59 Magnetorotational PPTs View free & download

The Magnetorotational Instability PowerPoint PPT Presentation

The Magnetorotational Instability - The Magnetorotational Instability. 16 October 2004. Large Scale Computation in Astrophysics ... Jean-Pierre De Villiers (UVa; U. Calgary) Steven A. Balbus (UVa) ...

The Magnetorotational Instability. 16 October 2004. Large Scale Computation in Astrophysics ... Jean-Pierre De Villiers (UVa; U. Calgary) Steven A. Balbus (UVa) ...

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Magnetorotational instability PowerPoint PPT Presentation

Magnetorotational instability - Full GR-MHD calculations (Hirose et al. 2004) Findings... Turbulence transports angular momentum and allows accretion to proceed ...

Full GR-MHD calculations (Hirose et al. 2004) Findings... Turbulence transports angular momentum and allows accretion to proceed ...

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Dynamo theory and magnetorotational instability PowerPoint PPT Presentation

Dynamo theory and magnetorotational instability - Christensson et al. (2001, PRE 64, 056405) helical vs. nonhelical. 5. Helical decay law: ... M. Christensson, M. Hindmarsh, A. Brandenburg: 2005, AN 326, 393. 7 ...

Christensson et al. (2001, PRE 64, 056405) helical vs. nonhelical. 5. Helical decay law: ... M. Christensson, M. Hindmarsh, A. Brandenburg: 2005, AN 326, 393. 7 ...

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Core-Collapse Supernovae: Magnetorotational Explosions and Jet Formation PowerPoint PPT Presentation

Core-Collapse Supernovae: Magnetorotational Explosions and Jet Formation - Core-Collapse Supernovae: Magnetorotational Explosions and Jet ... MERLIN 5GHz. Fender (1999) X-ray image of. microquasar. XTE J1550-564(center) with two jets. ...

Core-Collapse Supernovae: Magnetorotational Explosions and Jet ... MERLIN 5GHz. Fender (1999) X-ray image of. microquasar. XTE J1550-564(center) with two jets. ...

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Helical MagnetoRotational Instability and Issues in Astrophysical Jets PowerPoint PPT Presentation

Helical MagnetoRotational Instability and Issues in Astrophysical Jets - but jets are already prone to several vigorous instabilities. pinch, kink, Kelvin-Helmholtz, ... Astrophysical jets & outflows' ...

but jets are already prone to several vigorous instabilities. pinch, kink, Kelvin-Helmholtz, ... Astrophysical jets & outflows' ...

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An experimental demonstration of the Magnetorotational Instability PowerPoint PPT Presentation

An experimental demonstration of the Magnetorotational Instability - New scheme for driving end caps scales with rotation speed ... Larger for profiles with larger flow shear and higher speed. Qualitative results from data ...

New scheme for driving end caps scales with rotation speed ... Larger for profiles with larger flow shear and higher speed. Qualitative results from data ...

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Magnetorotational Instability in Protostellar Discs PowerPoint PPT Presentation

Magnetorotational Instability in Protostellar Discs - Convective turbulence (Lin & Papaloizou 1980, Ryu & Goodman 1992, ... Ampere's Law. Ohm's Law. Conservation of momentum. Disc Model. Vertical Stratification ...

Convective turbulence (Lin & Papaloizou 1980, Ryu & Goodman 1992, ... Ampere's Law. Ohm's Law. Conservation of momentum. Disc Model. Vertical Stratification ...

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Magnetorotational instability in the solar core and Ap star envelopes PowerPoint PPT Presentation

Magnetorotational instability in the solar core and Ap star envelopes - decay close-up. Rm = 104. Pm = 1. Ra = 0. Differential-rotation. decay close-up. Resolution at high Reynolds number. t = 1 rotation. t = 4 rotations ...

decay close-up. Rm = 104. Pm = 1. Ra = 0. Differential-rotation. decay close-up. Resolution at high Reynolds number. t = 1 rotation. t = 4 rotations ...

