Zachary Robinson Phys 406.  What creates the sun’s energy? ◦ Composition of Sun ◦ Fusion in the Sun (and other stars)  Creation of the elements  Studying.

Slides:



Advertisements
Similar presentations
Announcements Star Assignment 3, due Wednesday March 17 –READ chapter 16, –Do Angel quiz, –Do Astronomy Place tutorial “Measuring Cosmic Distances: Lesson.
Advertisements

Double Beta Decay Neodymium, a rare earth element, will be added to the liquid scintillator in SNO+ (at 0.1% by weight). This will enable a search for.
Einstein’s Energy Mass Equivalence Powers the Sun!
Neutrino oscillations/mixing
Recent Discoveries in Neutrino Physics: Understanding Neutrino Oscillations 2-3 neutrino detectors with variable baseline 1500 ft nuclear reactor Determining.
Slide 1 Test 2 results Test 2 average: 77 (test 1: 82) Test 2 median: 79 (test 1: 87)
Neutrino Physics - Lecture 5 Steve Elliott LANL Staff Member UNM Adjunct Professor ,
Prospects for 7 Be Solar Neutrino Detection with KamLAND Stanford University Department of Physics Kazumi Ishii.
7 THE SUN The star we see by day. 7 Goals Summarize the overall properties of the Sun. What are the different parts of the Sun? Where does the light we.
Neutrinos Jason Cook. Topics of Interest Neutrinos  History  Sources  Detection  Solar Neutrino Problem  Neutrino Oscillation  Practicality of Neutrinos.
Solar Neutrinos and the SNO Experiment JJ Anthony April 11, 2006 Astronomy 007.
© 2005 Pearson Education Inc., publishing as Addison-Wesley The Sun: Our Star 29 April 2008.
Neutrino Mass By Ben Heimbigner.
Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%
Chapter three Sun’s model Major contributions in building the Sun’s model have been made by Eddington (1930’s), Hoyle (1950’s),Bahcall, Clayton (1980’s)
If the sun is a burning ball of gas … just what gas is it burning? Warmup Question:
Section 1: Structure of the Sun
The Sun Internal structure of the Sun Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.
Lecture 13. Review: Static Stellar structure equations Hydrostatic equilibrium: Mass conservation: Equation of state: Energy generation: Radiation Convection.
Chapter 29 The Sun 29.1 Structure of the Sun
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2 Solar Interior/ Nuclear Fusion.
THE SUN The star we see by day.
The Sun and other stars. The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and.
Methods and problems in low energy neutrino experiments (solar, reactors, geo-) I G. Ranucci ISAPP 2011 International School on Astroparticle physics THE.
Survey of the Universe Tom Burbine
Section 1: Structure of the Sun
Monday, Feb. 24, 2003PHYS 5326, Spring 2003 Jae Yu 1 PHYS 5326 – Lecture #11 Monday, Feb. 24, 2003 Dr. Jae Yu 1.Brief Review of sin 2  W measurement 2.Neutrino.
Stars Physics Astrophysics. Brightness Different brightness. Different color. How bright are they really? What is due to distance? What is due.
Made by Stanislav Hristov. Why Solar Neutrino?  Examining solar neutrino allows us to find what the physics of the Sun’s core is.  The Sun produces.
Wednesday, Feb. 14, 2007PHYS 5326, Spring 2007 Jae Yu 1 PHYS 5326 – Lecture #6 Wednesday, Feb. 14, 2007 Dr. Jae Yu 1.Neutrino Oscillation Formalism 2.Neutrino.
Neutrino Nobel Prize overview
Lecture 19: The Sun Our Star Some Facts about the Sun  distance from Earth: 1.5 x 10 8 km  luminosity: 3.86 x W  mass: 1.98 x kg (3.33.
SNO and the new SNOLAB SNO: Heavy Water Phase Complete Status of SNOLAB Future experiments at SNOLAB: (Dark Matter, Double beta, Solar, geo-, supernova.
Analysis of Alpha Background in SNO Data Using Wavelet Analysis
Chapter 9 Our Star, the Sun. What do you think? What is the surface of the Sun like? Does the Sun rotate? What makes the Sun shine?
Kamiokande = Kamioka Nucleon Decay Experiment
{ Week 22 Physics.  Understand that a star is in equilibrium under the action of two opposing forces, gravitation and the radiation pressure of the star.
The Heart of the Sun Energy Generation in Sun-like Stars.
J. Goodman – January 03 The Solution to the Solar Problem Jordan A. Goodman University of Maryland January 2003 Solar Neutrinos MSW Oscillations Super-K.
Neutrinos: What we’ve learned and what we still want to find out Jessica Clayton Astronomy Club November 10, 2008.
10.2 Nuclear Fusion in the Sun Our Goals for Learning How does nuclear fusion occur in the Sun? How does the energy from fusion get out of the Sun? How.
Main Sequence Stars Internal structure Nuclear fusion –Protons, neutrons, electrons, neutrinos –Fusion reactions –Lifetime of the Sun Transport of energy.
P Spring 2002 L18Richard Kass The Solar Neutrino Problem M&S Since 1968 R.Davis and collaborators have been measuring the cross section of:
Solar Neutrinos By Wendi Wampler. What are Neutrinos? Neutrinos are chargeless, nearly massless particles Neutrinos are chargeless, nearly massless particles.
The Sun Part 2.
Light, Astronomical Observations, and the Sun. Terms Spectrum –A range of something, e.g. colors Spectra –Plural of spectrum Incandescent –Hot enough.
STELLAR EVOLUTION – THE STANDARD SOLAR MODEL AND SOLAR NEUTRINOS – MARIE ZECH.
Solar Neutrinos Learning about the core of the Sun Guest lecture: Dr. Jeffrey Morgenthaler Jan 26, 2006.
If the sun is a burning ball of gas … just what gas is it burning? Warmup Question:
Solar neutrino physics The core of the Sun reaches temperatures of  15.5 million K. At these temperatures, nuclear fusion can occur which transforms 4.
The Sun 1)H-R diagram 2)Solar Structure 3)Nuclear Fusion 4)Solar Neutrinos 5)Solar Wind/Sunspots October 21, 2002.
Our Star, the Sun Chapter Eighteen. Guiding Questions 1.What is the source of the Sun’s energy? 2.What is the internal structure of the Sun? 3.How can.
THE SUN The star we see by day.
The Sun – Our Star.
HCP: Particle Physics Module, Lecture 4
The Sun The Sun’s Spectrum
Solar Neutrino Problem
THE SUN The star we see by day.
The Sun I.
The Sun Internal structure of the Sun Nuclear fusion
Charles Hakes Fort Lewis College 1.
Pauli´s new particle * nt nm ne e m t Beta-Decay Pa 234 b (electron)
Section 1: Structure of the Sun
Solar neutrinos: form their production to their detection
The Earth and the Sun -Hydrogen (about 70%) is the Sun’s main fuel source -Helium (about 25%) and energy are the main products of fusion from the Sun -there.
7. Internal structure. II.
Q. 65: What Holds the Nucleus Together?
1930: Energy conservation violated in β-decay
Fission & Fusion.
Presentation transcript:

