The Standard Solar Model and Experiments Predictions versus experiments Uncertainties in predictions Challenges and open questions BP00: astro-ph/0010346.

Slides:

Advertisements

Similar presentations

Standard Solar Model Calculation of Neutrino Fluxes Aldo Serenelli Institute for Advanced Study NOW 2006 Conca Specchiulla 11-Sept-2006.

Advertisements

SUSSP61: Neutrino Physics - St. Andrews, Scotland – 8 th to 23 rd, August, 2006 Standard Solar Models II Aldo Serenelli Institute for Advanced Study, Princeton.

The Standard Solar Model and Its Evolution Marc Pinsonneault Ohio State University Collaborators: Larry Capuder Scott Gaudi.

Neutrinos Louvain, February 2005 Alan Martin Arguably the most fascinating of the elementary particles. Certainly they take us beyond the Standard Model.

Teppei Katori, Indiana University1 PRD74(2006) Global 3 parameter Lorentz Violation model for neutrino oscillation with MiniBooNE Teppei Katori,

The Role of Neutrinos in Astrophysics A.B. Balantekin University of Wisconsin GDR Neutrino Laboratoire Astroparticule et Cosmologie.

Recent Discoveries in Neutrino Physics: Understanding Neutrino Oscillations 2-3 neutrino detectors with variable baseline 1500 ft nuclear reactor Determining.

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%

G. Sullivan - Princeton - Mar 2002 What Have We Learned from Super-K? –Before Super-K –SK-I ( ) Atmospheric Solar –SNO & SK-I Active solar –SK.

Solar Neutrinos, Neutrino Cross Sections, and NUSEL Developments A.B. Balantekin ORNL SNS Workshop August 28, 2003.

1 The pp-chain and the CNO-cycle after KamLAND Solar neutrinos after SNO and KamLAND The Boron flux The Beryllium flux Nuclear physics of the pp-chain.

1 Neutrino: a spy of the innermost solar interior Nuclear reactions in the Sun and solar neutrinos.

1 Trieste Sept Standard and non-standard solar models Success of stellar evolutionary theory Basic inputs of the theory Standard solar.

From Nuclei to Neutrinos The Naming of the Denys Wilkinson Building 21 June 2002 Nick Jelley.

CP-phase dependence of neutrino oscillation probability in matter 梅 (ume) 田 (da) 義 (yoshi) 章 (aki) with Lin Guey-Lin ( 林貴林 ) National Chiao-Tung University.

Properties of stars during hydrogen burning Hydrogen burning is first major hydrostatic burning phase of a star: Hydrostatic equilibrium: a fluid element.

1 Some key problems and key reactions in Nuclear Astrophysics Main issues: BBN: was the universe always the same? What’s in the core of Sun and other MS.

Reactor & Accelerator Thanks to Bob McKeown for many of the slides.

Results and Future of the KamLAND Experiment

Nuclear reactions and solar neutrinos

1 The pp-chain (and the CNO-cycle) after SNO and KamLAND Barbara Ricci, University of Ferrara and INFN Fourth International Conference on Physics Beyond.

1 Nuclear fusion in the Sun The spies of solar interior: –neutrinos –helioseismology What can be learnt about the Sun? What can be learnt about nuclear.

21-25 January 2002 WIN 2002 Colin Okada, LBNL for the SNO Collaboration What Else Can SNO Do? Muons and Atmospheric Neutrinos Supernovae Anti-Neutrinos.

1 B.Ricci* What have we learnt about the Sun from the measurement of 8B neutrino flux? Experimental results SSM predictions SSM uncertainties on  (8B)

October 3, 2003IFIC, UVEG-CSIC A road map to solar fluxes, osc. param., and test for new physics Carlos Pena Garay IAS ~

APS Neutrino Study: Reactor Working Group Beyond   Gabriela Barenboim.

CNO cycle All initial abundances within a cycle serve as catalysts and accumulate at largest  Extended cycles introduce outside material into CN cycle.

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%

Neutrinos from the primary proton- proton fusion process in the Sun pp neutrinos constitute nearly the entirety of solar neutrino flux Secondary neutrinos.

The Importance of Low-Energy Solar Neutrino Experiments Thomas Bowles Los Alamos National Laboratory Markov Symposium Institute for Nuclear Research 5/13/05.

SUSSP61: Neutrino Physics - St

李玉峰中科院高能所 JUNO中微子天文和天体物理学研讨会

GNO and the pp - Neutrino Challenge  T.Kirsten/GNO Till A. Kirsten Max-Planck-Institut für Kernphysik, Heidelberg for the GNO Collaboration NDM03 Nara/Japan.

Solar Neutrinos Perspectives and Objectives Mark Chen Queen’s University and Canadian Institute for Advanced Research (CIFAR)

Solar neutrino measurement at Super Kamiokande ICHEP'04 ICRR K.Ishihara for SK collaboration Super Kamiokande detector Result from SK-I Status of SK-II.

Neutrino oscillation physics II Alberto Gago PUCP CTEQ-FERMILAB School 2012 Lima, Perú - PUCP.

