International conference on particle physics and astrophysics

The first results of analysis of nuclear track emulsion exposed to relativistic nucleus $_{}^{11}C$ and $_{}^{10}B$

6 Oct 2015, 14:30

30m

Milan Hotel 4*

Nuclear physics and particle physics Poster Session I

Description

Featuring an excellent sensitivity and spatial resolution nuclear track emulsion (NTE) maintains the position of a universal and inexpensive detector for survey and exploratory research in microcosm physics. Use of this classical technique on beams of modern accelerators and reactors turns out highly productive. In a number of important tasks the completeness of observations provided in NTE cannot be achieved for electronic detection methods. In particular, in the last decade clustering work of a whole family of light nuclei including radioactive ones was investigated in the processes of dissociation of relativistic nuclei in NTE [1, 2]. Recent data on pattern of diffractive dissociation of the $^{11}C$ and $^{10}B$ will be discussed in this context. It is already established that 144 "white" stars produced by the $^{11}C$ in NTE are distributed over the charge channels in the following way: 2He + 2H (50%), 3He (17%), $^{7}Be$ + He (13%), He + 4H (11%), B+H (5%), Li + He + H (3%), 6H (2%). The distributions of He fragments over the opening angle $\theta_{2He}$ show that $^{8}Be_{g.s}$ decays are presented in 21% 2He + 2H and 19% in the 3He events. These distributions allow one to assume a strong contribution of $^{8}Be_{2+}$ decays but it is a subject of future consideration. The $^{9}B$ nucleus can exist in $^{11}C$ as an independent virtual component or as a component of a virtual basis $^{10}B$. Measurements of the first 21 stars pointed to four decays $^{8}Be_{g.s}$, two of which originated from $^{9}B_{g.s.}$ decays. Measurements of "white" stars $^{10}B$, including identification of He and H isotopes by a multiple scattering method, are in progress now. 1. P.I. Zarubin // Lect. Notes in Phys. 2013 V.875. P.51. 2. K.Z. Mamatkulov et al. // Phys. At. Nucl. 2013 V.76. P.1224.