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Which Parts of Protoplanetary Disks are Susceptible to the Magnetorotational Instability PowerPoint PPT Presentation

Which Parts of Protoplanetary Disks are Susceptible to the Magnetorotational Instability - T Tauri disks in Taurus observed to viscously spread with ~ 10-2 [Hartmann et al. ... Steep profile (r) = 343 (r / 10 AU)-2.17 g cm-2 is not consistent with steady ...

T Tauri disks in Taurus observed to viscously spread with ~ 10-2 [Hartmann et al. ... Steep profile (r) = 343 (r / 10 AU)-2.17 g cm-2 is not consistent with steady ...

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Lecture%205.%20Population%20synthesis%20of%20NSs PowerPoint PPT Presentation

Lecture%205.%20Population%20synthesis%20of%20NSs - Lecture 5. Population synthesis of NSs Sergei Popov (SAI MSU) Population synthesis in astrophysics Why PS is necessary? Tasks Two variants Examples Magnetorotational ...

Lecture 5. Population synthesis of NSs Sergei Popov (SAI MSU) Population synthesis in astrophysics Why PS is necessary? Tasks Two variants Examples Magnetorotational ...

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Core-Collapse Supernovae: explosions mechanism and jet formation PowerPoint PPT Presentation

Core-Collapse Supernovae: explosions mechanism and jet formation - Title: Magnetorotational mechanism: 2D Simulations of Supernova Explosions and ejections Author: max Last modified by: GENA Created Date: 2/5/2001 1:31:21 PM

Title: Magnetorotational mechanism: 2D Simulations of Supernova Explosions and ejections Author: max Last modified by: GENA Created Date: 2/5/2001 1:31:21 PM

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Steven A. Balbus PowerPoint PPT Presentation

Steven A. Balbus - Steven A. Balbus. Ecole Normale Sup rieure. Physics Department. Paris, France. IAS MRI Workshop ... The MAGNETOROTATIONAL INSTABILITY (MRI) has taught us that ...

Steven A. Balbus. Ecole Normale Sup rieure. Physics Department. Paris, France. IAS MRI Workshop ... The MAGNETOROTATIONAL INSTABILITY (MRI) has taught us that ...

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Magnetic activity in protoplanetary discs PowerPoint PPT Presentation

Magnetic activity in protoplanetary discs - ... Magnetic diffusion ... on charged particles deeper layers shielded from ionising radiation for r

... Magnetic diffusion ... on charged particles deeper layers shielded from ionising radiation for r

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The birth-ultrafast-magnetic-field-decay model applied to isolated millisecond pulsars PowerPoint PPT Presentation

The birth-ultrafast-magnetic-field-decay model applied to isolated millisecond pulsars - The birth-ultrafast-magnetic-field-decay model applied to isolated millisecond pulsars Ricardo Heras Preparatoria Abierta SEIEM Edo. Mexico

The birth-ultrafast-magnetic-field-decay model applied to isolated millisecond pulsars Ricardo Heras Preparatoria Abierta SEIEM Edo. Mexico

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Pencil Code: progress since August 2006 PowerPoint PPT Presentation

Pencil Code: progress since August 2006 - Antony Mee (Univ. Newcastle) Nils Haugen (NTNU, Trondheim) and many more... Started in Sept. 2001 with Wolfgang Dobler. High order (6th order in space, 3rd ...

Antony Mee (Univ. Newcastle) Nils Haugen (NTNU, Trondheim) and many more... Started in Sept. 2001 with Wolfgang Dobler. High order (6th order in space, 3rd ...

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The Growth of the MRI in Protoplanetary Disks PowerPoint PPT Presentation

The Growth of the MRI in Protoplanetary Disks - Mark Wardle Macquarie University Sydney, Australia Protoplanetary disks Magnetic diffusion MRI with diffusion Ionisation equilibrium Live and Dead zones

Mark Wardle Macquarie University Sydney, Australia Protoplanetary disks Magnetic diffusion MRI with diffusion Ionisation equilibrium Live and Dead zones

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A Heino-Centric View of the History of Galactic Center Theory PowerPoint PPT Presentation

A Heino-Centric View of the History of Galactic Center Theory - A Heino-Centric View of the History of Galactic Center Theory ... Spin, precession and variability of Sgr A*. Linear Polarization images near the event horizon ...

