Carbon Burning in the Universe and the Laboratory
|
|
|
- Claire Gray
- 5 years ago
- Views:
Transcription
1 Carbon Burning in the Universe and the Laboratory X. Tang University of Notre Dame
2 Carbon burning processes in the Universe Carbon burning in the laboratory Limits on the molecular resonance strengths Future experiments
3 Carbon burning p,α,n 23 Na, 20 Ne, 23 Mg
4 Fuel for the stars T. Spillane, Ph.D. Thesis, U. Of Connecticut
5 Impact to nucleosynthesis Standard Reduced rates Chieffi, Limongi, ApJ 647 (2006) 483 Gasques et al. PRC 76 (2007)
6 Type Ia supernova models: White dwarfs merge Or accreting white dwarf Carbon ignition in the core Institute for Structure and Nuclear Astrophysics Trigger for the explosion Disk Neutron star Superburst model: Accreting neutron stars Carbon ignition in the crust
7 Ignition conditions in type Ia supernovae thermonuclear burning White dwarf standard rate reduced rate Yakovlev et al. PRC 74 (2006) ; Gasques et al. PRC 76 (2007) pycnonuclear burning
8 20 Ne+α Light particle: p, n, α Gamma: 440 kev (p channel) 1634 kev (α channel) Fusion residue: 20 Ne, 23 Na no success under barrier 23 Mg: decay spectroscopy
9 The world's first tandem accelerator installed at Chalk River in Molecular resonances in the 12 C+ 12 C fusion reaction measured by Almqvist et al., in 1960
10 proton and alpha spectroscopy (Patterson 69, Mazarakis 73, Becker 78) <5 pμa 12 C Set up of Becker s experiment
11 Charged particle spectroscopy Only count the proton and alpha peaks which can be identified 8 Be? p, α? Potentially underestimate total fusion cross section Eg. missing 8 Be, neutron any more particle?
12 (Kettner 77, Erb 80, Aguilera Nuclear 06, Spillane Science Laboratory 07) Pictures are adapted from Spillane s talk
13 Kettner et al., Institute for Structure and Nuclear Astrophysics Good selectivity Low efficiency (3.6% for 440 kev and 1.9% for 1634 kev) Assume isotropic ang. distribution Need decay branching information to correct for the decay channels which do not decay via the first excited state!! (eg. ground state transition) Spillane et al., Ph.D. Thesis (2007)
14 The extrapolation to low energy is uncertain and more experimental and theoretical studies are urgently needed. Fowler, Nobel Lecture (1983) C. A. Barnes, P.193, Essays in Nuclear Astrophysics (1982)
15 Even more problematic? Hindrance?? R. Cooper et al., APJ (2009) 702, 660 Gasques et al. PRC 72 (2005) Jiang et al. PRC 75 (2007) Challenge for Laboratory nuclear-astrophysics in Underground and Surface 2009: CLAUS2009
16 12 C+ 13 C 13 C+ 13 C Provide potential to model the smooth behavior 13 C+ 13 C 12 C+ 12 C 12 C( 12 C,a) 20 Ne Direct measurement 24 Mg(a,a ) inelastic The exact cross section Search the possible resonances 12 C( 12 C,p) 23 Na 12 C( 12 C,n) 23 Mg 12 C( 12 C, 8 Be) 16 O
17 The 12 C+ 13 C experiment Institute for Structure and Nuclear Astrophysics Carbon stripping (100 ena) Gas stripping 2 eμa 13 C eμa 13 C - graphite disk Very compact beta counter 12 Ec.m.=2.83 MeV, C( 13 C, 24 Na)p 1puA*28hr,379 counts 10 MV FN ND Full (Ungated) 1.37MeV Gated 2.74MeV
18 Fusion reactions of carbon isotopes 4 nb Before correction Notre Dame 12 C+ 12 C(red, Becker et al., 1981) 12 C+ 13 C(blue, Notani et al., 2009) 13 C+ 13 C(purple, Trentalange 1982) Cross section factor: S(E)=σ*E*exp(87.21/sqrt(E)) The 12 C +12 C is not enhanced but suppressed!