Zachary Robinson Phys 406

 What creates the sun’s energy? ◦ Composition of Sun ◦ Fusion in the Sun (and other stars)  Creation of the elements  Studying the sun with helioseismology ◦ What is it? ◦ How is it used?  Studying the sun through neutrino detection ◦ Solar neutrino problem ◦ SNO

 74% Hydrogen  24% Helium  2% Trace Elements jpg

Hydrogen Recycling: Images from:

Images from:

Positron

 Video from NOVA’s “Origins” mini-series:  er_embedded&v=neMEo8ZrwuI er_embedded&v=neMEo8ZrwuI

 What is it? ◦ Study of the interior of the sun via observations of sound waves on its surface  How does it work? ◦ Sun acts as a spherical resonant cavity for acoustic waves ◦ Oscillations from acoustic waves result in small Doppler shifts of spectrum lines

 How is it used? ◦ By numerically solving solar models we can determine information about the sun  For example: Solar structure, chemical composition, temperature at different depths

 Detecting the proper amount of neutrinos from the sun would verify fusion theories  Solar Neutrino Problem (SNP): ◦ Solar neutrino measurements have yielded inconsistent and perplexing results ◦ Presently the measured flux of neutrinos is significantly less than the expected output from the sun’s fusion reactions!  SAGE and GALLEX detect only 60 to 70% of expected

 The sun’s reaction mechanisms are not correctly understood ◦ This would be a huge blow to models which have otherwise been very successful ◦ No satisfactory modifications have been proposed  Experiments could be performed incorrectly  Reaction rates in the Sun could be lower than calculations predict  Something could happen to the neutrinos in transit to earth…

 Three types of neutrinos: ◦ Electron, muon, tau  The sun should only produce electron neutrinos  Until recently, neutrino detectors could only detect electron neutrinos  MSW effect: Sun’s high mass densities enhance the flavor oscillations of neutrinos conferences.fnal.gov

 Detector that could detect all three flavors  Built 6800 feet underground in Canada  Cherenkov detector using 1000 metric tons of heavy water (D 2 O)  All air, water, and materials in detector are extremely pure to reduce background noise from radioactive elements  Collecting data since

"Fusion Process of the Sun." Grant Chronicles. GrantChronicles.com, Web. 28 Nov Guenther, D.B. "Age of the Sun." Astrophysics Journal (1989): Print. Graps, Amara. "Helioseismology." Stanford.edu. Stanford University, 19 Feb Web. 6 Dec "How the Sun Shines". Nobelprize.org. 30 Nov Stark, P.B.. "Sounding the Sun: Helioseismology." AAAS Seminars. University of California, Apr Web. 3 Dec Strobel, Nick. "Neutrino." The Sun and Stellar Structure. AstronomyNotes.com, 12 Jun Web. 3 Dec "The SNO Homepage." The Sudbury Neutrino Observatory. The SNO Institute, 21 Apr Web. 24 Nov

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2025 SlidePlayer.com. Inc. All rights reserved.