'Solar neutrino problem' diaporamas de présentation

Neutrinos and the stars

Neutrinos and the stars. Neutrinos and the Stars. Georg Raffelt, MPI for Physics Lectures at the Topical Seminar Neutrino Physics & Astrophysics 17 - 21 Sept 2008, Beijing, China. Where do Neutrinos Appear in Nature?. Nuclear Reactors. ?. Sun. ?. Supernovae (Stellar Collapse).

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Chapter 14

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Chapter 10 Our Star

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THE SUN

THE SUN. Our source for light, heat and (nearly all) energy on the earth. The Sun: Our Prototype Star. We know much more about it than any other star We describe all other stars in terms of it So you MUST memorize its key properties. Solar Properties.

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Neutrino Physics

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Visible Image of the Sun

The Sun. Visible Image of the Sun. Our sole source of light and heat in the solar system A very common star: a glowing ball of gas held together by its own gravity and powered by nuclear fusion at its center.

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Clicker Question:

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Science

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Chapter 9 The Main Sequence

Chapter 9 The Main Sequence. Four fundamental forces of nature. Hydrostatic equilibrium: negative feedback loop. If core T drops, fusion rate drops, core contracts heats up. If core heats up, fusion rate rises core expands cools down.

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Neutrinos and the Universe

Neutrinos and the Universe. Susan Cartwright University of Sheffield. Neutrinos and the Universe. Discovering neutrinos Detecting neutrinos Neutrinos and the Sun Neutrinos and Supernovae Neutrinos and Dark Matter Neutrinos and the Universe. Discovering neutrinos. Neutrinos have

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Evidence of Neutrino Oscillation from SNO

Evidence of Neutrino Oscillation from SNO. Chun Shing Jason Pun Department of Physics The University of Hong Kong Presented at the HKU Neutrino Workshop 28 November, 2003. Outline. The Solar Neutrino Problem (Brief) Descriptions of SNO Results from SNO Future (and present) plans for SNO

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Solar Magnetism

Solar Magnetism. Differential Rotation, Sunspots, Solar Cycle Guest lecture: Dr. Jeffrey Morgenthaler Jan 30, 2006. Neutrino Summary. Principle of CONSERVATION OF ENERGY led to proposal of neutrino by Wolfgang Pauli

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Neutrino emission

Neutrino emission. <E>=0.27 MeV. E=0.39,0.86 MeV. <E>=6.74 MeV. ppIII loss: 28%. ppII loss: 4%. ppI loss: ~2%. note: <E>/Q= 0.27/26.73 = 1%. Total loss: 2.3%. 2 neutrino energies from 7Be electron capture ?. 7 Be + e - ? 7 Li + n e. E n. E n. Continuous fluxes in /cm 2 /s/MeV

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Ab initio calculations of radiative capture

Ab initio calculations of radiative capture. CAWONAPS 2010, December 9-10, 2010. Petr Navratil | TRIUMF. Understanding our Sun. Light nuclei from first principles. Goal : Predictive theory of structure and reactions of light nuclei Needed for

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Neutrino Oscillations:

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Neutrino Oscillations: the NOMAD experiment

Neutrinos @ CERN. 1993-1998. Neutrino Oscillations: the NOMAD experiment.

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