19 Fusion reactions of carbon isotopes After correcting the isotope effect (difference in mass and radius)
20 S(E)(MeV*b) Institute for Structure and Nuclear Astrophysics Limits on the resonance strengths S factor (MeV*b) Cooper (2009) Spillane (2007) Predicted 12 C+ 12 C without cc 12C+ 12 C experiments: Becker (1981) Spillane (2007) Kovar (1979) Becker (1981) E c.m. (MeV) Predicted 12 C+ 12 C with cc CF88 Recommended S factor Kovar (1979) First precise systematic description of the molecular resonance strengths Upper limit: ~2.5xCF88 Lower limit: 0.7*CF88 OR LESS HINDRANCE
21 Naples Experiment Detector coincidence to veto cosmic rays Ω=0.19 sr
22 Preliminary results from Caserta S*(E)=S(E)*exp(0.46*E) Uncertainties below 2.5 MeV range from % on each curve Gamma ray data correspond to the 440 kev line of 23 Na and charged particle data to P0 and P1 groups (normalization necessary) Modifications are necessary to achieve energies below 2 MeV (higher beam currents, larger efficiency, etc.) Jim Zickefoose, U. Conn Thesis (2010)
23 The past 12 C( 12 C,n) 23 Mg experiment -Potential neutron source for the weak s-process -Sharp peak in β n? -Model calculation requires renormalization!
24 Study by Pignatari et al Measure 12 C( 12 C,n) 23 Mg at lower energies with better uncertainties!
25 Preliminary Results B. Bucher, Session CG 006, Thursday cüxä Å ÇtÜç cüxä Å ÇtÜç -Cover the entire energy range measured before. -Working on measurement towards lower energies. -Confirm peak in β n! -Statistical model calculation not reliable! -Use mirror symmetry instead.
26 Future experiments Find treasure at the end of rainbow? Earlier preliminary result from Caserta, May 2009 Indirect search of unknown resonances ( 24 Mg(a,a ) at RCNP) Extend measurement towards lower energies 1) Particle-gamma experiment 2) Solenoid spectrometer
27 Extension of 12 C + 12 C towards lower energies: Particle γ coincidences (e.g. p γ or α γ) Particle recoil coincidences (e.g. p 23 Na) γ recoil coincidences (e.g. γ 23 Na) E cm =4MeV 100 pna beam
28 Notre Dame-ANL fusion experiment Georgina at ND Clover array at ANL A 5 MV Pelletron with ECR source in terminal. Will be installed at the end of 2011.
29 Jr. Helios at Notre Dame High efficiency, good resolution, economic upgrade!
30
31 Long Range Plan: DUSEL
32 Summary Institute for Structure and Nuclear Astrophysics The extrapolation to low energy is VERY uncertain and more experimental and theoretical studies are urgently needed. Using Isotope fusion, the upper limit is defined. The lower limit may be further reduced by the hindrance effect. The proposed new developments, particle-gamma array and solenoid spectrometer coupling with the forthcoming new accelerator at ND, will provide us the best opportunity than ever to address the key problems in nuclear astrophysics.
33 Carbon burning and more A new research program in NSL EG`z Institute for Structure and Nuclear Astrophysics The 2010 dream team: Coach: X. Tang (Prof.) Supernova players: B. Bucher (Grad.) X. Fang (Grad.) A. Alongi (Undergrad.) J. Browne (Undergrad.) + the whole NSL lab + Esbensen and ANL Some key players who have contributed in the carbon burning project from 2007 to 2009: M. Notani (postdoc, ) JINA support visiting students from Surrey: P. Davies (2007), S. Thomas (2008) Grad: C. Ma (master, ) REU: N. Schroeder, A. Hillmer, G. Buffaloe(F), C. Garcia(F), A. Moncion Undergrad: D. Cerrone ( )
Perspectives on Nuclear Astrophysics
Perspectives on Nuclear Astrophysics and the role of DUSEL Nuclear Astrophysics is a broad field that needs facilities from 1keV-100GeV A low energy accelerator DIANA a DUSEL is a unique instrument for
High Resolution Spectroscopy in Nuclear Astrophysics. Joachim Görres University of Notre Dame & JINA
High Resolution Spectroscopy in Nuclear Astrophysics Joachim Görres University of Notre Dame & JINA Nuclear Astrophysics Studies at RCNP Osaka Notre Dame Groningen Started in 2002 (Georg @ RCNP) with a
PoS(NIC XI)019. Low energy beam induced background studies for a. 12 C( 12 C,p) 23 Na reaction cross section measurement
Low energy beam induced background studies for a 12 C( 12 C,p) 23 Na reaction cross section measurement James Zickefoose, Jeffrey Schweitzer, Timothy Spillane University of Connecticut Storrs CT, USA zickefoose@phys.uconn.edu
First direct measurement of 12 C( 12 C,n) 23 Mg at stellar energies
EPJ Web of Conferences 109, 04009 (2016) DOI: 10.1051/ epjconf/ 201610904009 C Owned by the authors, published by EDP Sciences, 2016 First direct measurement of 12 C( 12 C,n) 23 Mg at stellar energies
Ne(alpha,n) revisited
22 Ne(alpha,n) revisited Joachim Görres University of Notre Dame & JINA Ph.D. Thesis of Rashi Talwar Neutron sources for the s-process Main Component A>100 Weak Component A< 100 low mass AGB stars T= 0.1
Subbarrier fusion of carbon isotopes ~ from resonance structure to fusion oscillations ~
Subbarrier fusion of carbon isotopes ~ from resonance structure to fusion oscillations ~ Kouichi Hagino, Tohoku University Neil Rowley, IPN Orsay 1. Introduction: 12 C + 12 C fusion 2. Molecular resonances
Preliminary results of the indirect study of the 12 C( 12 C,α) 20 Ne reaction via the THM applied to the 16 O( 12 C,α 20 Ne )α reaction
Preliminary results of the indirect study of the 12 C( 12 C,α) 20 Ne reaction via the THM applied to the 16 O( 12 C,α 20 Ne )α reaction G.G. Rapisarda, 1,2,6 C. Spitaleri, 1,2 C. Bordeanu, 3 Z. Hons, 4
Fusion Reactions with Carbon Isotopes
Fusion Reactions with Carbon Isotopes Henning Esbensen Argonne National Laboratory, Argonne IL, USA Problems: Large structures in 12 C+ 12 C fusion data. Large systematic uncertainties of 15% or more.
