Carl A. Gagliardi

Search for the lepton family number nonconserving decay mu+ ---> e+ gamma

The MEGA experiment, which searched for the muon- and electron-number violating decay μ +→e + γ, is described. The spectrometer system, the calibrations, the data taking procedures, the data analysis, and the sensitivity of the experiment are discussed. The most stringent upper limit on the branching ratio, B(μ + →e + γ)l1.2×10 -11 with 90% confidence, is derived from a likelihood analysis.

Tests of transfer reaction determinations of astrophysical S factors

The {sup 16}O({sup 3}He,d){sup 17}F reaction has been used to determine asymptotic normalization coefficients for transitions to the ground and first excited states of {sup 17}F. The coefficients provide the normalization for the tails of the overlap functions for {sup 17}F{r_arrow}{sup 16}O+p and allow us to calculate the {ital S} factors for {sup 16}O(p,{gamma}){sup 17}F at astrophysical energies. The calculated {ital S} factors are compared to measurements and found to be in very good agreement. This provides a test of this indirect method to determine astrophysical direct capture rates using transfer reactions. In addition, our results yield S(0) for capture to the ground and first excited states in {sup 17}F, without the uncertainty associated with extrapolation from higher energies. {copyright} {ital 1999} {ital The American Physical Society}

Asymptotic normalization coefficients for B-8 ---> Be-7 + p from a study of Li-8 ---> Li-7 + n

Asymptotic normalization coefficients (ANCs) for 8Li->7Li+n have been extracted from the neutron transfer reaction 13C(7Li,8Li)12C at 63 MeV. These are related to the ANCs in 8B->7Be+p using charge symmetry. We extract ANCs for 8B that are in very good agreement with those inferred from proton transfer and breakup experiments. We have also separated the contributions from the p_1/2 and p_3/2 components in the transfer. We find the astrophysical factor for the 7Be(p,gamma)8B reaction to be S_17(0)=17.6+/-1.7 eVb. This is the first time that the rate of a direct capture reaction of astrophysical interest has been determined through a measurement of the ANCs in the mirror system.

Scattering of Be-7 and B-8 and the astrophysical S(17) factor

tension of the angular range was done to obtain a better determination of the optical potential in the incoming channel. We also measured the elastic scattering of a 8 B beam on a C target with the aim of checking, for the first time, the OMP that were used in the outgoing channel 8 B+ 13 C. Below we describe the radioactive beam production, the experimental setups, and the procedure for the data reduction. We then give results of calculations for optical potentials in both the incoming and outgoing channels based on a double folding procedure with an effective nucleon-nucleon interaction. We discuss the consequences of the improved secondary beam normalization, and compare revised DWBA calculations to the 14 N( 7 Be, 8 B) 13 C data from Ref. [10] in order to extract a new value for the ANCs and the corresponding astrophysical factor S17.

Breakup of B-8 and the S-17 astrophysical factor reexamined

Existing experimental data for the breakup of

Construction of the MEGA photon detector

^{8}\mathrm{B}

Results of R&D on a new construction technique for W/ScFi Calorimeters

at energies from 30 to

Asymptotic normalization coefficient and important astrophysical process 15N(p,γ)160

1000\phantom{\rule{0.3em}{0ex}}\text{MeV}∕\text{nucleon}

Jet Production in Polarized pp Collisions at RHIC

on light through heavy targets are analyzed in detail in terms of an extended Glauber model. The predictions of the model are in excellent agreement with independent reaction data (reaction cross sections and parallel momentum distributions for corelike fragments). Final-state interactions have been included in the Coulomb dissociation component. We extract asymptotic normalization coefficients (ANC) from which the astrophysical factor

TWIST- The TRIUMF weak interaction symmetry test the Michel parameters from μ+ decay

{S}_{17}(0)