A Heino-Centric View of the History of Galactic Center Theory ... Spin, precession and variability of Sgr A*. Linear Polarization images near the event horizon ...

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Outline: - Momentum Transport D. Craig General Meeting of the Center for Magnetic Self-Organization In Laboratory and Astrophysical Plasmas August 4-6, 2004 in Madison, WI

Momentum Transport D. Craig General Meeting of the Center for Magnetic Self-Organization In Laboratory and Astrophysical Plasmas August 4-6, 2004 in Madison, WI

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Modelling of Astrophysical Plasma Processes in Laboratory Experiments PowerPoint PPT Presentation

Modelling of Astrophysical Plasma Processes in Laboratory Experiments - Magnetic fields are present on planets (Earth) ... map of the region illuminated by Hydra A, the. most luminous AGN in Hydra cluster (Taylor & Perley 1993) 4 ...

Magnetic fields are present on planets (Earth) ... map of the region illuminated by Hydra A, the. most luminous AGN in Hydra cluster (Taylor & Perley 1993) 4 ...

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ANGULAR MOMENTUM TRANSPORT PowerPoint PPT Presentation

ANGULAR MOMENTUM TRANSPORT - SHEARING SHEET. local model of a differentially rotating disc ... entirely absent (ky 0) in the shearing sheet. do not describe parallel shear flow instability ...

SHEARING SHEET. local model of a differentially rotating disc ... entirely absent (ky 0) in the shearing sheet. do not describe parallel shear flow instability ...

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Young Stars I,II PowerPoint PPT Presentation

Young Stars I,II - Title: Star formation - the accretion (luminosity) problem Author: Lee Hartmann Last modified by: Lee Hartmann Created Date: 6/6/1999 2:12:30 PM Document presentation ...

Title: Star formation - the accretion (luminosity) problem Author: Lee Hartmann Last modified by: Lee Hartmann Created Date: 6/6/1999 2:12:30 PM Document presentation ...

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Large scale simulations of astrophysical turbulence PowerPoint PPT Presentation

Large scale simulations of astrophysical turbulence - (Radiation: as a 3-step process) How to manage the contributions of 20 people ... MHD (Haugen), passive scalar (K pyl ), cosmic rays (Snod, Mee) Stratified layers ...

(Radiation: as a 3-step process) How to manage the contributions of 20 people ... MHD (Haugen), passive scalar (K pyl ), cosmic rays (Snod, Mee) Stratified layers ...

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Magneto-hydrodynamic turbulence: from the ISM to discs PowerPoint PPT Presentation

Magneto-hydrodynamic turbulence: from the ISM to discs - High order (6th order in space, 3rd order in time) Cache & memory efficient ... High resolution direct simulation. 5123 resolution. singular! 2563 (direct, new) ...

High order (6th order in space, 3rd order in time) Cache & memory efficient ... High resolution direct simulation. 5123 resolution. singular! 2563 (direct, new) ...

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Numerical simulation of astrophysical jets and accretion disks PowerPoint PPT Presentation

Numerical simulation of astrophysical jets and accretion disks - Understanding the physics of accretion-ejection flows. is central to the understanding of ... Jet acceleration and collimation. Emission from shocks in YSO jets ...

Understanding the physics of accretion-ejection flows. is central to the understanding of ... Jet acceleration and collimation. Emission from shocks in YSO jets ...

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Hideki Maki - We will study about the angular momentum transport in the primordial case. ... Thermal Evolution of Primordial Cloud (Omukai 2000) ...

We will study about the angular momentum transport in the primordial case. ... Thermal Evolution of Primordial Cloud (Omukai 2000) ...

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Hideki Maki - This work was partly supported by the 'Rikkyo University. Special Found ... generation of vorticity. dynamo by rotation of galaxy. within galaxy formation time ...

This work was partly supported by the 'Rikkyo University. Special Found ... generation of vorticity. dynamo by rotation of galaxy. within galaxy formation time ...