DIANA A NEXT GENERATION DEEP UNDERGROUND ACCELERATOR FACILITY
DIANA D. Leitner for the DIANA collaboration Michigan State University PAC 2011 New York, April 2011 A NEXT GENERATION DEEP UNDERGROUND ACCELERATOR FACILITY Outline of the Talk Why underground? Brief science
This is a repository copy of How well do we understand the reaction rate of C burning?.
This is a repository copy of How well do we understand the reaction rate of C burning?. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/126678/ Version: Published Version
A New Measurement of the E1 Component of
A New Measurement of the E1 Component of the 12 C(α,γ) 16 O Reaction X. Tang Physics Division Argonne National Laboratory Outline Why is the 12 C(α, γ) 16 O reaction important? The 12 C(α,γ) 16 O reaction
Direct (α,p) Reaction Measurements with HELIOS and the study of 20 Ne(α,p) 23 Na
Direct (α,p) Reaction Measurements with HELIOS and the study of 20 Ne(α,p) 23 Na Jianping Lai, Daniel Santiago-Gonzalez Catherine M. Deibel Louisiana State University 9/13/16 INPC 2016 1 (α,p) Reactions
Experimental Nuclear Astrophysics: Lecture 1. Chris Wrede National Nuclear Physics Summer School June 19 th, 2018
: Lecture 1 Chris Wrede National Nuclear Physics Summer School June 19 th, 2018 Outline Lecture 1: Introduction & charged-particle reactions Lecture 2: Neutron-capture reactions Lecture 3: What I do (indirect
Gamma Efficiency Simulations for Coincident Fusion Cross Section Measurements
Gamma Efficiency Simulations for Coincident Fusion Cross Section Measurements ANSRI 2016 Marcel Heine for the STELLA Collaboration CNRS Strasbourg 5/13/2016 Outlook 1 Deep Sub-barrier Fusion Cross Sections
Hydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects. Catherine M. Deibel Louisiana State University
Hydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects Catherine M. Deibel Louisiana State University 8/29/14 CGS15 August 25 29, 2014 1 Click Type to I X-Ray edit
From the Midwest to the World the Joint Institute for Nuclear Astrophysics Hendrik Schatz Michigan State University
From the Midwest to the World the Joint Institute for Nuclear Astrophysics Hendrik Schatz Michigan State University 15 Years of Nuclear Astrophysics with JINA It started all at Notre Dame National and
Research at FSU, using RESOLUT facility Development of and research with two new detector-systems
Nuclear Astrophysics and Structure Research with Radioactive Beams Research at FSU, using RESOLUT facility Development of and research with two new detector-systems ResoNeut: Low-energy neutron detector-array
12 C + 12 C reactions at astrophysical energies: Tests of targets behaviour under beam bombardment
12 C + 12 C reactions at astrophysical energies: Tests of targets behaviour under beam bombardment L. Morales-Gallegos, M. Aliotta, A. Di Leva, L. Gialanella, D. Schürmann, M. De Cesare, T. Davinson, G.
