Shell - model studies of the astrophysical rp reaction 29 P ( p , γ ) 30

نویسندگان

  • W. A. Richter
  • Alex Brown
چکیده

W. A. Richter1,2,* and B. Alex Brown3 1iThemba LABS, P. O. Box 722, Somerset West 7129, South Africa 2Department of Physics, University of the Western Cape, Private Bag X17, Bellville 7535, South Africa 3Department of Physics and Astronomy, and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824-1321, USA (Received 19 February 2013; revised manuscript received 2 May 2013; published 25 June 2013)

برای دانلود رایگان متن کامل این مقاله و بیش از 32 میلیون مقاله دیگر ابتدا ثبت نام کنید

ثبت نام

اگر عضو سایت هستید لطفا وارد حساب کاربری خود شوید

منابع مشابه

Determining the rp-process flow through 56Ni: resonances in 57Cu(p,γ)58Zn identified with GRETINA.

An approach is presented to experimentally constrain previously unreachable (p, γ) reaction rates on nuclei far from stability in the astrophysical rp process. Energies of all critical resonances in the (57)Cu(p,γ)(58)Zn reaction are deduced by populating states in (58)Zn with a (d, n) reaction in inverse kinematics at 75 MeV/u, and detecting γ-ray-recoil coincidences with the state-of-the-art ...

متن کامل

Proton Capture Cross Section of Sr Isotopes and Their Importance for Nucleosynthesis of Proton-rich Nuclides Typeset Using Revt E X 2

The (p,γ) cross sections of three stable Sr isotopes have been measured in the astrophysically relevant energy range. These reactions are important for the p-process in stellar nucleosynthesis and, in addition, the reaction cross sections in the mass region up to 100 are also of importance concerning the rp-process associated with explosive hydrogen and helium burning. It is speculated that thi...

متن کامل

Photon-induced Reactions in Stars and in the Laboratory: A Critical Comparison

Photon-induced reactions during the astrophysical p(or γ-) process occur at typical temperatures of 1.8 ≤ T9 ≤ 3.3. Experimental data of (γ,n), (γ,p), or (γ,α) reactions – if available in the relevant energy region – cannot be used directly to measure astrophysical (γ,n), (γ,p), or (γ,α) reaction rates because of the thermal excitation of target nuclei at these high temperatures. Usually, stati...

متن کامل

THE ASTROPHYSICAL S-FACTOR OF THE REACTION Be(p,γ)B IN THE DIRECT CAPTURE MODEL

The astrophysical S-factor for the reaction Be(p,γ)B up to an energy of 2 MeV (c.m.) and the capture cross section of Li(n,γ)Li up to 1 MeV (c.m.) are calculated using the Direct Capture model (DC). Both calculations are in good agreement with experimental data.

متن کامل

The astrophysical rate of O(α,γ)Ne via recoil-decay tagging and its implications for nova nucleosynthesis

The O(α,γ)Ne reaction is one of two known routes for breakout from the hot CNO cycles into the rp process. Its astrophysical rate depends on the decay properties of excited states in Ne lying just above the O + α threshold. We have measured the α-decay branching ratios for these states using the p(Ne,t)Ne reaction at 43 MeV/u. Combining our branching ratio measurements with previous determinati...

متن کامل

ذخیره در منابع من


  با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید

عنوان ژورنال:

دوره   شماره 

صفحات  -

تاریخ انتشار 2013