Impact Parameter Representation for Forward and Backward Scattering of Two Particles

1974 ◽  
Vol 52 (9) ◽  
pp. 830-837 ◽  
Author(s):  
J. M. Allerton ◽  
B. S. Bhakar
Keyword(s):  
Impact Parameter ◽  
High Energy ◽  
Energy Limit ◽  
High Energy Limit ◽  
Energy Shell ◽  
Parameter Representation

The Lippman–Schwinger equation is solved to obtain an impact parameter representation for the forward and backward scattering. The Blankenbecler and Goldberger type amplitude is obtained in the high energy limit without any angular restriction. Then, the off energy shell amplitude in the forward and backward cone is obtained, which reduces to Glauber form on the energy shell. Finally, unitarity restriction and the scope of the formalism are discussed.

HIGH ENERGY LIMIT IN QCD

2011 ◽  
Vol 26 (09) ◽  
pp. 603-623
Author(s):  
ANNA M. STASTO
Keyword(s):  
Inelastic Scattering ◽  
Deep Inelastic Scattering ◽  
Heavy Ion Collisions ◽  
Heavy Ion ◽  
High Energy ◽  
Energy Limit ◽  
High Energy Limit ◽  
Ion Collisions ◽  
Small X

We briefly review some selected topics in the small x physics. In particular, we discuss the progress in the problem related to the resummation at small x and the parton saturation phenomena. Finally we discuss some phenomenological applications to deep inelastic scattering, hadron and heavy ion collisions.

scholarly journals The β-ray spectrum of Ra E

1939 ◽  
Vol 170 (941) ◽  
pp. 190-205 ◽  
Keyword(s):  
Distribution Curve ◽  
High Energy ◽  
Energy Limit ◽  
Total Change ◽  
High Energy Limit ◽  
Nuclear Collisions ◽  
The Past ◽  
Low Energy Electrons ◽  
Energy Distribution Curve ◽  
Chamber Measurements

Interest in the continuous β-ray spectrum has been revived during the past few years by the discovery of induced β-ray activity and the difficulty which has been experienced in incorporating an account of the phenomenon in the theory of the nucleus. Attention has been focused on two features of the spectrum: the high-energy limit, the accurate measurement of which yields the total change in nuclear energy associated with the β disintegration, and the form of the energy distribution curve, which is discriminative in theories of the β-ray emission process. Owing to the convenience of R aE as a source, the β-ray spectrum of this element has received considerable attention, and a comprehensive table of previous work published in a recent paper by O’Conor (1937) shows that recent values of the high-energy limit obtained with magnetic spectrometers are in fair agreement. The form of the R aE spectrum, however, is still not known with any certainty. This can be made clear with the help of Table I, which sets out the results and significant experimental details of the work carried out since 1935 with magnetic spectrometers. Some recent work with cloud expansion chambers is not included because the results are rather discordant. With the relatively low energy electrons of R aE and the high probability of nuclear collisions in the chamber, measurements of the energies of the β-particles are extremely difficult, and the results are probably not as reliable as those obtained with magnetic spectrometers.

scholarly journals PROBING HIGH ENERGY PROPERTY OF STRING SCATTERING BY EFFECTIVE FIELD THEORY

2013 ◽  
Vol 21 ◽  
pp. 153-154
Author(s):  
CHUAN-TSUNG CHAN ◽  
SHOICH KAWAMOTO ◽  
DAN TOMINO
Keyword(s):  
Field Theory ◽  
Effective Field Theory ◽  
Open String ◽  
High Energy ◽  
Effective Field ◽  
Energy Limit ◽  
High Energy Limit ◽  
Linear Relations ◽  
Massive Spin ◽  
Symmetry Structure

It is known that infinitely many linear relations among string scattering amplitudes appear in high energy limit. These linear relations would imply a symmetry structure that is not manifest before taking the high energy limit. Motivated by this observation, we study an effective field theory of massive spin-2 and spin-1 particles, and try to understand what kind of structure reproduces the linear relations among the amplitudes of bosonic open string.

Observational constraints on reheating in braneworld inflation

2019 ◽  
Vol 34 (27) ◽  
pp. 1950152
Author(s):  
Z. Sakhi ◽  
A. Safsafi ◽  
M. Ferricha-Alami ◽  
H. Chakir ◽  
M. Bennai
Keyword(s):  
Cosmological Parameters ◽  
High Energy ◽  
Observational Constraints ◽  
Brane Tension ◽  
Energy Limit ◽  
Polynomial Potential ◽  
High Energy Limit ◽  
Slow Roll ◽  
Braneworld Inflation ◽  
Best Fit

The reheating era after inflation is analyzed in the framework of the braneworld models. We study reheating by calculating the reheating temperature in a braneworld inflation for various cosmological parameters. The variation of reheating [Formula: see text]-folding number and reheating temperature were obtained and analyzed as function of a spectrum of perturbation for a polynomial potential [Formula: see text]. We have applied the slow-roll approximation in the high energy limit to constraint the parameter potentials by confronting our results to recent Planck 2018 observations. We have shown that in general the best values of the predicted reheating temperature is of the order [Formula: see text] GeV, with a brane tension [Formula: see text] GeV4. We have also shown that the polynomial potential in the case [Formula: see text] provides the best fit results with recent observational constraints.

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