic (MHD) processes. Over the past few decades, many general relativistic MHD (GRMHD) codes have been developed and applied to model relativistic jet formation in various conditions. This short review provides an overview of the recent progress of GRMHD simulations in generating relativistic jets and their modeling for observations.
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Abstract
The generation of relativistic jets in active sources such as blazars is a complex problem with many aspects, most of them still not fully understood. Relativistic jets are likely produced by the accretion of matter and magnetic fields onto spinning black holes. Ergospheric dragging effects launch a Poynting-dominated outflow in the polar directions of these systems. Observations with very high resolution of the jet in the nearby radio galaxy M87 and evidence of extremely fast variability in the non-thermal radiation of several other objects indicate that charged particles produce synchrotron emission and gamma rays very close to the base of the jet. How these particles are injected into the magnetically shielded outflow is a mystery. Here we explore the effects of various processes in the hot accretion inflow close to the black hole that might result in the copious production of neutral particles which, through annihilation and decay in the jet’s funnel, might load the outflow with mass and charged particles on scales of a few Schwarzschild radii.
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PKS 2155-304: A Case Study of Blazar Variability Power Spectrum at the Highest Energies and on the Longest Timescales. GALAXIES 2019. [DOI: 10.3390/galaxies7030073] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
We present the results of our Power Spectral Density (PSD) analysis for the BL Lac object PKS 2155−304, utilizing the nightly-binned long-term light curve from the decade-long monitoring, as well as the minute-binned intra-night light curve from the High Energy Stereoscopic Survey (H.E.S.S.; >200 GeV). The source is unique for exhibiting the shortest flux-doubling timescale at Very High Energy (VHE) among its class and thus provides a rare opportunity to study the particle acceleration on the smallest spatial scales in blazar jets. The light curves are modeled in terms of the Continuous-Time Auto-Regressive Moving Average (CARMA) process. The combined long-term and intra-night PSD extends up to ∼6 decades in the temporal frequency range; unprecedented at the TeV energies for a blazar source. Our systematic approach reveals that PKS 2155−304 shows, on average, a complex shape of variability power spectrum, with more variability power on longer timescales. The long-term variability is best modeled by the CARMA(2,1) process, while the intra-night variability is modeled by a CARMA(1,0) process. We note that the CARMA(1,0) process refers to an Ornstein–Uhlenbeck process where the power-law PSD slope (PSD varies as a function of variability frequency to the power of the negative slope) changes from two to zero, above a certain “characteristic/relaxation” timescale. Even though the derived power spectrum of the intra-night light curve did not reveal a flattening, we speculate such relaxation must occur on timescales longer than a few hours for the source.
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Abstract
Black holes represent extreme conditions of physical laws. Predicted about a century ago, they are now accepted as astrophysical reality by most of the scientific community. Only recently has more direct evidence of their existence been found—the detection of gravitational waves from black hole mergers and of the shadow of a supermassive black hole in the center of a galaxy. Astrophysical black holes are typically embedded in an active environment which is affected by the strong gravity. When the environmental material emits radiation, this radiation may carry imprints of the black hole that is hosting the radiation source. In order to understand the physical processes that take place in the close neighborhood of astrophysical black holes, numerical methods and simulations play an essential role. This is simply because the dynamical evolution and the radiative interaction are far too complex in order to allow for an analytic solution of the physical equations. A huge progress has been made over the last decade(s) in the numerical code development, as well as in the computer power that is needed to run these codes. This review tries to summarize the basic questions and methods that are involved in the undertaking of investigating the astrophysics of black holes by numerical means. It is intended for a non-expert audience interested in an overview over this broad field. The review comes along without equations and thus without a detailed expert discussion of the underlying physical processes or numerical specifics. Instead, it intends to illustrate the richness of the field and to motivate further reading. The review puts some emphasis on magneto-hydrodynamic simulations but also touches radiation transfer and merger simulations, in particular pointing out differences in these approaches.
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Abstract
Numerical simulations have been playing a crucial role in the understanding of jets from active galactic nuclei (AGN) since the advent of the first theoretical models for the inflation of giant double radio galaxies by continuous injection in the late 1970s. In the almost four decades of numerical jet research, the complexity and physical detail of simulations, based mainly on a hydrodynamical/magneto-hydrodynamical description of the jet plasma, have been increasing with the pace of the advance in theoretical models, computational tools and numerical methods. The present review summarizes the status of the numerical simulations of jets from AGNs, from the formation region in the neighborhood of the supermassive central black hole up to the impact point well beyond the galactic scales. Special attention is paid to discuss the achievements of present simulations in interpreting the phenomenology of jets as well as their current limitations and challenges.
