A Universe of Disks, from Planets, to Stars, to Black...
Transcript of A Universe of Disks, from Planets, to Stars, to Black...
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News from the NBIA - Niels Bohr Institute - November 22, 2012
Dr. Martin Pessah
A Universe of Disks, from Planets, to Stars, to Black Holes...
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I. Basics of Disk Physics
IV. Numerical Simulations
II. Types of Disks in the Universe
III. Observational Evidence
Plan for the Talk
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I. Basics of Disk Physics
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What is a Disk?
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Astrophysical Disks
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Angular Momentum Conservation
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Why Do Disks Form?
* To a first approximation the gas is falling into a central potential
* Angular momentum is mostly conserved
* Gas can cool down faster than it can get rid of angular momentum
* Flattened, rotating structure (also known as disk!) forms...
Imagine a cloud of gas collapsing due to its own gravity
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R
Astrophysical disks rotate differentially
Particles in a central potential move in stable Keplerian orbits(like planets in solar system!)
Basic Disk Dynamics
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Why Do We Study These Disks?
- How stars and planets form?- What powers the brightest X-ray sources in the sky?- Why Active Galactic Nuclei (Quasars) shine?- How does space-time behave close to a black hole?
Release of gravitational energy in accretion disks responsible for some of the most powerful phenomena in nature!
Proto-star X-ray Binary Active Galactic Nucleus
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II. Types of Disks in the Universe
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Saturn’s Rings
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Saturn’s Rings
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Protoplanetary Disks
Atlas featuring 30 proplyds, or protoplanetary discs, recently discovered in the Orion Nebula with the Hubble Space Telescope. CREDIT: NASA/ESA and L. Ricci (ESO)
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Protoplanetary Disks
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Formation of Protostellar Cores
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Disk Dispersal and Planet Formation
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Accretions Disks in Binary Systems
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Remillard & McClintock, 2006
X-ray Binary Disks
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Disks in Active Galactic Nuclei
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Spiral Galaxies
M51
NGC 4565
Centaurus A
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Disk-like Galaxies
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Disk-like Galaxies
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Typical Masses, Sizes, and Luminosities
1 AU = Sun-Earth distance 1 pc = 206365 AU
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III. Observational Evidence
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Basics of Light
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The Perfect Emitter
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Spectral Lines
Line profiles encode a lot of physical information!
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Doppler Effect
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Evidence for Disks. I.
Time
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Evidence for Disks. II.
From ‘Accretion Power in Astrophysics’; Frank, King, & Raine, 1995
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Evidence for Disks. III.
From ‘Accretion Power in Astrophysics’; Frank, King, & Raine, 1995
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Evidence for Disks. IV.
From ‘Accretion Power in Astrophysics’; Frank, King, & Raine, 1995
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Relativistic Iron Lines
Broad iron lines in AGN (Fabian et al.)Sensitive to ‘inner edge’
Sensitive to inclination
Detailed modeling of lineprofile allows us to ‘map’
the space-time aroundblack holes
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IV. Numerical Simulations
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Why Are Accretion Disk so Hard to Understand?
Magnetic fields do not seem to influence stellar structure significantly
Gravity balanced bypressure gradient along REnergy flows along R too!
R
Magnetic fields are essential for accretion
disks to work
Rφz
MassMomentumEnergy
Non-thermal processesMostly thermal energy
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Turbulent Magnetized Accretion Disks
From J. Hawley’s websiteFrom J. Stone’s website
We need to understand the dynamics of magnetic fields in differentially rotating plasmas!!!
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Supercomputers
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Global 3D MHD Simulations
Beckwith et al. 2011
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Global 3D MHD Simulations
Beckwith et al. 2011
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Magnetized Accretion onto a Black Hole
Kato et al. 2011
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Magnetized Accretion onto a Black Hole
Tchekhovskoy et al. 2011
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Global 3D MHD Simulations
Flock et al. 2012
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Magnetized Accretion onto a Black Hole
Flock et al. 2012
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Planet-Disk Interactions
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