Neutrino Physics and Nuclear Astrophysics: the LUNA-MV project at Gran Sasso
Neutrino Physics and Nuclear Astrophysics: the LUNA-MV project at Gran Sasso I.N.F.N., Sezione di Genova, Italy Via Dodecanneso, 16146 Genoa (Italy) E-mail: sandra.zavatarelli@ge.infn.it Solar neutrinos
Investigation of radiative proton-capture reactions using high-resolution g-ray spectroscopy
Investigation of radiative proton-capture reactions using high-resolution g-ray spectroscopy P. Scholz, F. Heim, J. Mayer, M. Spieker, and A. Zilges Institute for Nuclear Physics, University of Cologne
Nuclear Astrophysics - I
Nuclear Astrophysics - I Carl Brune Ohio University, Athens Ohio Exotic Beam Summer School 2016 July 20, 2016 Astrophysics and Cosmology Observations Underlying Physics Electromagnetic Spectrum: radio,
Nuclear Astrophysics II
Nuclear Astrophysics II Lecture 5 Fri. June 1, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437 shawn.bishop@ph.tum.de http://www.nucastro.ph.tum.de/ 1 Where to from here? We are now at a crossroads for
Nuclear Astrophysics with DRAGON at ISAC:
Nuclear Astrophysics with DRAGON at ISAC: The 21 Na(p, γ) 22 Mg reaction John M. D Auria for the DRAGON Collaboration Simon Fraser University Burnaby, British Columbia, Canada Abstract The DRAGON facility
Experimental Initiatives in Nuclear Astrophysics
Experimental Initiatives in Nuclear Astrophysics Carl Brune Astrophysics: H and He burning, S process Facilities: neutron and gamma beams, underground accelerators, ICF plasmas Joint DNP Town Meetings
MRC-1: Low Energy Nuclear Reactions and Stellar Evolution
MRC-1: Low Energy Nuclear Reactions and Stellar Evolution Michael Wiescher Focus-1: Stellar Hydrogen burning in massive stars Re-evaluation of CNO cycles Focus-2: Stellar He-burning neutron sources for
Recoil Separators for Nuclear Astrophysics studies Manoel Couder
Recoil Separators for Nuclear Astrophysics studies Manoel Couder Institute for Structure and Nuclear Astrophysics University of Notre Dame Joint Institute for Nuclear Astrophysics Outline Nuclear astrophysics
H/He burning reactions on unstable nuclei for Nuclear Astrophysics
H/He burning reactions on unstable nuclei for Nuclear Astrophysics PJ Woods University of Edinburgh H T O F E E U D N I I N V E B R U S I R T Y H G Explosive H/He burning in Binary Stars Isaac Newton,
PoS(NIC XI)182. The effect of 12 C + 12 C rate uncertainties on the weak s-process component
The effect of C + C rate uncertainties on the weak s-process component Michael E. Bennett a, Raphael Hirschi ab, Marco Pignatari gcd, Steven Diehl e, Chris Fryer f, Falk Herwig g, William Hillary g, Aimee
Primer: Nuclear reactions in Stellar Burning
Primer: Nuclear reactions in Stellar Burning Michael Wiescher University of Notre Dame The difficulty with low temperature reaction rates CNO reactions in massive main sequence stars He burning reactions
SURROGATE REACTIONS. An overview of papers by Jason Burke from LLNL
SURROGATE REACTIONS An overview of papers by Jason Burke from LLNL Compound Nuclear Reaction cross sections Cross sections for compound-nuclear reactions are required input for astrophysical models and
Future research of 12 C(a,g) 16 O. Claudio Ugalde
Future research of 12 C(a,g) 16 O Claudio Ugalde 12 C(a,g) 16 O Reaction Key reaction for stellar structure, evolution, and nucleosynthesis in stars. Affects the synthesis of most of the elements of the
Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams
Hirschegg 06-1 Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams S. Kubono Center for Nuclear Study (CNS) University of Tokyo 1. Low Energy RI Beam Production 2. Proton Resonance
X-ray superburst ~10 42 ergs Annual solar output ~10 41 ergs. Cumming et al., Astrophys. J. Lett. 559, L127 (2001) (2)
Neutron stars, remnant cores following supernova explosions, are highly interesting astrophysical environments In particular, accreting neutron stars presents a unique environment for nuclear reactions
Physics opportunities with the AT-TPC. D. Bazin NSCL/MSU at ReA
Physics opportunities with the AT-TPC D. Bazin NSCL/MSU at ReA Reaction studies at ReA Radioactive beams are used in inverse kinematics Target is now the (usually light) probe nucleus Scattered particles
Experimental Nuclear Astrophysics: Lecture 3. Chris Wrede National Nuclear Physics Summer School June 20 th, 2018
: Lecture 3 Chris Wrede National Nuclear Physics Summer School June 20 th, 2018 Outline Lecture 1: Introduction & charged-particle reactions Lecture 2: Neutron-induced reactions Lecture 3: What I do (indirect
From Notre Dame to National Labs: Cross sections at no charge!