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The Mochi LabJet Experiment for Measurements of Canonical Helicity Injection in a Laboratory Astrophysical Jet. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4365/aaba6f] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Multiwavelength Observations of Relativistic Jets from General Relativistic Magnetohydrodynamic Simulations. GALAXIES 2018. [DOI: 10.3390/galaxies6010031] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
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Sun L, Paschalidis V, Ruiz M, Shapiro SL. Magnetorotational collapse of supermassive stars: Black hole formation, gravitational waves, and jets. PHYSICAL REVIEW. D. (2016) 2017; 96:043006. [PMID: 30038964 PMCID: PMC6053688 DOI: 10.1103/physrevd.96.043006] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
We perform magnetohydrodynamic simulations in full general relativity of uniformly rotating stars that are marginally unstable to collapse. These simulations model the direct collapse of supermassive stars (SMSs) to seed black holes that can grow to become the supermassive black holes at the centers of quasars and active galactic nuclei. They also crudely model the collapse of massive Population III stars to black holes, which could power a fraction of distant, long gamma-ray bursts. The initial stellar models we adopt are Γ = 4/3 polytropes initially with a dynamically unimportant dipole magnetic field. We treat initial magnetic-field configurations either confined to the stellar interior or extending out from the stellar interior into the exterior. We find that the black hole formed following collapse has mass MBH ≃ 0.9M (where M is the mass of the initial star) and dimensionless spin parameter aBH/MBH ≃ 0.7. A massive, hot, magnetized torus surrounds the remnant black hole. At Δt ~ 400-550M ≈ 2000 - 2700(M/106M⊙)s following the gravitational wave peak amplitude, an incipient jet is launched. The disk lifetime is Δt ~ 105(M/106M⊙)s, and the outgoing Poynting luminosity is LEM ~ 1051-52 ergs/s. If > ˜ 1 % - 10 % of this power is converted into gamma rays, Swift and Fermi could potentially detect these events out to large redshifts z ~ 20. Thus, SMSs could be sources of ultra-long gamma-ray bursts (ULGRBs), and massive Population III stars could be the progenitors that power a fraction of the long GRBs observed at redshift z ~ 5-8. Gravitational waves are copiously emitted during the collapse and peak at ~15(106M⊙/M) mHz [~0.15(104 M⊙/M) Hz], i.e., in the LISA (DECIGO/BBO) band; optimally oriented SMSs could be detectable by LISA (DECIGO/BBO) at z < ˜ 3 ( z < ˜ 11 ) .Hence, 104M⊙ SMSs collapsing at z ~ 10 are promising multimessenger sources of coincident gravitational and electromagnetic waves.
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Affiliation(s)
- Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | | | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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Punsly B, Balsara D, Kim J, Garain S. Riemann solvers and Alfven waves in black hole magnetospheres. COMPUTATIONAL ASTROPHYSICS AND COSMOLOGY 2016; 3:5. [PMID: 31149560 PMCID: PMC6511996 DOI: 10.1186/s40668-016-0018-1] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 04/23/2016] [Accepted: 08/17/2016] [Indexed: 11/29/2022]
Abstract
In the magnetosphere of a rotating black hole, an inner Alfven critical surface (IACS) must be crossed by inflowing plasma. Inside the IACS, Alfven waves are inward directed toward the black hole. The majority of the proper volume of the active region of spacetime (the ergosphere) is inside of the IACS. The charge and the totally transverse momentum flux (the momentum flux transverse to both the wave normal and the unperturbed magnetic field) are both determined exclusively by the Alfven polarization. Thus, it is important for numerical simulations of black hole magnetospheres to minimize the dissipation of Alfven waves. Elements of the dissipated wave emerge in adjacent cells regardless of the IACS, there is no mechanism to prevent Alfvenic information from crossing outward. Thus, numerical dissipation can affect how simulated magnetospheres attain the substantial Goldreich-Julian charge density associated with the rotating magnetic field. In order to help minimize dissipation of Alfven waves in relativistic numerical simulations we have formulated a one-dimensional Riemann solver, called HLLI, which incorporates the Alfven discontinuity and the contact discontinuity. We have also formulated a multidimensional Riemann solver, called MuSIC, that enables low dissipation propagation of Alfven waves in multiple dimensions. The importance of higher order schemes in lowering the numerical dissipation of Alfven waves is also catalogued.
