8364889
Determination of the cross sections for the production of fragments from relativistic nucleus-nucleus interactions. II. Parametric fits.
11658466
Cosmic ray isotopes
Since this is the first rapporteur talk on cosmic ray isotopes 
in thirteen Cosmic Ray Conferences, I will begin by 
briefly summarizing our interest in isotopic composition 
as follows: 
a) Isotopes, not elements, are the result of various 
nucleosynthesis processes. Thus, we must know the 
isotopic composition of cosmic rays in order to 
adequately exploit the relationship of cosmic rays 
and stellar processes. 
b) Isotopes, not elements, are the result of secondary 
fragmentation processes, either in cosmic ray 
source regions or in the interstellar medium. 
Thus, we must know the isotopic composition in 
order to completely unravel source composition 
from secondary composition. 
c) Isotopes, not elements, are radioactive. Thus, 
we must know the isotopic composition in order to 
take full advantage of various radioactive nuclei 
as cosmic ray clocks which can be used to determine 
the age of cosmic rays. 
With this short summary, I now turn to a brief review of 
the results presented at this conference. Since I can't 
possibly discuss each new measurement, I have chosen the 
following topics: I) Hand He isotopes, II) Be isotopes, 
III) Al isotopes, IV) Fe isotopes, V) cross sections and 
model calculations, and VI) instrumental considerations.
117760493
The Elemental Abundance Ratios of Interstellar Secondary and Primary Cosmic Rays
The rigidity dependence of the ratios. of abundances of interstellar 
secondary and primary cosmic rays contains important 
information on their confinement and propagation in the Galaxy. 
Recent results suggest that high energy cosmic rays (> 20 GeV/nucleon) 
have propagated through much less interstellar matter than 
lower energy nuclei (< 1 GeV/nucleon). We report new observations 
of abundances in the charge range 2 ≤ Z ≤ 10, which were obtained 
with a dE/dx-Cerenkov detector launched into a polar orbit on OGO-6 
as part of the Caltech Solar and Galactic Cosmic Ray Experiment. 
Integral rigidity spectra of all the elements observed have shapes 
similar to that of the helium spectrum in the rigidity range ~ 2 
to ~ 14 GV, approaching a power law with exponent -1.6 above 8 GV. 
Calculations of interstellar propagation assuming a steady-state 
model and including the presence of interstellar helium and the 
effects of solar modulation predict a variation with rigidity of 
ratios such as Be/O and B/O, which is not observed. The data can 
be explained by assuming a rigidity-dependent confinement of 
cosmic rays within the Galaxy.
16029184
The effects of a local interstellar magnetic field on voyager 1 and 2 observations
We show that an interstellar magnetic field can produce a north-south asymmetry in the solar wind termination shock. Using Voyager 1 and 2 measurements, we suggest that the angle α between the interstellar wind velocity and the magnetic field is 30° < α < 60°. The distortion of the shock is such that termination shock particles could have streamed outward along the spiral interplanetary magnetic field connecting Voyager 1 to the shock when the spacecraft was within ~2 AU of the shock. The shock distortion is larger in the southern hemisphere, and Voyager 2 could be connected to the shock when it is within ~5 AU of the shock, but with particles from the shock streaming inward along the field. Tighter constraints on the interstellar magnetic field should be possible when Voyager 2 crosses the shock in the next several years.
121487391
Cosmic-ray negatron and positron spectra between 12 and 220 Mev.
The interplanetary negatron and positron spectra from 12 to 220 MeV have been determined with a balloon-borne magnetic spectrometer. The observed charge ratio e^+(e^+ + e^−)≈0.3 indicates that the flux most likely consists of a mixture of "primary" negatrons and interstellar "secondary" negatrons and positrons. We deduce an absolute solar modulation of the interstellar positron flux which decreases with decreasing magnetic rigidity below about 80 MV.
122267950
The UH-nuclei cosmic ray detector on the third high energy astronomy observatory
The third High Energy Astronomy Observatory satellite (HEAO-3) carries a particle telescope for the detection of highly charged cosmic ray nuclei. These nuclei, which have Z ≳ 28, are much rarer than the lower charged nuclei in the cosmic radiation. As a consequence, this particle telescope was required to have a large collecting area as well as an ability to resolve individual elements. This paper describes the telescope, composed of large area parallel plate ionization chambers, multiwire ion chamber hodoscopes and a Cherenkov radiation detector. The resulting telescope has a total geometry factor of 59,000 cm^2 sr and is capable of measuring the charges of nuclei in the range 14 ≲ Z ≲ 120.
9087449
Study of pi + pi - transitions from the Upsilon (3S) and a search for the hb.
We have investigated the transitions Y(3S)~m+vr Y(1S), Y(3S)~~+~ Y(2S) and the cascade process Y(3S)~Y(2S)+X,Y(2S)~m+w Y(1S), both in the exclusive decay mode, with the daughter Y state decaying into two leptons, and in the inclusive decay mode, with the daughter Y state decaying hadronically. Results are presented on the branching fractions and properties of the system. The m+ ~ invariant-mass spectra for the decays Y( 3S)~~+ m Y( 1S) and Y(3S)~m ~ Y(2S) are measured and compared with theoretical predictions. We also present the results of a search for the h&(1 'P, ) and Y(1 'D) states in inclusive Y(3S) decays, and for the ex
23950285
Coherent-state path integrals and the bosonization of chiral fermions.
By using coherent-state path integrals I provide a derivation of a two-dimensional chiral boson action which is equivalent to a free Weyl fermion.
35372756
Inclusive B-meson decays into charm.
We have measured the B-meson decay fractions into D/sup 0/, D/sup +/, and D/sup *//sup +/ mesons to be 0.39 +- 0.05 +- 0.04, 0.17 +- 0.04 +- 0.04, and 0.22 +- 0.04/sub -0.04//sup +0.07/, respectively, if we use the D/sup 0/..-->..K/sup -/..pi../sup +/ and D/sup +/..-->..K/sup -/..pi../sup +/..pi../sup +/ branching ratios determined by the Mark III Collaboration. These results suggest that B decay to noncharm final states is substantial. We also find that B decay to spin-1 D/sup */ mesons dominates over direct decay to spin-0 D mesons and that the ratio (D/sup 0/+D/sup *//sup 0/)/(D/sup +/+D/sup *//sup +/) is consistent with unity.
11439667
Schur functions, chiral bosons, and the quantum-Hall-effect edge states.
I demonstrate how the many-body wave function may be used to describe the bosonization of the edge excitations of a droplet of \ensuremath{\nu}=1 quantum-Hall liquid. In particular, I exhibit an isomorphism between the charge-neutral edge-state excitations of the droplet and the space of universal symmetric polynomials. There are two natural bases for this space; the first, the Schur functions, correspond to the fermion picture; the second, generated by the power sums, yields the Bose picture and the Kac-Moody algebra. I also show explicitly how the loop group LU(1) acts to create the coherent-state deformations of the droplet shape used in path-integral bosonization and in the quantization of chiral bosons.
33893527
Edge waves in the quantum Hall effect and quantum dots.
We have studied numerically the spectrum of low-energy excitations for quantum dots containing up to 400 electrons near densities corresponding to the quantum-Hall-effect filling fraction \ensuremath{\nu}=1. The results show that, despite strong Coulomb interaction effects, the edge modes are well described as weakly interacting chiral boson edge waves.