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?? - Title: Author: shibata Last modified by: Ryoji Matsumoto Created Date: 9/7/2003 3:09:43 PM

Title: Author: shibata Last modified by: Ryoji Matsumoto Created Date: 9/7/2003 3:09:43 PM

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The Zoo Of Neutron Stars PowerPoint PPT Presentation

The Zoo Of Neutron Stars - Title: 1 Author: polar Last modified by: PKSternberg Created Date: 3/4/2005 6:54:47 AM Document presentation format: On-screen Show Company

Title: 1 Author: polar Last modified by: PKSternberg Created Date: 3/4/2005 6:54:47 AM Document presentation format: On-screen Show Company

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Magnetohydrodynamic turbulence: from the ISM to discs - Magneto-hydrodynamic turbulence: from the ISM to discs. Axel ... Depends on Rm of vortical flow component. Bimodal: Rm=35 (w/o shocks), 70 (w/ shocks) ...

Magneto-hydrodynamic turbulence: from the ISM to discs. Axel ... Depends on Rm of vortical flow component. Bimodal: Rm=35 (w/o shocks), 70 (w/ shocks) ...

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Magnetic fields in protoplanetary discs PowerPoint PPT Presentation

Magnetic fields in protoplanetary discs - Equipartition field in the minimum solar nebula. Evidence for 0.1 1 G fields in the solar nebula at 1AU ... minimum solar nebula. assume isothermal in z-direction ...

Equipartition field in the minimum solar nebula. Evidence for 0.1 1 G fields in the solar nebula at 1AU ... minimum solar nebula. assume isothermal in z-direction ...

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General Relativistic MHD Simulations of Black Hole Accretion Disks PowerPoint PPT Presentation

General Relativistic MHD Simulations of Black Hole Accretion Disks - Julian H. Krolik, Shigenobu Hirose (JHU) Charles F. Gammie (Illinois) ... Hirose, Krolik, De Villiers, & Hawley 2004, ApJ, 606, 1083 ...

Julian H. Krolik, Shigenobu Hirose (JHU) Charles F. Gammie (Illinois) ... Hirose, Krolik, De Villiers, & Hawley 2004, ApJ, 606, 1083 ...

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???~(1-10)?km PowerPoint PPT Presentation

???~(1-10)?km - Title: Author: shibata Last modified by: shibata Created Date: 1/18/2004 10:22:16 AM Document presentation format

Title: Author: shibata Last modified by: shibata Created Date: 1/18/2004 10:22:16 AM Document presentation format

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Observation of magnetocoriolis waves in the Princeton MRI Experiment - Observation of magnetocoriolis waves in the Princeton MRI Experiment

Observation of magnetocoriolis waves in the Princeton MRI Experiment

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Magnetic activity in protoplanetary discs - large for YSO discs, so determines field evolution ... Magnetic diffusion varies quantitatively and qualitatively within the disk ...

large for YSO discs, so determines field evolution ... Magnetic diffusion varies quantitatively and qualitatively within the disk ...

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Space%20Cowboys%20Odissey:%20Beyond%20the%20Gould%20Belt PowerPoint PPT Presentation

Space%20Cowboys%20Odissey:%20Beyond%20the%20Gould%20Belt - Title: Close-by young isolated neutron stars (and black holes) Author: polar Last modified by: sergepolar Created Date: 4/1/2005 6:24:30 AM Document presentation format

Title: Close-by young isolated neutron stars (and black holes) Author: polar Last modified by: sergepolar Created Date: 4/1/2005 6:24:30 AM Document presentation format

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The Physical Origin of Negative Superhumps PowerPoint PPT Presentation

The Physical Origin of Negative Superhumps - Common superhumps shown by Whitehurst and several others to be the result of ... Bonnet-Bidaud, Motch, & Mouchet (1985) first to suggest the 5.2-hr period in TV ...

Common superhumps shown by Whitehurst and several others to be the result of ... Bonnet-Bidaud, Motch, & Mouchet (1985) first to suggest the 5.2-hr period in TV ...

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Electromagnetic Models of Gamma Ray Bursts: A Tutorial PowerPoint PPT Presentation

Electromagnetic Models of Gamma Ray Bursts: A Tutorial - Relativistic accretion disks/tori. More energy may come from the disk than the hole ... Dissipation inevitable if V c/ln(qmax/qmin) ~ 0.1c; otherwise not. cf PWN ...