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Affiliation(s)
- Brian Punsly
- 1415 Granvia Altamira, Palos Verdes Estates, CA 90274 USA
- ICRANet, Piazza della Repubblica 10, Pescara, 65100 Italy
| | - Dinshaw Balsara
- Physics Department, University of Notre Dame du Lac, 225 Nieuwland Science Hall, Notre Dame, IN 46556 USA
| | - Jinho Kim
- Physics Department, University of Notre Dame du Lac, 225 Nieuwland Science Hall, Notre Dame, IN 46556 USA
| | - Sudip Garain
- Physics Department, University of Notre Dame du Lac, 225 Nieuwland Science Hall, Notre Dame, IN 46556 USA
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HIGH-SENSITIVITY 86 GHz (3.5 mm) VLBI OBSERVATIONS OF M87: DEEP IMAGING OF THE JET BASE AT A RESOLUTION OF 10 SCHWARZSCHILD RADII. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/817/2/131] [Citation(s) in RCA: 110] [Impact Index Per Article: 13.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Martí JM, Müller E. Grid-based Methods in Relativistic Hydrodynamics and Magnetohydrodynamics. ACTA ACUST UNITED AC 2015; 1:3. [PMID: 30652121 PMCID: PMC6319500 DOI: 10.1007/lrca-2015-3] [Citation(s) in RCA: 52] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Accepted: 12/01/2015] [Indexed: 12/01/2022]
Abstract
An overview of grid-based numerical methods used in relativistic hydrodynamics (RHD) and magnetohydrodynamics (RMHD) is presented. Special emphasis is put on a comprehensive review of the application of high-resolution shock-capturing methods. Results of a set of demanding test bench simulations obtained with different numerical methods are compared in an attempt to assess the present capabilities and limits of the various numerical strategies. Applications to three astrophysical phenomena are briefly discussed to motivate the need for and to demonstrate the success of RHD and RMHD simulations in their understanding. The review further provides FORTRAN programs to compute the exact solution of the Riemann problem in RMHD, and to simulate 1D RMHD flows in Cartesian coordinates.
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Affiliation(s)
- José María Martí
- 1Departamento de Astronomía y Astrofísica, Universidad de Valencia, 46100 Burjassot, Valencia, Spain.,2Observatori Astronòmic, Universidad de Valencia, 46980 Burjassot, Valencia, Spain
| | - Ewald Müller
- 3Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
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Pan Z, Yu C. Fourth-order split monopole perturbation solutions to the Blandford-Znajek mechanism. Int J Clin Exp Med 2015. [DOI: 10.1103/physrevd.91.064067] [Citation(s) in RCA: 18] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Tchekhovskoy A. Launching of Active Galactic Nuclei Jets. THE FORMATION AND DISRUPTION OF BLACK HOLE JETS 2015. [DOI: 10.1007/978-3-319-10356-3_3] [Citation(s) in RCA: 39] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/21/2023]
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Lasota JP, Gourgoulhon E, Abramowicz M, Tchekhovskoy A, Narayan R. Extracting black-hole rotational energy: The generalized Penrose process. Int J Clin Exp Med 2014. [DOI: 10.1103/physrevd.89.024041] [Citation(s) in RCA: 52] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Carrasco-González C, Rodríguez LF, Anglada G, Martí J, Torrelles JM, Osorio M. Discovery of synchrotron emission from a YSO jet. EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136103003] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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22
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Meier DL. The Phoenix Fire Model for Jet Creation: The Role of Magnetic Fields in the Production and Propagation of Relativistic Jets. EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136101001] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Gehrels N, Cannizzo JK. High-energy transients. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2013; 371:20120270. [PMID: 23630376 DOI: 10.1098/rsta.2012.0270] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
We present an overview of high-energy transients in astrophysics, highlighting important advances over the past 50 years. We begin with early discoveries of γ-ray transients, and then delve into physical details associated with a variety of phenomena. We discuss some of the unexpected transients found by Fermi and Swift, many of which are not easily classifiable or in some way challenge conventional wisdom. These objects are important insofar as they underscore the necessity of future, more detailed studies.