February 23, 2005Neutrino Telescopes, Venice Comparing Solar and KamLAND Data Comparing Solar and KamLAND Data Carlos Pena Garay IAS, Princeton ~

LAGUNA Large Apparatus for Grand Unification and Neutrino Astrophysics Launch meeting, Heidelberg, March 2007, Lothar Oberauer, TUM.

Methods and problems in low energy neutrino experiments (solar, reactors, geo-) I G. Ranucci ISAPP 2011 International School on Astroparticle physics THE.

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.

KamLAND : Studying Neutrinos from Reactor Atsuto Suzuki KamLAND Collaboration KEK : High Energy Accelerator Research Organization.

Kopylov A.V. Erice School/Workshop 2009 on Neutrinos in Cosmology, in Astro, in Particle and in Nuclear Physics in Erice/Trapani/Sicily/Italy on September.

Tests of non-standard neutrino interactions (NSI) Cecilia Lunardini Institute for Nuclear Theory University of Washington, Seattle.

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 from the sun, earth and SN’s: a brief excursion Aldo IFAE 2006 Pavia April 19 th.

Masatoshi Koshiba Raymond Davis Jr. The Nobel Prize in Physics 2002 "for pioneering contributions to astrophysics, in particular for the detection of cosmic.

 ( E ) = S(E) e –2   E -1 2      m  m   m   m   Reaction Rate(star)    (E)  (E) dE Gamow Peak  Maxwell Boltzmann.

Astroparticle physics 1. stellar astrophysics and solar neutrinos Alberto Carramiñana Instituto Nacional de Astrofísica, Óptica y Electrónica Tonantzintla,

Measuring  13 with Reactors Stuart Freedman HEPAP July 24, 2003 Bethesda Reactor Detector 1Detector 2 d2d2 d1d1.

Solar Neutrino Results from SNO

Cristina VOLPE BETA-BEAMS The beta-beam concept The baseline scenario The physics potential Conclusions LOW ENERGY BETA-BEAMS A N D The idea Motivation.

October 14th, 2006LONU-LENS, Virginia Tech Solar Luminosity by Neutrinos Solar Luminosity by Neutrinos Carlos Pena Garay IFIC, Valencia ~

5th June 2003, NuFact03 Kengo Nakamura1 Solar neutrino results, KamLAND & prospects Solar Neutrino History Solar.

SNO + SNO+ Steve Biller, Oxford University.  total SSM June 2001 (indirect) April 2002 (direct) (unconstrained CC spectrum) Sept 2003 (salt - unconstrained)

News from the Sudbury Neutrino Observatory Simon JM Peeters July 2007 o SNO overview o Results phases I & II o hep neutrinos and DSNB o Update on the III.

Solar Neutrinos & Homestake or Something new under the Sun Kevin T. Lesko Lawrence Berkeley National Laboratory Berkeley, CA.

Neutrino Physics II Hitoshi Murayama University of Pisa February 25, 2003.

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.

Solar Neutrinos on the beginning of 2017

MuD project: m + d  n + n + n

Solar & Supernova Neutrinos Detection Methods and Prospects

Solar Neutrino Problem

The pp-chain and the CNO-cycle after KamLAND

7. Internal structure. II.

1930: Energy conservation violated in β-decay

1.1 Neutrinos from the sun 1. Introduction

DUNE as the Next-Generation Solar Neutrino Experiment

Some Nuclear Physics with Solar Neutrinos

Solar Neutrino Flux -- in 3 lines

Presentation transcript:

The Standard Solar Model and Experiments Predictions versus experiments Uncertainties in predictions Challenges and open questions BP00: astro-ph/

Neutrino spectrum

diffgs98best Helioseismology confirms solar model to No free parameters Are standard solar models reliable? PRL 78, astro-ph/

2001: First direct confirmation 2002: SNO NC Agree to 0.03  Highlights: Agree to 0.3 

Precision measurements of 6 measurements 3 measurements Modern precision measurement: urgently required: ± 3%!

Cross section: Standard

BP00 %Uncertainties astro-ph/ Luminosity Diffusion Opacity Composition p-p Source

Why do low energy solar neutrino experiments?

Test (refine) neutrino oscillation solutions –Same behavior at high energies –Different behavior at low energies –Could be wrong! Test solar fusion theory –SSM: 99.99% of solar neutrinos < 5 MeV –Low energy fluxes predicted more precisely Redundancy, redundancy, redundancy

SSM: Fundamental Low-Energy tests CNO neutrinos represent 1.5% of luminosity Stellar evolution theory predicts: pp fusion formula: summarizes competition between different fusion chains.

KamLAND (Japan) reactor anti-neutrinos CPT Test hep-ph/ hep-ph/ Sterile neutrinos hep-ph/

Does the solar luminosity determine the pp flux? Theoretical error = 1% CNO cycle: 0 pp neutrinos Luminosity determines pp flux: 0 –1.0 max flux

Date published vs. date published Ground state only  Bahcall et al.  Others

7 Experiments; 34 years; 0.01% of the flux. A solar neutrino “opportunity”; not a problem.