From Notre Dame to National Labs: Cross sections at no charge! NSL 80 th Anniversary Celebration A. Couture 8 April 2018 Operated by Los Alamos National Security, LLC for the U.S. Department of Energy's
EVOLUTION OF SHELL STRUCTURE
EVOLUTION OF SHELL STRUCTURE W A RICHTER ITHEMBA LABS UNIVERSITY OF THE WESTERN CAPE Focus points: 1. Single-particle structure of nuclei 2. Elastic scattering 3. The Interface between Nuclear structure
Progress in measuring GMR in unstable nuclei: Decay detector calibration and inverse reaction experiment. J. Button, Y.-W. Lui, and D.H.
Progress in measuring GMR in unstable nuclei: Decay detector calibration and inverse reaction experiment J. Button, Y.-W. Lui, and D.H. Youngblood I. Introduction The Giant Monopole Resonance (GMR) is
Latest results from LUNA
Journal of Physics: Conference Series PAPER OPEN ACCESS Latest results from LUNA To cite this article: Rosanna Depalo and LUNA collaboration 2018 J. Phys.: Conf. Ser. 940 012026 View the article online
Hydrogen & Helium Burning in Stars
Hydrogen & Helium Burning in Stars What remains to be done and how to do it! Hydrogen Burning: 4 He, 14 N Helium Burning: 12 C, 16 O, 22 Ne, n, s-nuclei Alba Formicola (on behalf of LUNA collaboration)
13 Synthesis of heavier elements. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
13 Synthesis of heavier elements introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 The triple α Reaction When hydrogen fusion ends, the core of a star collapses and the temperature can reach
Ne(p,γ) 23 Na MEASUREMENT AT LUNA II AND IMPACT ON ASTROPHYSICAL SCENARIOS. MARIE-LUISE MENZEL for the LUNA collaboration
22 Ne(p,γ) 23 Na MEASUREMENT AT LUNA II AND IMPACT ON ASTROPHYSICAL SCENARIOS MARIE-LUISE MENZEL for the LUNA collaboration 1. INTRODUCTION 1.1 NEON-SODIUM-CYCLE 1.2 THE 22 Ne(p,γ) 23 Na REACTION INTRODUCTION
Constraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies
Constraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies Christoph Langer (JINA/NSCL) INT Workshop: Reactions and Structure of Exotic Nuclei March 2015 1 Understanding
FUSION REACTIONS IN MULTICOMPONENT DENSE MATTER
FUSION REACTIONS IN MULTICOMPONENT DENSE MATTER D. G. Yakovlev Ioffe Physico-Technical Institute, Poliekhnicheskaya 26, 194021 Saint-Petersburg, Russia Department of Physics & The Joint Institute for Nuclear
Capabilities at the National Superconducting Cyclotron Laboratory. Sean Liddick NDNCA workshop, May 26-29, 2015
Capabilities at the National Superconducting Cyclotron Laboratory Sean Liddick NDNCA workshop, May 26-29, 2015 NSCL and FRIB Laboratory NSCL is funded by the U.S. National Science Foundation to operate
The 22 Ne(α,n) 25 Mg reaction at astrophysical energies studied via the Trojan Horse Method applied to the 2 H( 25 Mg, α 22 Ne) 1 H reaction
The 22 Ne(α,n) 25 Mg reaction at astrophysical energies studied via the Trojan Horse Method applied to the 2 H( 25 Mg, α 22 Ne) 1 H reaction R. Spartà 1, M. La Cognata 1, C. Spitaleri 1,2, S. Cherubini
Experimental Study of Stellar Reactions at CNS
Experimental Study of Stellar Reactions at CNS Shigeru KUBONO ( 久保野茂 ) Center for Nuclear Study (CNS) University of Tokyo 1. Nucleosynthesis under Explosive Conditions + CNS-RIKEN AVF-Upgrade Project 2.
A Comparison between Channel Selections in Heavy Ion Reactions
Brazilian Journal of Physics, vol. 39, no. 1, March, 2009 55 A Comparison between Channel Selections in Heavy Ion Reactions S. Mohammadi Physics Department, Payame Noor University, Mashad 91735, IRAN (Received
Production and Separation of Radioactive Beams. Mg and 20 Na with MARS
Production and Separation of Radioactive Beams 20 Mg and 20 Na with MARS Gopal Subedi, Colby College REU 2009, Cyclotron Institute, TAMU Advisor: Dr. Robert E. Tribble August 23, 2009 1 Overview Motivation
Recent neutron capture measurements at FZK
René Reifarth Recent neutron capture measurements at FZK Outline: Overview of s-process nucleosynthesis Nuclear data needs for the s-process where do we stand? Recent (n,γ) cross section measurements at
Stellar Evolution: what do we know?
Stellar Evolution: what do we know? New Tools - Astronomy satellite based observatories Hubble Space Telescope Compton Gamma-Ray Observatory Chandra X-Ray Observatory INTEGRAL ground based observatories
JINA collaborations & conferences
JINA collaborations & conferences Goal of JINA is to initiate a broad spectrum of collaboration to maximize expertise and input to address specific research goals addressed by MRC1 and MRC2! Goal of JINA
Spectroscopy of light exotic nuclei using resonance scattering in inverse kinematics.