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Affiliation(s)
- Neil Gehrels
- Astroparticle Physics Division, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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Abramowicz MA, Fragile PC. Foundations of Black Hole Accretion Disk Theory. LIVING REVIEWS IN RELATIVITY 2013; 16:1. [PMID: 28179840 PMCID: PMC5256006 DOI: 10.12942/lrr-2013-1] [Citation(s) in RCA: 25] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 11/15/2012] [Indexed: 05/27/2023]
Abstract
This review covers the main aspects of black hole accretion disk theory. We begin with the view that one of the main goals of the theory is to better understand the nature of black holes themselves. In this light we discuss how accretion disks might reveal some of the unique signatures of strong gravity: the event horizon, the innermost stable circular orbit, and the ergosphere. We then review, from a first-principles perspective, the physical processes at play in accretion disks. This leads us to the four primary accretion disk models that we review: Polish doughnuts (thick disks), Shakura-Sunyaev (thin) disks, slim disks, and advection-dominated accretion flows (ADAFs). After presenting the models we discuss issues of stability, oscillations, and jets. Following our review of the analytic work, we take a parallel approach in reviewing numerical studies of black hole accretion disks. We finish with a few select applications that highlight particular astrophysical applications: measurements of black hole mass and spin, black hole vs. neutron star accretion disks, black hole accretion disk spectral states, and quasi-periodic oscillations (QPOs).
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Affiliation(s)
- Marek A. Abramowicz
- Physics Department, Göteborg University, SE-412-96 Göteborg, Sweden
- N. Copernicus Astronomical Center, Bartycka 18, PL-00-716 Warszawa, Poland
| | - P. Chris Fragile
- Department of Physics & Astronomy, College of Charleston, Charleston, SC 29424 USA
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McKinney JC, Tchekhovskoy A, Blandford RD. Alignment of magnetized accretion disks and relativistic jets with spinning black holes. Science 2013; 339:49-52. [PMID: 23160958 DOI: 10.1126/science.1230811] [Citation(s) in RCA: 129] [Impact Index Per Article: 11.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Accreting black holes (BHs) produce intense radiation and powerful relativistic jets, which are affected by the BH's spin magnitude and direction. Although thin disks might align with the BH spin axis via the Bardeen-Petterson effect, this does not apply to jet systems with thick disks. We used fully three-dimensional general relativistic magnetohydrodynamical simulations to study accreting BHs with various spin vectors and disk thicknesses and with magnetic flux reaching saturation. Our simulations reveal a "magneto-spin alignment" mechanism that causes magnetized disks and jets to align with the BH spin near BHs and to reorient with the outer disk farther away. This mechanism has implications for the evolution of BH mass and spin, BH feedback on host galaxies, and resolved BH images for the accreting BHs in SgrA* and M87.
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Affiliation(s)
- Jonathan C McKinney
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94309, USA.
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Mizuno Y, Lyubarsky Y, Hardee PE, Nishikawa KI. Current-Driven Kink Instability in Magnetically Dominated Rotating Relativistic Jet. EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136102004] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Ferreira J, Petrucci PO, Garnier Q. Is the disc thermal state controlling the Blandford & Znajek/Blandford & Payne jet dichotomy? EPJ WEB OF CONFERENCES 2013. [DOI: 10.1051/epjconf/20136101005] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Shcherbakov R, Pe’er A, Reynolds C, Haas R, Bode T, Laguna P. Prompt emission from tidal disruptions of white dwarfs by intermediate mass black holes. EPJ WEB OF CONFERENCES 2012. [DOI: 10.1051/epjconf/20123902007] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Doeleman SS, Fish VL, Schenck DE, Beaudoin C, Blundell R, Bower GC, Broderick AE, Chamberlin R, Freund R, Friberg P, Gurwell MA, Ho PTP, Honma M, Inoue M, Krichbaum TP, Lamb J, Loeb A, Lonsdale C, Marrone DP, Moran JM, Oyama T, Plambeck R, Primiani RA, Rogers AEE, Smythe DL, SooHoo J, Strittmatter P, Tilanus RPJ, Titus M, Weintroub J, Wright M, Young KH, Ziurys LM. Jet-Launching Structure Resolved Near the Supermassive Black Hole in M87. Science 2012; 338:355-8. [DOI: 10.1126/science.1224768] [Citation(s) in RCA: 314] [Impact Index Per Article: 26.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Sheperd S. Doeleman
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Vincent L. Fish
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - David E. Schenck
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | | | - Ray Blundell
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Geoffrey C. Bower
- Department of Astronomy, University of California Berkeley, Hearst Field Annex, Berkeley, CA 94720, USA
| | - Avery E. Broderick
