Observation of the Astrophysically Important 3[sup +] State in N[number sign]^{18e via Elastic Scattering of a Radioactive F[number sign]17 Beam from H[number sign]1}

Journal Article · Thu Jul 01 00:00:00 EDT 1999 · Physical Review Letters

DOI:https://doi.org/10.1103/PhysRevLett.83.45· OSTI ID:6469840

Bardayan, D W; Blackmon, J C; Hansper, V Y; Ma, Z; Pierce, D E; Rabban, M T; Smith, M S ^[1]; Bardayan, D W; Chen, A A; Parker, P D; Swartz, K B; Visser, D W ^[2]; Brune, C R; Champagne, A E; Hansper, V Y ^[3]; Cox, J M; Johnson, B A; Kozub, R L ^[4]; Davinson, T; Shotter, A C ; Woods, P J ^[5]; Hofstee, M A ^[6]; Ma, Z ^[7]

---

1. Physics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831 (United States)
2. A. W. Wright Nuclear Structure Laboratory, Yale University, New Haven, Connecticut 06511 (United States)
3. Department of Physics and Astronomy, University of North Carolina, Chapel Hill, North Carolina 27599 (United States)
4. Physics Department, Tennessee Technological University, Cookeville, Tennessee 38505 (United States)
5. Department of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ (United Kingdom)
6. Department of Physics, Colorado School of Mines, Golden, Colorado 80401 (United States)
7. Chinese Institute for Atomic Energy, Beijing, 102413, People's Repub

The [sup 17]F( p,thinsp[gamma])[sup 18]Ne reaction is important in stellar explosions, but its rate has been uncertain because of an expected 3[sup +] state in [sup 18]Ne that has never been conclusively observed. This state would provide a strong [ell]=0 resonance and, depending on its excitation energy, could dominate the stellar reaction rate. We have observed this missing 3[sup +] state by measuring the [sup 1]H( [sup 17]F,thinspp) [sup 17]F excitation function with a radioactive [sup 17]F beam at the ORNL Holifield Radioactive Ion Beam Facility. We find that the state lies at a center-of-mass energy of E[sub r]=599.8[plus minus]1 .5[sub stat][plus minus]2.0[sub sys] keV (E[sub x]=4523.7[plus minus] 2.9 keV) and has a width of [Gamma]=18[plus minus]2[sub stat][plus minus]1[sub sys] keV . [copyright] [ital 1999] [ital The American Physical Society]

• DOE Contract Number: AC05-96OR22464; FG02-91ER40609
• OSTI ID: 6469840
• Journal Information: Physical Review Letters, Vol. 83:1; ISSN 0031-9007
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC X-RAY BURSTS
ELASTIC SCATTERING
FLUORINE
FLUORINE 17
NEON
NEON 18
NOVAE
PROTON REACTIONS
STELLAR ACTIVITY
SUPERNOVAE
BARYON REACTIONS
BETA DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
CHARGED-PARTICLE REACTIONS
COSMIC RADIATION
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
ELEMENTS
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
FLUIDS
FLUORINE ISOTOPES
GASES
HADRON REACTIONS
HALOGENS
IONIZING RADIATIONS
ISOTOPES
LIGHT NUCLEI
MINUTES LIVING RADIOISOTOPES
NEON ISOTOPES
NONMETALS
NUCLEAR REACTIONS
NUCLEI
NUCLEON REACTIONS
ODD-EVEN NUCLEI
PRIMARY COSMIC RADIATION
RADIATIONS
RADIOISOTOPES
RARE GASES
SCATTERING
SECONDS LIVING RADIOISOTOPES
STARS
VARIABLE STARS
663430* - Nucleon-Induced Reactions & Scattering- (1992-)
661300 - Other Aspects of Physical Science- (1992-)