Spectroscopy of light exotic nuclei using resonance scattering in inverse kinematics. Grigory Rogachev RESOLUT: a new radioactive beam facility at FSU Solenoid 2 Magnetic Spectrograph Magnetic Spectrograph
Background (α,n) reactions at low energies: 10,11 B(α,n) 13,14 N
Background (α,n) reactions at low energies: 10,11 B(α,n) 13,14 N (Richard) James deboer Nuclear Physics in Astrophysics VIII Catania, Italy June 20, 2017 Improved rates for neutron production reactions
Nuclear Astrophysics Underground Status & Future
Nuclear Astrophysics Underground Status & Future Frank Strieder South Dakota School of Mines & Technology XV International Symposium on Nuclei in the Cosmos Laboratori Nazionali del Gran Sasso, Assergi,
Resonance scattering and α- transfer reactions for nuclear astrophysics.
Resonance scattering and α- transfer reactions for nuclear astrophysics. Grigory Rogachev Outline Studying resonances using resonance scattering Studying resonances using transfer reactions Resonances
Lecture 13: Binary evolution
Lecture 13: Binary evolution Senior Astrophysics 2017-04-12 Senior Astrophysics Lecture 13: Binary evolution 2017-04-12 1 / 37 Outline 1 Conservative mass transfer 2 Non-conservative mass transfer 3 Cataclysmic
Nuclear physics activities in Vietnam (highlight from NHEP2016 conference)
Nuclear physics activities in Vietnam (highlight from NHEP2016 conference) Experimental nuclear physics (INST Hanoi, INR Da Lat, IOP Hanoi): mainly through the international collaboration projects (nuclear
Nucleosynthesis. at MAGIX/MESA. Stefan Lunkenheimer MAGIX Collaboration Meeting 2017
Nucleosynthesis 12 C(α, γ) 16 O at MAGIX/MESA Stefan Lunkenheimer MAGIX Collaboration Meeting 2017 Topics S-Factor Simulation Outlook 2 S-Factor 3 Stages of stellar nucleosynthesis Hydrogen Burning (PPI-III
International Nuclear Physics Conference Adelaide, Australia September 13, 2016
International Nuclear Physics Conference Adelaide, Australia September 13, 2016 This work was performed under the auspices of the U.S. Department of Energy by under contract DE-AC52-07NA27344. Lawrence
Reaction rates in the Laboratory
Reaction rates in the Laboratory Example I: 14 N(p,γ) 15 O slowest reaction in the CNO cycle Controls duration of hydrogen burning Determines main sequence turnoff glob. cluster ages stable target can
Study of Neutron-Proton Correlation & 3N-Force in 12 C
Study of Neutron-Proton Correlation & 3N-Force in C Outline: 1. Interesting physics on np-correlations in C 2. Probe: Two-nucleon knockout reaction Partial cross section and P // measurements 3. Experimental
Nuclear astrophysics studies with charged particles in hot plasma environments
Nuclear astrophysics studies with charged particles in hot plasma environments Manoel Couder University of Notre Dame Summary I NSTITUTE FOR S TRUCTURE AND N UCLEAR A STROPHYSICS Accelerator based nuclear
The LUNA - MV project at the Gran Sasso Laboratory
The LUNA - MV project at the Gran Sasso Laboratory Roberto Menegazzo for the LUNA Collaboration 3ème Andromède Workshop - Orsay, 9 Juillet 2014 outlook LUNA: Why going underground to measure nuclear fusion
Measurements of the Astrophysically Important 40 Ca(α,γ) 44 Ti Reaction Rate. Daniel Robertson JINA Frontiers Meeting Oct.
