'Matter density' diaporamas de présentation

Starry Monday at Otterbein

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Dark Matter: Evidenze, Candidati, Esperimenti

Dark Matter: Evidenze, Candidati, Esperimenti. Gianpiero Mangano INFN, Sezione di Napoli Italy. Summary. A short tour of cosmology Observational evidences: baryons vs matter Relic abundance: baryogenesis vs freezing Candidates Experiments. A basic list of References.

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Neutrino quantum states and spin light in matter

Neutrino quantum states and spin light in matter. Neutrino quantum states and spin light in matter. Neutrino motion and radiation in matter. Alexander Studenikin. Moscow State University. 08/03/2005 Turin. References. A.Studenikin, A.Ternov, Phys.Lett . B 608 (2005) 107.

754 views • 48 slides

Cosmology and Relic Neutrinos

Cosmology and Relic Neutrinos. Expanding Universe Big Bang Nucleosynthesis Cosmic Microwave Background measurements Relic neutrinos Informations about neutrino mass Leptogenesis. Galaxies. Antennae galaxies. Andromeda galaxy. Galaxy Evolution Explorer.

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Measuring Earth Matter Density and Testing MSW

Measuring Earth Matter Density and Testing MSW. Hisakazu Minakata Tokyo Metropolitan University. n a =U a i n i. Exploring the unknowns; 1-3 sector and ? mass hierarchy. Atm + accel n =>. <= solar + reactor n. SK atm. solar+KamLAND. Invitation to the question I want to address.

502 views • 40 slides

Leptons, Photons & the CMB

Leptons, Photons & the CMB. Ned Wright, UCLA 16 Aug 2007. Nobel Prize in Physics 2006. John Mather for the CMB Spectrum George Smoot for the CMB anisotropy. COBE View of the CMB Sky. Two Fluids in the Early Universe. Most of the mass is dark matter 80-90% of the density Zero pressure

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Observational Probes of Dark Energy

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Leptons, Photons & the CMB

Leptons, Photons & the CMB. Ned Wright, UCLA 16 Aug 2007. Nobel Prize in Physics 2006. John Mather for the CMB Spectrum George Smoot for the CMB anisotropy. COBE View of the CMB Sky. Two Fluids in the Early Universe. Most of the mass is dark matter 80-90% of the density Zero pressure

487 views • 38 slides

Basics of the Cosmic Microwave Background

Basics of the Cosmic Microwave Background. Eiichiro Komatsu (UT Austin) Lecture at Max Planck Institute August 14, 2007. Night Sky in Optical (~0.5nm). Night Sky in Microwave (~1mm). A. Penzias & R. Wilson, 1965. 3.5K. NOW. R. Dicke and J. Peebles, 1965. P. Roll and D. Wilkinson, 1966.

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Local Rate of Short Hard Gamma-ray Bursts & Life time of SHB Progenitors

Local Rate of Short Hard Gamma-ray Bursts & Life time of SHB Progenitors. Soomin Jeong Chang-Hwan Lee Pusan National University, Korea. Contents. GRB & SHB Motivation Model in calculation Results Conclusions. What is Gamma Ray burst?(1).

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Dr Martin Hendry University of Glasgow

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Scientific Visualization Case Studies

Scientific Visualization Case Studies. Amit Chourasia Visualization Scientist San Diego Supercomputer Center Presented at : Scientific Computing Institute, Univ. of Utah. Jun 20, 2007. Large? Data?. What kind of data?

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Physics with a very long neutrino factory baseline

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The Role of Neutrinos in Galaxy Formation

The Role of Neutrinos in Galaxy Formation. Katherine Cook and Natalie Johnson. http://zebu.uoregon.edu/1999/ph123/lec08.html. http://astro.ph.unimelb.edu.au/~mdrinkwa/lectures/pgc_astro98/galaxy_form/part01. html. Mommy, Where Do Galaxies Come From?. 1-2. 3. 4-7. 8.

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Visible universe is an infinitesimal fraction of the material from the big bang

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Incompressible df/dt=0

Incompressible df/dt=0 N star identical particles moving in a small bundle in phase space (Vol= ? x ? p ), phase space deforms but maintains its area. Likewise for y-p y and z-p z . Phase space density f=Nstars/ ? x ? p ~ const. p x. p x. x. x. Stars flow in phase-space.

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Incompressible df/dt=0 N star identical particles moving in a small bundle in phase space (Vol= ? x ? p ),

Incompressible df/dt=0 N star identical particles moving in a small bundle in phase space (Vol= ? x ? p ), phase space deforms but maintains its area. Likewise for y-p y and z-p z . Phase space density f=Nstars/ ? x ? p ~ const . p x. p x. x. x.

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Cosmology

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How are physical and chemical properties different?

S8P1d. Distinguish between physical and chemical properties of matter as physical (i.e., density, melting point, boiling point) or chemical (i.e., reactivity, combustibility). How are physical and chemical properties different?. Properties of Matter.

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Magnetic Field: A Biased Tracer Element in Deciding Cosmological Bias

In this universe 90% of the matter is dark matter which is not visible and 10% of the matter is baryonic matter which is visible. Baryonic matter includes all the galaxies that we see today. But the evolution of large scale structure includes the underlying dark matter. Dark matter is only affected by gravitational field whereas the baryonic matter is affected by gravitational field as well as radiation pressure, magnetic field etc. This difference leads to the study of bias factor called as cosmological bias. The field of research is open for the study of cosmological properties which is possible by the study of cosmological bias. It is the ratio of baryonic matter density to the dark matter density.

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