Does the 12 C+ 12 C fusion reaction ignite superbursts?

Slides:

Advertisements

Similar presentations

Saed Dababneh. Seventh Symposium on Use of Nuclear Techniques in Environmental Studies. Yarmouk University, JORDAN. 3-5 Sept Manipulated Gamma Spectroscopy:

Advertisements

Accelerator Physics, JU, First Semester, (Saed Dababneh).

Nuclear Binding Energy

NuPECC - Milan Present and future of Laboratory Underground Nuclear Astrophysics Alba Formicola - Status of the D(, ) 6 Li measurement -Status of.

Nuclear Astrophysics Experiments in ATOMKI Gy. Gyürky Institute of Nuclear Research (ATOMKI) Debrecen, Hungary.

Max-Planck-Institut für Plasmaphysik EURATOM Assoziation Interaction of nitrogen plasmas with tungsten Klaus Schmid, A. Manhard, Ch. Linsmeier, A. Wiltner,

Section 2: Nuclear Fission and Fusion

Polarization Observables in Hyperon Photoproduction with CLAS Craig Paterson University of Glasgow Eurotag Workshop Glasgow, 1 st September 2008.

University of Notre Dame

FUSTIPEN Topical Meeting ”Structure of the neutron star crust: experimental and observational signatures" May 26-27, 2014, GANIL, Caen, France Organizers:

W. A. Horowitz Quark Matter 2005 A Promising Solution to the Elliptic Quench Puzzle at RHIC William A. Horowitz Columbia University August 4-5, 2005.

Progress on the 40 Ca(α,  ) 44 Ti reaction using DRAGON Chris Ouellet Supervisor: Alan Chen Experiment leader: Christof Vockenhuber ● Background on the.

The Role of 12 C( 12 C,n) in the Astrophysical S-Process Brian Bucher University of Notre Dame.

The 12C+12C fusion reaction: a new opportunity at ATLAS Xiaodong Tang 1 & Chenglie Jiang 2 1) Univ. of Notre Dame 2) ANL.

JINA Frontiers 2005 Lifetimes of the astrophysically important states in 19 Ne Wanpeng Tan University of Notre Dame Collaborators: J. Görres, M. Wiescher,

May/27/05 Exotic Hadron WS 1 Hypothetical new scaler particle X for  + and its search by the (K +, X + ) reaction T. Kishimoto Osaka University.

Heavy Quark Probes of QCD Matter at RHIC Huan Zhong Huang University of California at Los Angeles ICHEP-2004 Beijing, 2004.

3  reaction  +  +  12 C  p process: 14 O+  17 F+p 17 F+p 18 Ne 18 Ne+  … In detail:  p process Alternating ( ,p) and (p,  ) reactions: For.

Astrophysical S(E)-factor of the 15 N(p,α) 12 C reaction at sub-Coulomb energies via the Trojan-horse method Daniel Schmidt, Liberty University Cyclotron.

Astrophysical S(E)-factor of the 15N(p,α)12C reaction at sub-Coulomb energies via the Trojan-horse method Daniel Schmidt, Liberty University Cyclotron.

Reaction rates in the Laboratory Example I: 14 N(p,  ) 15 O stable target  can be measured directly: slowest reaction in the CNO cycle  Controls duration.

Tony WeidbergNuclear Physics Lectures1 Applications of Nuclear Physics Fusion –(How the sun works covered in Astro lectures) –Fusion reactor Radioactive.

Gang Wang (WWND2010)1 Search for local parity violation with STAR ZDC-SMD Gang Wang (UCLA) for STAR Collaboration.

Measurement of B (D + →μ + ν μ ) and the Pseudoscalar Decay Constant f D at CLEO István Dankó Rensselaer Polytechnic Institute representing the CLEO Collaboration.

If the sun is a burning ball of gas … just what gas is it burning? Warmup Question:

Isotopes Mass Defect E = mc2

How cold is cold fusion? Janne Wallenius Associate professor Department of Reactor Physics Royal Institute of Technology.

New methods to measure the cross sections of 12 C+ 12 C fusion reaction Xiao Fang Department of Physics University of Notre Dame.

Experimental investigation of stellar 12 C+ 12 C fusion toward extremely low energies by direct and indirect methods Xiao Fang University of Notre Dame.

Mary Beard University of Notre Dame Reaction Rates Calculations in Dense Stellar Matter Frontiers 2005 Aim: To establish a general reaction.

One-proton Breakup of 24 Si and the 23 Al( p, γ ) 24 Si Reaction in Type I X-ray Bursts How can we measure capture cross-sections for 23 Al(p,γ) 24 Si.