Measurements of the Astrophysically Important 40 Ca(α,γ) 44 Ti Reaction Rate Daniel Robertson JINA Frontiers Meeting 21-23 Oct. 2010 Why study 44 Ti at all? Recent observations of live 44 Ti highlight
Accreting Neutron Stars
Tracy K. Steinbach Indiana University Accreting Neutron Stars ² The outer crust of an accreting neutron star is an unique environment for nuclear reactions ² Identified as the origin of energetic X-ray
Evolution and nucleosynthesis prior to the AGB phase
Evolution and nucleosynthesis prior to the AGB phase Amanda Karakas Research School of Astronomy & Astrophysics Mount Stromlo Observatory Lecture Outline 1. Introduction to AGB stars, and the evolution
Introductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM
Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M
Experiments on reaction rates for the astrophysical p-process
Experiments on reaction rates for the astrophysical p-process Zs. Fülöp ATOMKI Debrecen, Hungary Science case Experimental needs Used technique Trends in available data Plans for the future Heavy element
Supernova Nucleosynthesis
Supernova Nucleosynthesis Andrea Kulier Princeton University, Department of Astrophysical Sciences November 25, 2009 Outline o Overview o Core-Collapse Supernova Nucleosynthesis o Explosive Nucleosynthesis
Method of active correlations in the experiment 249 Cf+ 48 Ca n
Method of active correlations in the experiment 249 Cf+ 48 Ca 297 118 +3n Yu.S.Tsyganov, A.M.Sukhov, A.N.Polyakov Abstract Two decay chains originated from the even-even isotope 294 118 produced in the
He-Burning in massive Stars
He-Burning in massive Stars He-burning is ignited on the He and ashes of the preceding hydrogen burning phase! Most important reaction -triple alpha process 3 + 7.6 MeV Red Giant Evolution in HR diagram
Accreting neutron stars provide a unique environment for nuclear reactions
, Tracy Steinbach, Jon Schmidt, Varinderjit Singh, Sylvie Hudan, Romualdo de Souza, Lagy Baby, Sean Kuvin, Ingo Wiedenhover Accreting neutron stars provide a unique environment for nuclear reactions High
Presentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7
Presentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7 Outline 1. Background 1.1 Decay for proton-rich nuclei 1.2 Astrophysical implications 2. Experiments 2.1 Introduction 2.2 Experimental
Nuclear Waiting Points and Double Peaked X-Ray Bursts
Nuclear Waiting Points and Double Peaked X-Ray Bursts WITH TODAY'S HONORARY CO-AUTHORSHIP: David Miles Kahl Department of Physics & Astronomy, McMaster University, 1280 Main Street West, ABB 248, Hamilton,
The Application of R-Matrix Analysis to Experimental Data. 1 - Resonance Properties. Alex Murphy & David Mountford
The Application of R-Matrix Analysis to Experimental Data 1 - Resonance Properties Alex Murphy & David Mountford Contents The R-Matrix Formalism Context: The 18 F(p,α) 15 O Reaction (Doing an ) R-Matrix
PoS(ENAS 6)050. Resonances in 19 Ne with relevance to the astrophysically important 18 F(p,α) 15 O reaction
Resonances in 19 Ne with relevance to the astrophysically important 18 F(p,α) 15 O reaction David Mountford, A.St J. Murphy, T. Davinson, P.J. Woods University of Edinburgh E-mail: d.j.mountford@sms.ed.ac.uk
at Gran Sasso Laboratories, Italy
Underground Nuclear Astrophysics at Gran Sasso Laboratories, Italy Francesca Cavanna Università di Genova and INFN Genova, Italy Helmholtz Zentrum Dresden Rossendorf, Germany Laboratory Underground Nuclear
Theory for nuclear processes in stars and nucleosynthesis
Theory for nuclear processes in stars and nucleosynthesis Gabriel Martínez Pinedo Nuclear Astrophysics in Germany November 15-16, 2016 Nuclear Astrophysics Virtual Institute Outline 1 Ab-initio description
Nuclear Reactions A Z. Radioactivity, Spontaneous Decay: Nuclear Reaction, Induced Process: x + X Y + y + Q Q > 0. Exothermic Endothermic
Radioactivity, Spontaneous Decay: Nuclear Reactions A Z 4 P D+ He + Q A 4 Z 2 Q > 0 Nuclear Reaction, Induced Process: x + X Y + y + Q Q = ( m + m m m ) c 2 x X Y y Q > 0 Q < 0 Exothermic Endothermic 2
Decay spectroscopy for nuclear astrophysics
Decay spectroscopy for nuclear astrophysics 1 Cyclotron Institute, Texas A&M University College Station, TX 77843-3366, USA E-mail: livius_trache@tamu.edu Abstract. In many radiative proton capture reactions
Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
Spin assignments of 22 Mg states through a 24 Mg(p,t) 22 Mg measurement, K. L. Jones, B. H. Moazen, S. T. Pittman Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996,
Scientific goal in Nuclear Astrophysics is to explore:
Nuclear Physics in Stars Michael Wiescher University of Notre Dame Joint Institute for Nuclear Astrophysics Scientific goal in Nuclear Astrophysics is to explore: Nuclear Signature in the Cosmos The Nuclear
