'Big bang nucleosynthesis' presentation slideshows

Questions

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Gravitino Production from Heavy Scalar Decay

Gravitino Production from Heavy Scalar Decay. M. Yamaguchi (Tohoku Univ.) with T. Asaka & S. Nakamura April 21, 2006 @ SNU, Korea Refs. Nakamura & MY, hep-ph/0602081 Asaka, Nakamura & MY, hep-ph/0604132 See also:

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The Beginning of Time:

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Your Cosmic Connection to the Elements

Your Cosmic Connection to the Elements. James Lochner (USRA) & Suzanne Pleau Kinnison (AESP), NASA/GSFC. Elementary Connections. The Big Bang. The Big Bang Cosmology. The expansion of the universe began at a finite time in the past, in a state of enormous density, pressure and temperature.

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The Inflationary Universe

The Inflationary Universe . Wednesday, November 26. The universe is very lumpy today because it was slightly inhomogeneous when the universe became transparent. But why was it slightly inhomogeneous then instead of being perfectly smooth?.

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Where do we come from? What are we? Where are we going?

Where do we come from? What are we? Where are we going? . Friday, December 5. If you would like an estimate of your letter grade going into the final exam, send an email to ryden@astronomy.ohio-state.edu.

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Announcements

Announcements.

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The Cosmological Energy Density of Neutrinos from Oscillation Measurements

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SCALES: TIME

SCALES: TIME. COSMIC HISTORY. t = 0 : The Big Bang. The moment in time when the universe started expanding from its initial extremely dense state. How do we know that this happened?. Universe was denser in the past; extrapolating back to infinite density , that was a finite time ago.

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Basic Research Directions Workshop on User Science at the National Ignition Facility

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Primordial Nucleosynthesis (K&T chapter 4)

Primordial Nucleosynthesis (K&T chapter 4). Kinetic eqm, nuclear species A(Z) with mass A and charge Z:. Chemical eqm:. Binding energy:. Mass fraction:. N => all nucleons. Eqm result:. Binding energies of some light nuclei. Phase 1: Nuclear statistical eqm in the early universe.

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Primordial Nucleosynthesis (K&T chapter 4)

Primordial Nucleosynthesis (K&T chapter 4). Kinetic eqm, nuclear species A(Z) with mass A and charge Z:. Chemical eqm:. Binding energy:. Mass fraction:. N => all nucleons. Eqm result:. Binding energies of some light nuclei. Phase 1: Nuclear statistical eqm in the early universe.

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Major Epochs in the Early Universe

Major Epochs in the Early Universe. t<3x10 5 years : Universe radiation dominated t>3x10 5 years : Universe matter dominated Why? Let R be the scale length of the Universe (the separation between your favorite pair of galaxies, say).

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