Anthony Mezzacappa Department of Physics and Astronomy University - - PowerPoint PPT Presentation

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Anthony Mezzacappa Department of Physics and Astronomy University - - PowerPoint PPT Presentation

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Anthony Mezzacappa Department of Physics and Astronomy University of Tennessee Joint Institute for Computational Sciences Oak Ridge National Laboratory Saturday Morning Physics University of Tennessee 3/9/2017 1 Universe Evolution of the

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Anthony Mezzacappa Department of Physics and Astronomy University of Tennessee Joint Institute for Computational Sciences Oak Ridge National Laboratory Saturday Morning Physics University of Tennessee

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Understanding our universe and

  • ur place in it will require an

understanding of phenomena on all scales.

Universe Evolution of the Universe as a whole. Large-Scale Structure Filaments of clusters and “superclusters” of galaxies. Galaxies Formation and evolution

  • f individual galaxies.

Stars and Planets Formation and evolution

  • f stars and solar systems.

Stellar Death: Supernovae Compact Objects Formation and evolution

  • f neutron stars and black holes.
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How did galaxies and clusters and superclusters form?

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Number of Zeros Name 1024 Septillion 1021 Sextillion 1018 Quintillion 1015 Quadrillion 1012 Trillion 109 Billion 106 Million 103 Thousand 6 x 1023 Mole (600 Sextillion)

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  • How many galaxies are there in the

Universe?

  • 100 Billion – 1000 Billion (1 Trillion)
  • How many stars are there in the Universe?
  • 10 Sextillion – 1000 Sextillion (1 Septillion)!
  • About 1/10 Mole 
  • How many water molecules are there in a

drop of water?

  • 1 Sextillion
  • 1/100 Mole

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There is a maximum mass for white dwarf stars known as the Chandrasekhar Mass. If a (C-O) white dwarf is near another star, matter from the other star is gravitationally attracted to the white dwarf, and the Chandrasekhar Mass is exceeded. The white dwarf collapses, which initiates a thermonuclear runaway and generates a thermonuclear supernova. The other kind of supernova, a core collapse supernova, is what we will discuss today.

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Speed of Light

  • 671,000,000 miles per hour.
  • Around the Earth
  • 0.1 seconds
  • From Earth to the Moon
  • 1.3 seconds
  • From Earth to the Sun
  • 8.3 minutes
  • From Earth to Proxima Centauri (the closest star to our

Sun)

  • 4.2 years

1 Light Year is about 6,000,000,000,000 miles!

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SN185: First supernova recorded by humankind, recorded by Chinese astronomers. SN1006: Brightest supernova ever recorded, recorded by Chinese. (~7200 ly) SN1054: Crab Supernova (~6500 ly) SN1572: Tycho’s Supernova (~7500 ly) SN1604: Kepler’s Supernova (~20,000 ly) Last supernova in Milky Way seen with naked eye. 1006: Thermonuclear 1054: Core Collapse 1572: Thermonuclear 1604: Thermonuclear Changed humankind’s view of the Universe!

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Supernovae shine as brightly as their host galaxies.

First, and only, time we’ve seen the neutrinos from such an event.

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10 Light Years Constellation: Cassiopeia Distance: 11,000 ly Chandra (X-Ray) 18,000,000 0F Chandra (X-Ray) Spitzer (IR) 50 0F Hubble (Optical) 18,000 0F Shell expanding at 10 million MPH.

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< 700 ly < 900 ly

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Red ochre—Fe2O3—is a simple compound of iron and oxygen that absorbs yellow, green, and blue light and appears red. It’s what makes red paint red.

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Core Collapse Supernova Paradigm and Problem Description

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Transition from nuclei to nuclear matter

  • ccurs through a “pasta” phase.

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Leading Roles  Gravity  Neutrinos  Convection  Standing Accretion Shock Instability (SASI) Supporting Roles  Nuclear Burning  Rotation  Magnetic Fields the most fundamental question in supernova theory

How is the supernova shock w ave revived?

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Unshocked Cold Core Shocked Hot Mantle

Neutrinospheres 44 key weak interactions 8 key weak interactions

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Photons (Light) Neutrinos Gravitational Waves

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Infinite Number of Points Finite Number of Points

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Initial State of the Star Computer Code New State of the Star Repeat

We need to solve the equations of physics to get the new state of the star given the old state of the star.

Laws of Physics

We represent the equations of physics as algebraic equations.

Algebraic Equations

We solve these algebraic equations to get the new state of the star.

Computer Code

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Photons (Light) Neutrinos Gravitational Waves

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Gravity is the result of curved space!

  • Orbits result from spatial curvature.

(In the case of the Sun-Earth or Earth-Moon systems, it’s the curvature of space-time that matters.) Space is physical! It’s a fabric! And you can have waves propagating across it!

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Laser Interferometer Gravitational Wave Observatory (LIGO) LIGO Hanford LIGO Livingston

Sources: Core Collapse Supernovae, Neutron-Star Mergers, Black Hole Mergers Gravitational waves are quadrupolar. Test masses will move less than the diameter of a proton!

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Knowledge of Our Cosmic Origins

Experiment and Observation Computation Theory

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“Per aspera ad astra.” Lucius Annaeus Seneca Roman Philosopher, Statesman, Dramatist 4 BC – 65 AD