Relativistic accretion disks/tori. More energy may come from the disk than the hole ... Dissipation inevitable if V c/ln(qmax/qmin) ~ 0.1c; otherwise not. cf PWN ...

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The Growth of the MRI in Protoplanetary Disks - Magnetic diffusion regimes. ions, electrons and neutrals decoupled. ions and electrons decoupled ... distinct diffusion regimes: Ohmic (resistive) Hall ...

Magnetic diffusion regimes. ions, electrons and neutrals decoupled. ions and electrons decoupled ... distinct diffusion regimes: Ohmic (resistive) Hall ...

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Magnetic Fields and Jet Formation PowerPoint PPT Presentation

Magnetic Fields and Jet Formation - Black Hole rotation vertical field: Blandford-Znajek Poynting flux jet ... Black hole accretion process require us to describe the behaviour of matter ...

Black Hole rotation vertical field: Blandford-Znajek Poynting flux jet ... Black hole accretion process require us to describe the behaviour of matter ...

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Stabilization of the Resistive Wall Mode Using Moving Metal Walls - Stabilization of the Resistive Wall Mode Using Moving Metal Walls

Stabilization of the Resistive Wall Mode Using Moving Metal Walls

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??????? - 2005 10 18 40 4 30 5 10

2005 10 18 40 4 30 5 10

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- The interaction of a giant planet with a disc with MHD turbulence II: The interaction of the planet with the disc Papaloizou & Nelson 2003, MNRAS 339 (4), 993

The interaction of a giant planet with a disc with MHD turbulence II: The interaction of the planet with the disc Papaloizou & Nelson 2003, MNRAS 339 (4), 993

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Jets, Disks, and Protostars PowerPoint PPT Presentation

Jets, Disks, and Protostars - Singular isothermal spheres have constant accretion rates ... Differential rotation stabilizes Jeans instability ... Jeans mass drops, hydrost. equil. reached ...

Singular isothermal spheres have constant accretion rates ... Differential rotation stabilizes Jeans instability ... Jeans mass drops, hydrost. equil. reached ...

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Massive Objects at the Centers of Galaxies PowerPoint PPT Presentation

Massive Objects at the Centers of Galaxies - 1961-2 Hoyle, Fowler - radio sources are powered by ... 1964 Zel'dovich & Novikov, Salpeter et al - black holes. 1965 Dent - variability. More history ...

1961-2 Hoyle, Fowler - radio sources are powered by ... 1964 Zel'dovich & Novikov, Salpeter et al - black holes. 1965 Dent - variability. More history ...

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Gamma Rays from Accreting Black Holes PowerPoint PPT Presentation

Gamma Rays from Accreting Black Holes - Gamma Ray Bursts? 1 ix 05. GLAST GC Meeting. 3. Traditional Disks are: ... X. Can you measure the toroidal field pattern? Even Parity. Odd Parity. Mixed Parity ...

Gamma Ray Bursts? 1 ix 05. GLAST GC Meeting. 3. Traditional Disks are: ... X. Can you measure the toroidal field pattern? Even Parity. Odd Parity. Mixed Parity ...

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Recent advances in Astrophysical MHD PowerPoint PPT Presentation

Recent advances in Astrophysical MHD - ... in 2D dissipation rate. after saturation is sensitive to numerical dissipation: Code Test ... Numerical dissipation is ~1.5 times smaller with. CTU & 3rd ...

... in 2D dissipation rate. after saturation is sensitive to numerical dissipation: Code Test ... Numerical dissipation is ~1.5 times smaller with. CTU & 3rd ...

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Growth of Massive Black Holes in Active Galactic Nuclei PowerPoint PPT Presentation

Growth of Massive Black Holes in Active Galactic Nuclei - Growth of Massive Black Holes in Active Galactic Nuclei Roger Blandford KIPAC, Stanford Assumptions and Notation Astrophysical holes depend upon mass and spin Charge ...

Growth of Massive Black Holes in Active Galactic Nuclei Roger Blandford KIPAC, Stanford Assumptions and Notation Astrophysical holes depend upon mass and spin Charge ...

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Star Formation PowerPoint PPT Presentation

Star Formation - How are starbursts, low surface brightness galaxies different? Timescales ... value depends on corrections for dust obscuration, surface-brightness dimming ...