Alpha Particle: or Beta Particle: or Neutron: or n 0. Positron: Proton: or p + Gamma Ray:
Key Worksheet 21 Nuclear Chemistry Objectives To be able to write and use a nuclear chemical equation. To be able to predict the missing reactants or products in a nuclear chemical reaction. To be able
Fossil Records of Star Formation: John Beacom, The Ohio State University
Fossil Records of Star Formation: Supernova Neutrinos and Gamma Rays Basic Pitch Supernovae are of broad and fundamental interest Neutrinos and gamma rays are direct messengers Recent results show that
Nuclear Astrophysics Research at HIγS
Nuclear Astrophysics Research at HIγS Selected Examples of Work in Progress Werner Tornow Duke University & TUNL Outline A. What is HIγS? B. Few-Body Physics (see T. Shima) C. Nuclear Astrophysics 4 9
b delayed g decay measurements to probe thermonuclear astrophysical explosions
b delayed g decay measurements to probe thermonuclear astrophysical explosions Chris Wrede Michigan State University and NSCL for the NSCL E10034, E12028 & E14066 collaborations NIC XIII, Debrecen, Hungary
Search for 24 Mg resonances inside the Gamowwindow for 12 C+ 12 Cfusion. Neven Soić, Ruđer Bošković Institute, Zagreb, Croatia
Search for 24 Mg resonances inside the Gamowwindow for C+ Cfusion C γ 24 Mg C γ Neven Soić, Ruđer Bošković Institute, Zagreb, Croatia Collaborators 1) S. Blagus, L. Grassi, D. Jelavić Malenica, T. Mijatović,
(EXPERIMENTAL) NUCLEAR ASTROPHYSICS. study energy generation processes in stars study nucleosynthesis of the elements
(EXPERIMENTAL) NUCLEAR ASTROPHYSICS Ø Ø study energy generation processes in stars study nucleosynthesis of the elements What is the origin of the elements? How do stars/galaxies form and evolve? What
HiRA: Science and Design Considerations
HiRA: Science and Design Considerations Scientific Program: Astrophysics: Transfer reactions Resonance spectroscopy Nuclear Structure: Inelastic scattering Transfer reactions Resonance spectroscopy Breakup
A. Gyurjinyan. Receved 05 February 2016
Armenian Journal of Physics, 2016, vol. 9, issue 1, pp. 39-43 16 O 8 Be + 8 Be Decay Simulation A. Gyurjinyan Experimental Physics Division, Yerevan Physics Institute, Yerevan, Armenia, 0038 Physics Department,
S1378: Lifetime Measurement of the MeV State in 23 Mg
S1378: Lifetime Measurement of the 7.786 MeV State in 23 Mg Charles Akers, Peter Bender, Alison Cheeseman, Greg Christian, Randy Churchman, David Cross, Barry Davids, Lee Evitts, Jennifer Fallis, Naomi
Novae Reaction Rates and Measurements
Nova Cygni Nova T Pyxidis Novae Reaction Rates and Measurements Measuring Nuclear Reaction Rates One Step at a Time Shawn Bishop, TUM Erice School, 2010 1 Talk Outline Astrophysics Primer Experimental
The Origin of the Elements between Iron and the Actinides Probes for Red Giants and Supernovae
The Origin of the Elements between Iron and the Actinides Probes for Red Giants and Supernovae I Outline of scenarios for neutron capture nucleosynthesis (Red Giants, Supernovae) and implications for laboratory
RCNP cyclotron facility
11th International Conference on HEAVY ION ACCELERATOR TECHNOLOGY RCNP cyclotron facility K. Hatanaka hatanaka@rcnp.osaka-u.ac.jp Research Center for Nuclear Physics Osaka University HIAT09 TU9 June 9,
Nuclear Astrophysics
Nuclear Astrophysics I. Stellar burning Karlheinz Langanke GSI & TU Darmstadt Aarhus, October 6-10, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics Aarhus, October 6-10, 2008 1 / 32
GALACTIC Al 1.8 MeV GAMMA-RAY SURVEYS WITH INTEGRAL
Proceedings of the 3rd Galileo Xu Guangqi Meeting International Journal of Modern Physics: Conference Series Vol. 23 (2013) 48 53 c World Scientific Publishing Company DOI: 10.1142/S2010194513011069 GALACTIC
Studying the nuclear pairing force through. Zack Elledge and Dr. Gregory Christian
Studying the nuclear pairing force through 18 O( 26 Mg, 28 Mg) 16 O Zack Elledge and Dr. Gregory Christian Weizsaecker Formula Binding energy based off of volume and surface terms (strong force), coulomb
What do we measure, and how do we measure it?
What do we measure, and how do we measure it? Production of transactinides Isolation of nuclei of interest Instrumentation and measurements K. Hauschild Production of Transactinides N-capture + β-decay
(10%) (c) What other peaks can appear in the pulse-height spectrum if the detector were not small? Give a sketch and explain briefly.
Sample questions for Quiz 3, 22.101 (Fall 2006) Following questions were taken from quizzes given in previous years by S. Yip. They are meant to give you an idea of the kind of questions (what was expected