- Perimeter Institute, 31 Caroline Street, North Waterloo, Ontario N2L 2Y5, Canada
- Department of Physics and Astronomy, University of Waterloo, 200 University Avenue West, Waterloo, Ontario N2l 3G1, Canada
| | - Richard Chamberlin
- Caltech Submillimeter Observatory, 111 Nowelo Street, Hilo, HI 96720, USA
| | - Robert Freund
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | - Per Friberg
- James Clerk Maxwell Telescope, Joint Astronomy Centre, 660 North A'ohoku Place University Park, Hilo, HI 96720, USA
| | - Mark A. Gurwell
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Paul T. P. Ho
- Academia Sinica Institute for Astronomy and Astrophysics, 11F Astronomy-Mathematics Building, National Taiwan University, No. 1, Roosevelt Road, Section 4 Taipei 10617, Taiwan, R.O.C
| | - Mareki Honma
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
- The Graduate University for Advanced Studies, Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Makoto Inoue
- Academia Sinica Institute for Astronomy and Astrophysics, 11F Astronomy-Mathematics Building, National Taiwan University, No. 1, Roosevelt Road, Section 4 Taipei 10617, Taiwan, R.O.C
| | - Thomas P. Krichbaum
- Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
| | - James Lamb
- Owens Valley Radio Observatory, California Institute of Technology, 100 Leighton Lane, Big Pine, CA 93513–0968, USA
| | - Abraham Loeb
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Colin Lonsdale
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - Daniel P. Marrone
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | - James M. Moran
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Tomoaki Oyama
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Richard Plambeck
- Department of Astronomy, University of California Berkeley, Hearst Field Annex, Berkeley, CA 94720, USA
| | - Rurik A. Primiani
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | | | | | - Jason SooHoo
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - Peter Strittmatter
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
| | - Remo P. J. Tilanus
- James Clerk Maxwell Telescope, Joint Astronomy Centre, 660 North A'ohoku Place University Park, Hilo, HI 96720, USA
- Netherlands Organisation for Scientific Research, Laan van Nieuw Oost-Indie 300, NL2509 AC The Hague, Netherlands
| | - Michael Titus
- MIT Haystack Observatory, Off Route 40, Westford, MA 01886, USA
| | - Jonathan Weintroub
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Melvyn Wright
- Department of Astronomy, University of California Berkeley, Hearst Field Annex, Berkeley, CA 94720, USA
| | - Ken H. Young
- Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
| | - Lucy M. Ziurys
- Steward Observatory, Arizona Radio Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721–0065, USA
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Tchekhovskoy A, McKinney JC. Prograde and retrograde black holes: whose jet is more powerful? ACTA ACUST UNITED AC 2012. [DOI: 10.1111/j.1745-3933.2012.01256.x] [Citation(s) in RCA: 140] [Impact Index Per Article: 11.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/27/2022]
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Tchekhovskoy A, Narayan R, McKinney JC. Efficient generation of jets from magnetically arrested accretion on a rapidly spinning black hole. ACTA ACUST UNITED AC 2011. [DOI: 10.1111/j.1745-3933.2011.01147.x] [Citation(s) in RCA: 637] [Impact Index Per Article: 49.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/29/2022]
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Ioka K, Ohira Y, Kawanaka N, Mizuta A. Gamma-Ray Burst without Baryonic and Magnetic Load? ACTA ACUST UNITED AC 2011. [DOI: 10.1143/ptp.126.555] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/05/2022]
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Carrasco-González C, Rodríguez LF, Anglada G, Martí J, Torrelles JM, Osorio M. A Magnetized Jet from a Massive Protostar. Science 2010; 330:1209-12. [DOI: 10.1126/science.1195589] [Citation(s) in RCA: 132] [Impact Index Per Article: 9.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Affiliation(s)
- Carlos Carrasco-González
- Instituto Astrofísica Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Camino Bajo de Huétor 50, E-18008 Granada, Spain
- Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México (UNAM), Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico
| | - Luis F. Rodríguez
- Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México (UNAM), Apartado Postal 3-72 (Xangari), 58089 Morelia, Michoacán, Mexico
| | - Guillem Anglada
- Instituto Astrofísica Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Camino Bajo de Huétor 50, E-18008 Granada, Spain
| | - Josep Martí
- Departamento de Física, Escuela Politécnica Superior de Jaén (EPSJ), Universidad de Jaén, Campus Las Lagunillas s/n, Edif. A3, 23071 Jaén, Spain
| | - José M. Torrelles
- Instituto de Ciencias del Espacio (CSIC/IEEC)-UB, Universitat de Barcelona, Martí i Franquès 1, E-08028 Barcelona, Spain
| | - Mayra Osorio
- Instituto Astrofísica Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Camino Bajo de Huétor 50, E-18008 Granada, Spain
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