How are starbursts, low surface brightness galaxies different? Timescales ... value depends on corrections for dust obscuration, surface-brightness dimming ...

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Accretion Power in Astrophysics PowerPoint PPT Presentation

Accretion Power in Astrophysics - Accretion Power in Astrophysics Andrew King Theoretical Astrophysics Group, University of Leicester, UK Accreting Black Holes in a Nearby Galaxy (M101) Accreting ...

Accretion Power in Astrophysics Andrew King Theoretical Astrophysics Group, University of Leicester, UK Accreting Black Holes in a Nearby Galaxy (M101) Accreting ...

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The Zoo Of Neutron Stars - Intermediate SGR bursts. Examples of intermediate bursts. ... Unidentified EGRET sources. Grenier (2000), Gehrels et al. (2000) ...

Intermediate SGR bursts. Examples of intermediate bursts. ... Unidentified EGRET sources. Grenier (2000), Gehrels et al. (2000) ...

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Lucio Mayer Zurich, Thomas Quinn University of PowerPoint PPT Presentation

Lucio Mayer Zurich, Thomas Quinn University of - have rotation rates such that Vrot ~ 0.3-2 x Vrot (Jupiter) after. contraction down to the mean ... Snapshots of sims with different. Tcool, all after ~ 10 Torb ...

have rotation rates such that Vrot ~ 0.3-2 x Vrot (Jupiter) after. contraction down to the mean ... Snapshots of sims with different. Tcool, all after ~ 10 Torb ...

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Young Stars I,II - Essentially ALL protostellar cloud magnetic flux must be lost during star ... collimation. Alfven surface. Accretion leads to ejection. dM/dt (wind) = 0.1 dM/dt (acc) ...

Essentially ALL protostellar cloud magnetic flux must be lost during star ... collimation. Alfven surface. Accretion leads to ejection. dM/dt (wind) = 0.1 dM/dt (acc) ...

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CDP Workshop on Magnetic Fields and Structures Magnetic fields on Normal i'e', nondegenerate Stars PowerPoint PPT Presentation

CDP Workshop on Magnetic Fields and Structures Magnetic fields on Normal i'e', nondegenerate Stars - ... for stellar magnetic cycles from the Mt. Wilson Ca II index program (Baliunas et ... Applied to the chemically peculiar star 53 Cam. ...

... for stellar magnetic cycles from the Mt. Wilson Ca II index program (Baliunas et ... Applied to the chemically peculiar star 53 Cam. ...

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NonAxisymmetric Dynamics and Magnetoacoustic Flux in Core Collapse PowerPoint PPT Presentation

NonAxisymmetric Dynamics and Magnetoacoustic Flux in Core Collapse - A Crab-like field of 1012 Gauss and a Crab-like rotation. of 33 ms are dynamically unimportant. ... m = 1 single spiral arm mode. Outward transport of angular ...

A Crab-like field of 1012 Gauss and a Crab-like rotation. of 33 ms are dynamically unimportant. ... m = 1 single spiral arm mode. Outward transport of angular ...

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Simulations of General Relativistic Hydrodynamics PowerPoint PPT Presentation

Simulations of General Relativistic Hydrodynamics - Fluid dynamics in a strong Gravitational field. Astrophysics (mainly for NSs) ... CVS Hydra Whisky_DriftCorrect Whisky_MeudonData Whisky_TOVSolverC ...

Fluid dynamics in a strong Gravitational field. Astrophysics (mainly for NSs) ... CVS Hydra Whisky_DriftCorrect Whisky_MeudonData Whisky_TOVSolverC ...

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The Formation and Longterm Evolution of Circumstellar Disks PowerPoint PPT Presentation

The Formation and Longterm Evolution of Circumstellar Disks - FU Ori. FUor's are YSO's with significant circumstellar material. ... Observed frequency of FU Ori eruptions (last 50 years) is several times greater ...

FU Ori. FUor's are YSO's with significant circumstellar material. ... Observed frequency of FU Ori eruptions (last 50 years) is several times greater ...

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Magnetorotational PowerPoint PPT Presentations