'Cno cycle' diaporamas de présentation

Lecture 9 Hydrogen Burning Nucleosynthesis, Classical Novae, and X-Ray Bursts

Lecture 9 Hydrogen Burning Nucleosynthesis, Classical Novae, and X-Ray Bursts. Once the relevant nuclear physics is known in terms of the necessary rate factors, l = N A < s v>, the composition can be solved from the coupled set of rate equations:.

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The first year of Borexino data

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Nuclear Astrophysics II

Nuclear Astrophysics II. Lecture 2 Thurs. April 26, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437. shawn.bishop@ph.tum.de. The CNO1 Cycle. 1. 2. 3. 4. 5. 6.

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1) Big Bang ( nucleosintesi cosmologica )

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Creation of the Chemical Elements

Creation of the Chemical Elements. By Dr. Harold Williams of Montgomery College Planetarium http://montgomerycollege.edu/Departments/planet/. 17.3 Life as a High-Mass Star. Our goals for learning What are the life stages of a high-mass star?

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The birth of a star Chapter 11

The birth of a star Chapter 11. Questions to be addressed:. Where are the birth places of stars? What are the main components of a protostar? When and how a new is born? What prevents a star from collapsing?. How does a star form?.

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Nuclear Astrophysics

Nuclear Astrophysics. Lecture 10 Thurs. Jan. 12, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437. shawn.bishop@ph.tum.de. Summary of Reaction Rate. Energy Generation & Standard Model.

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Nuclear Astrophysics

Nuclear Astrophysics. Lecture 10 Thurs. Jan. 12, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437. shawn.bishop@ph.tum.de. Summary of Reaction Rate. Energy Generation & Standard Model.

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Philip Salter School of Physics & Astronomy

Philip Salter School of Physics & Astronomy. Time-reversed measurement of the 18 Ne( a ,p) 21 Na cross section relevant to breakout from the Hot-CNO cycle in X-ray bursts. Outline. Overview of X-ray bursts Outline of relevant nuclear processes Experimental investigation

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Prospettive delle attivita' di Astrofisica Nucleare con Recoil Mass Separators

Prospettive delle attivita' di Astrofisica Nucleare con Recoil Mass Separators. Gianluca Imbriani per la collaborazione ERNA. Solar burnings: pp chain. p + p ? 2 H + e + + n p + e - + p ? 2 H + e + + n 2 H + p ? 3 He + g

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Stellar Structure

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LUNA 1 50 kV

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The Sun as a Star

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Ch 11 & 12 : Star Structure

Ch 11 & 12 : Star Structure. What is the interior structure of stars?. (1) Hydrostatic Equilibrium. When a star is stable (neither expanding or contracting) Everywhere within the star : inwards force = outwards force gravity = pressure

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CNO cycle

CNO cycle. CN cycle (99.9%). O Extension 1 (0.1%). O Extension 2. O Extension 3. Ne(10). F(9). O(8). N(7). C(6). 3. 4. 5. 6. 7. 8. 9. neutron number. All initial abundances within a cycle serve as catalysts and accumulate at largest t.

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