Searching for the Low-Energy Resonances in the 12 C( 12 C,n) 23 Mg Reaction Cross Section Relevant for S-Process Nucleosynthesis Brian Bucher University.

1 Reaction Mechanisms with low energy RIBs: limits and perspectives Alessia Di Pietro INFN-Laboratori Nazionali del Sud.

Zagreb IP: Experimental nuclear physics inputs for thermonuclear runaway - NuPITheR Neven Soić, Ru đ er Bošković Institute, Zagreb, Croatia EuroGENESIS.

Heavy flavor production at RHIC Yonsei Univ. Y. Kwon.

Nuclear structure and fundamental interactions Solid state physics Material irradiation Micrometeorite research and study Astrophysics Nuclear astrophysics.

Some aspects of reaction mechanism study in collisions induced by Radioactive Beams Alessia Di Pietro.

Hadron Spectroscopy with high momentum beam line at J-PARC K. Ozawa (KEK) Contents Charmed baryon spectroscopy New experiment at J-PARC.

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

June 16-20, 2005 北京 1 Atsushi Hosaka (RCNP, Osaka Univ) Decay and production of  + hep-ph/ , PRD71: (2005) A. H., M. Oka and T. Shinozaki.

Institute for Structure and Nuclear Astrophysics Nuclear Science Laboratory E381: Search of potential resonances in the 12 C+ 12 C fusion reaction using.

Nuclear Reaction Questions 1.In 1909, what did Ernest Rutherford aim to discover? 2.Describe the equipment set-up he used to carry out his experiment.

Applications of Nuclear Physics

High Resolution Spectroscopy in Nuclear Astrophysics Joachim Görres University of Notre Dame & JINA.

ERNA: Measurement and R-Matrix analysis of 12 C(  ) 16 O Daniel Schürmann University of Notre Dame Workshop on R-Matrix and Nuclear Reactions in Stellar.

Institute for Structure and Nuclear Astrophysics Nuclear Science Laboratory The 12 C+ 12 C fusion reaction at stellar energies Xiaodong Tang (Aggie since.

Fusion of light halo nuclei

Reaction cross sections of carbon isotopes incident on proton and 12 C International Nuclear Physics Conference, Tokyo, Japan June 3-8, 2007 W. Horiuchi.

Determining the rp-Process Flow through 56 Ni 56 Ni is a Waiting Point and imposes a delay Decay Lifetime: 2.3x10^4 s ; Burst Time: 10 – 100 s Largest.

FIVE REGIMES OF NUCLEAR BURNING IN DENSE STELLAR MATTER D.G. Yakovlev Ioffe Physical Technical Institute, St.-Petersburg, Russia Thermonuclear burning.

Notes 42 - Topic 7 - Atomic and Nuclear Physics Artificial.

In this talk Deep crustal heating on accreting neutron stars The fate of accreted matter, and deep crustal heating. NEW: heating is sensitive to composition.

Indirect measurements of the -3 keV resonance in the 13 C(α, n) 16 O reaction: the THM approach Marco La Cognata.

Institute for Structure and Nuclear Astrophysics Nuclear Science Laboratory NPA5 April 7, 2011 Upper limit on the molecular resonance strengths in the.

If the sun is a burning ball of gas … just what gas is it burning? Warmup Question:

Fusion excitation measurement for 20 O + 12 C at E/A = 1-2 MeV Indiana University M.J. Rudolph, Z.Q. Gosser, K. Brown ✼, D. Mercier, S. Hudan, R.T. de.

Bubble Chamber A novel technique for measuring thermonuclear rates at low energies Rashi TalwarAPS April Meeting 2016.

David Mountford University of Edinburgh

the s process: messages from stellar He burning

Direct measurements for nuclear

A few observations on strangeness production at SPS and RHIC

The D(4He,)6Li reaction at LUNA and the Big Bang Nucleosynthesis

Carbon, From Red Giants to White Dwarfs

Tan Ahn, S. Henderson, S. Aguilar, A. Simon, W. P. Tan,

Study of the resonance states in 27P by using

Recoil charge state distributions in 12C(a,g)16O at DRAGON

Elastic alpha scattering experiments

Experiment (Jlab Exp : CLAS eg3)

Chapter 3, Part2 Nuclear Chemistry CHEM 396 by Dr

Presentation transcript:

Does the 12 C+ 12 C fusion reaction ignite superbursts?

