212 research outputs found
Deformations of calibrated subbundles of Euclidean spaces via twisting by special sections
We extend the "bundle constructions" of calibrated submanifolds, due to
Harvey--Lawson in the special Lagrangian case, and to
Ionel--Karigiannis--Min-Oo in the cases of exceptional calibrations, by
"twisting" the bundles by a special (harmonic, holomorphic, parallel) section
of a complementary bundle. The existence of such deformations shows that the
moduli space of calibrated deformations of these "calibrated subbundles"
includes deformations which destroy the linear structure of the fibre.Comment: 16 pages, no figures. Version 2: Only minor cosmetic and
typographical revisions. To appear in "Annals of Global Analysis and
Geometry.
The space of hyperkähler metrics on a 4-manifold with boundary
Let X be a compact 4-manifold with boundary. We study the space of hyperk¨ahler
triples ω1, ω2, ω3 on X, modulo diffeomorphisms which are the identity on the boundary. We
prove that this moduli space is a smooth infinite-dimensional manifold and describe the tangent
space in terms of triples of closed anti-self-dual 2-forms. We also explore the corresponding
boundary value problem: a hyperk¨ahler triple restricts to a closed framing of the bundle of
2-forms on the boundary; we identify the infinitesimal deformations of this closed framing that
can be filled in to hyperk¨ahler deformations of the original triple. Finally we study explicit
examples coming from gravitational instantons with isometric actions of SU(2)
Measurement of the 18Ne(a,p_0)21Na reaction cross section in the burning energy region for X-ray bursts
The 18Ne(a,p)21Na reaction provides one of the main HCNO-breakout routes into
the rp-process in X-ray bursts. The 18Ne(a,p_0)21Na reaction cross section has
been determined for the first time in the Gamow energy region for peak
temperatures T=2GK by measuring its time-reversal reaction 21Na(p,a)18Ne in
inverse kinematics. The astrophysical rate for ground-state to ground-state
transitions was found to be a factor of 2 lower than Hauser-Feshbach
theoretical predictions. Our reduced rate will affect the physical conditions
under which breakout from the HCNO cycles occurs via the 18Ne(a,p)21Na
reaction.Comment: 5 pages, 3 figures, accepted for publication on Physical Review
Letter
Octupole transitions in the 208Pb region
The 208Pb region is characterised by the existence of collective octupole states.
Here we populated such states in 208Pb + 208Pb deep-inelastic reactions. γ-ray angular
distribution measurements were used to infer the octupole character of several E3 transitions.
The octupole character of the 2318 keV 17− → 14+ in 208Pb, 2485 keV 19/2
− → 13/2
+ in
207Pb, 2419 keV 15/2
− → 9/2
+ in 209Pb and 2465 keV 17/2
+ → 11/2
− in 207Tl transitions was
demonstrated for the first time. In addition, shell model calculations were performed using two
different sets of two-body matrix elements. Their predictions were compared with emphasis on
collective octupole states.This work is supported by the Science and Technology Facilities Council
(STFC), UK, US Department of Energy, Office of Nuclear Physics, under Contract No. DEAC02-06CH11357
and DE-FG02-94ER40834, NSF grant PHY-1404442
The abundance of 44Ti in core collapse supernovae : Measuring the 44Ti(α, p)47V reaction
Publisher PD
Study of the Ti-44(alpha, p)V-47 reaction and implications for core collapse supernovae
Peer reviewe
Spectroscopy of Na: Bridging the two-proton radioactivity of Mg
The unbound nucleus Na, the intermediate nucleus in the two-proton
radioactivity of Mg, was studied by the measurement of the resonant
elastic scattering reaction Ne(p,Ne)p performed at 4 A.MeV.
Spectroscopic properties of the low-lying states were obtained in a R-matrix
analysis of the excitation function. Using these new results, we show that the
lifetime of the Mg radioactivity can be understood assuming a sequential
emission of two protons via low energy tails of Na resonances
Decay properties of resonances and their impact on -process nucleosynthesis
The astrophysical -process is one of the two main processes forming
elements heavier than iron. A key outstanding uncertainty surrounding
-process nucleosynthesis is the neutron flux generated by the
reaction during the He-core
and C-shell burning phases of massive stars. This reaction, as well as the
competing reaction, is
not well constrained in the important temperature regime from --~GK, owing to uncertainties in the nuclear properties of resonances
lying within the Gamow window. To address these uncertainties, we have
performed a new measurement of the reaction in inverse kinematics, detecting the outgoing
deuterons and recoils in coincidence. We have
established a new decay branching ratio of for the key
MeV resonance in , which results in a new
strength for this resonance of eV when combined with
the well-established strength of this resonance. We have
also determined new upper limits on the partial widths of
neutron-unbound resonances at , , and
MeV. Monte-Carlo calculations of the stellar and rates, which incorporate these results, indicate
that both rates are substantially lower than previously thought in the
temperature range from --~GK.Comment: 17 pages, 4 figures, accepted for publication in Phys. Lett.
Spectroscopy of P 30 and the abundance of Si 29 in presolar grains
The astrophysical Si29(p,γ) reaction is expected to play a key role in determining the final Si29 yields ejected in nova explosions. Such yields are used to accurately identify the stellar origins of meteoritic stardust and recently, distinctive silicon isotopic ratios have been extracted from a number of presolar grains. Here, the light-ion Si28(He3,p) fusion-evaporation reaction was used to populate low-spin proton-unbound excited states in the nucleus P30 that govern the rate of the astrophysical Si29(p,γ) reaction. In particular, γ decays were observed from resonances up to Er=500keV, and key resonances at 217 and 315 keV have now been identified as 2+ and 2-levels, respectively. The present paper provides the first estimate of the 217-keV resonance strength and indicates that the strength of the 315-keV resonance, which dominates the rate of the Si29(p,γ) reaction over the entire peak temperature range of oxygen-neon novae, is higher than previously expected. As such, the abundance of Si29 ejected during nova explosions is likely to be less than that predicted by the most recent theoretical models
Direct Measurement of the Key e c. m.=456 keV Resonance in the Astrophysical Ne 19 (p,γ) Na 20 Reaction and Its Relevance for Explosive Binary Systems
We have performed a direct measurement of the Ne19(p,γ)Na20 reaction in inverse kinematics using a beam of radioactive Ne19. The key astrophysical resonance in the Ne19+p system has been definitely measured for the first time at Ec.m.=456-2+5 keV with an associated strength of 17-5+7 meV. The present results are in agreement with resonance strength upper limits set by previous direct measurements, as well as resonance energies inferred from precision (He3, t) charge exchange reactions. However, both the energy and strength of the 456 keV resonance disagree with a recent indirect study of the Ne19(d, n)Na20 reaction. In particular, the new Ne19(p,γ)Na20 reaction rate is found to be factors of ∼8 and ∼5 lower than the most recent evaluation over the temperature range of oxygen-neon novae and astrophysical x-ray bursts, respectively. Nevertheless, we find that the Ne19(p,γ)Na20 reaction is likely to proceed fast enough to significantly reduce the flux of F19 in nova ejecta and does not create a bottleneck in the breakout from the hot CNO cycles into the rp process
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