Superburst: ignited by Carbon burning Ashes from rp process (He burning) deposit in the outer crust. Crust processes (EC, pycnonuclear fusion)  crust heating  crust conductivity Picture by E. Brown ashes Key problem: the standard rate (CF88) is too low to explain observation!  Disk Companion Neutron star

3x10 16 MeV*b Astrophysical energy range

CF88 T. Spillane et al., Strong resonance at 2.14 MeV with width <12keV; No confirmation yet. PRL98 (2007) ; R. Cooper et al., APJ (2009) 702, 660 Strong resonances at deep sub-barrier energies

24 Mg(a,a’) inelastic Search the possible resonances Direct measurement The exact cross section 12 C+ 13 C 13 C+ 13 C Provide potential to model the smooth behavior 12 C+ 13 C 13 C+ 13 C Provide potential to model the smooth behavior 12 C+ 13 C 13 C+ 13 C 12 C+ 12 C 12 C( 12 C,n) 23 Mg 12 C( 12 C,p) 23 Na 12 C( 12 C,a) 20 Ne 12 C( 12 C, 8 Be) 16 O 12 C( 12 C,a) 20 Ne

NPA5 April 7, MV FN ND 20 e  A 13 C - 2 e  A 13 C 2+ Thick graphite disk Carbon stripping (100 enA) Gas stripping The 12 C+ 13 C experiment ---- Full (Un- gated) ---- Gated 1.37MeV 2.74MeV Ec.m.=2.83 MeV, 1puA*28hr,379 counts Very compact beta counter 12 C( 13 C, 24 Na)p

Eg. for 12 C+ 12 C, (E in MeV) Caltech 1983 Not good for comparing xsec among the three systems 12 C+ 13 C 12 C+ 12 C 13 C+ 13 C

Use the same conversion formula for all the three carbon systems. Good for the comparison of xsecs among the three systems!

Ah ha, 12 C+ 13 C matches with 13 C+ 13 C very well! Each data set (except our data) has additional 15%-30% systematic uncertainty arising from statistical model. The isotope difference (mass, radius) is negligible when Ecm>2.6 MeV. Two carbon isotope systems: 12 C+ 13 C and 13 C+ 13 C 1  b 20 nb 13 C+ 13 C(Trentalange)

Surprise! The 12 C+ 12 C is not enhanced but suppressed! The 12 C+ 12 C resonant xsecs of major resonances matches the xsec of the other two systems: 12 C+ 13 C and 13 C+ 13 C! Why ???? (Good question for the question session!) Three carbon isotope systems: 12 C+ 13 C, 13 C+ 13 C and 12 C+ 12 C xsec(12C+13C) or xsec(13C+13C) : Upper limit for 12C+12C 13 C+ 13 C(Trentalange)

12C+12C 12C+13C 13C+13C Above the Coulomb barrier

Extrapolation with the 12 C+ 12 C resonant cross sections Fit resonant cross sections with ESW (Best upper limit) CC-AW calculation (always over-predict xsecs at low Es, Safe upper limit ) The first quantitative description of the 12 C+ 12 C resonant cross sections! 13 C+ 13 C(Trentalange)

Our theory claims: 12 C+ 13 C (or 13 C+ 13 C)> 12 C+ 12 C The strong resonance at 2.14 MeV: the failure of our empirical relationship ? No confirmation of the 2.14 MeV yet: it may be a mistake in …..? Strong resonance At 2.14 MeV Isotope Systematics Systematics vs. Spillane’s Experiment 13 C+ 13 C(Trentalange)

The preliminary data from the recent experiment at Naples* SUPPORT our finding! No evidence for strange strong resonance! For the Ecm=1.5 MeV resonance: Safe upper limit: 6 x Fowler rate Best estimated upper limit: ~ Fowler rate * Dr. Zickefoose, U. Connecticut thesis, 2011 Systematics wins! Isotope Systematics Strong resonance At 2.14 MeV 13 C+ 13 C(Trentalange)

If the rate can not be that high, there must be some physics missing in the superburst model. Unknown process to heat up the crust to higher temperature. Carbon burning is not the one triggering superbursts! ashes

Notre Dame-ANL-IU fusion experiment A 5 MV Pelletron with ECR source in terminal. Will be installed at the end of Ecm=1.5 MeV Solenoid Spectrometer for Nuclear AstroPhysics (SSNAP)  Silicon Array at Notre Dame (SAND) By comparing with the Naples experiment, our setup will increase yield by two orders of magnitude!

Summary A strong and interesting empirical correlation found among three system: 12 C+ 12 C, 12 C+ 13 C and 13 C+ 13 C. First empirical upper limit rules out the possibility of strong resonances at 1.5 MeV and 2.14 MeV. Impose new constrain on superburst model. With new detector + new accelerator building at ND and 24 Mg( ,  ’) experiment at RCNP, better data will be available soon. There are still many puzzles on the 12 C+ 12 C resonances even this topic is more than 50 years old. Hope we may solve the carbon fusion problem before the next Rutherford conference!

24 Mg