Determination of fragmentation parameters of multicharge component of primary cosmic ray

Gagarin, Yu. F.

Ivanova, N. S.

English

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ST -CR -NP -10656 
DETERMINATION OF THE FRAGMENTATION PARAMETERS 
OF THE MULTI-CHARGE COMPONENT OF PRIMARY COSMIC RAYS 
by ' 
W. F. Gagarin 
N. S. lvanova i 
(USSR) 
c 
13 OCTOBER 1967 
https://ntrs.nasa.gov/search.jsp?R=19670029020 2020-03-24T01:12:58+00:00Z
ST-CR-NP-10656 
DETERMINATION OF THE F R A m A T I O N  PARAMETERS 
OF THE MULTI-CHARGE CCMPONENT OF PRIMARY COSMIC RAYS 
Kosmicheskiye Issledovaniya 
Tom 5, vypusk 3,  450 - 455, 
Izdatel'stvo "NAUKA", 1967. 
by Yu. F. Gagarin 
6 N. S. Ivanova 
S M Y  
The fragmentation parameters of heavy nuclei have been obtained on the 
"hydrogen" emulsion by utilizing nuclear emulsions exposed at 300 lan altitude, 
and sorting the interactions of heavy nuclei of cosmic rays with a number q 1 
of black and gray rays related to target nucleus. 
The possibilities of transition (fragmentation parameters) of nickel nuclei 
to groups H (Z > 10); H, (Z 20 28) ;  H, (Z = 16 + 19); H3 (Z = 10 + 15); 
M (Z  = 6 : 9) and L (Z = 3 f 5 )  were obtained by studying the interactions of 
protons with energy 10 Bev with nuclei of nickel, introduced into the emulsion 
in the form of spherical particles of Q, 9 mlan diameter. 
* 
* * 
One of the fundamental problem of theory of cosmic ray origin is the inter- 
pretation of data on the charge compmition of cosmic rays near Earth. P.t the 
same time, the most essential moment is accoutning of the transformation of 
cosmic radiation's charge composition durinq transit through interstellar gas. 
Such an accounting requires an as precise a knoweldge of fragmentation parame- 
ters Pik as possible (Pi 
forming, as an average, 8uring one interaction of the primary nucleus - i on 
interstellar hydrogen). 
The values of these parameters Pik determine to a significant degree the 
choice of the model of cosmic ray propagation: the quantity of matter traver- 
sed by cosmic radiation to Earth; the charge spectrum of cosmic rays after 
emergence from tile source and others [l] . 
being determined as the number of nuclei of kind - k
Data on fragmentation parameters are very scarce in literature [2  - 61. 
Part iculnrly small are the statistics for the group H (Z % 20). For the group 
t I  (Z 5 10) the total numbcr of cases brought out in literature is less than 100. 
c 
2 
Besides, there exist considerable discrepancies in the values of certain Pik 
in the works of different authors. 
The fragmentation parameters in the hydrogen nuclei may be obtained by two 
methods: a) from analysis of interactions of multi-charge particles of cosmic 
radiation in an emulsion exposed at great height; b) in a mirror system, when 
the various targets (Z = 6 : 28) are irradiated by protons of high energy on 
accelerators. Nearly all the data available in literature have been obtained 
by the first method. Some of the data may be obtained by the second method 
from the work [7]  (for carbon) and computed from radiochmical data [2, 81. 
The determination of the parameters Pik 
priate by both the first and the second methods. In the latter case values 
of Pik might be obtained for the heaviest nuclei of cosmic radiation (VH), 
whose determination by the first method with sufficient precision is difficult. 
appeared to us as being appro- 
DETERMINATION OF Pik IN AN EMULSION 
IRRADIATED BY COSMIC RAYS 
T -  A pellicle stack of 10 x 10 x 10 cm3 dimension, consisting of a t NIKFI-BR relativistic emulsion layers was irradiated during 72  hours at t e 
altitude of 300 km (Kosmos-4). 
charged particles of primary cosmic radiation with nuclei of the emulsion and 
up to 401 such interactions were detected. 
The interactions were investigated of multi- 
All primary multi-charge particles inducing interaction were traced in 
the emulsion prior to entry into the pellicle stack , and all secondary ones 
with Z 
The charge of multi-charge cosmic particles with E > 2 Bev/nucleon was 
determined by the number of &-electrons (ns) corresponding to 100 mkm of the 
path. 
tained for the same emulsion. 
3 - after egress, taking into account all secondary interactions. 
Utilized to that effect was graduated curve of ng dependence on Z, ob- 
Of all the cases investigated 74 interactions could be ascribed to those 
of interest to us, on "hydrogen", inasmuch as the number of gray and black rays 
related to the target-nucleus was respectively 0 and 1. 
Analysis of these cases allowed us to obtain data on fragmentation para- 
ineters Pi  
in Table  f .  
rclative to this group will be presented later. 
of groups H ( Z  % 10) and M ( Z  = 6 : 9) of cosmic radiation compiled 
The statistics relative to the group L so far is small, and data 
nata of other authors were also brought out for the sake of comparison. 
It may be seen that for the group H, the parameters P ~ H ,  FHM, AND pH 
by LIS coincide sufficiently well with the parameters computed from rffe combincd 
data of [2 - 61 (presented in [ 2 ] ) .  
pancy as regards the data on P L. 
data [9] ,  obtained by the dif P erence method on teflon and polyethylene with 
small statistics depart rather strongly from our own results and from those 
of the work [ 2 ] .  
obtained 
However, there is a considerable discre- 
Note at the same time that the Friedlander 
. 
- 
3 
For the group M and within the limits of experimental erros, parameters 
agree with the data of [2] and may be coordinated with the expe- Fjgl and 
rimental results by Frienlander [ 9 ] .  
extent the value brought out in [2]. 
According to our data, PM exceeds to some 
In the following a further refinement of all these parameters is anticipa- 
ted as statistics increase. 
The results of calculations [9, 21, obtained with the utilization of some 
radiochemical data, are compiled in the last two lines of Table 1. 
T A B L E  1 
A u t h o r  
Present work ............. 
A i  zu , Fu j imoto , Hasegava 
et a1 [2]. 
Combined results of [2-61 
. .  .... _ I  I 1 
DETERMINATION OF FRAGME3iTATION PARAMETERS 
- 
Group M (Z =6 I 9) 
FOR THE 
As already noted above, the fragmentation parameters for a specific 
nuclcus may be obtained during the study of interactions oc high energy protons 
with a specific nucleus. The results must not depend on 7,iiich of the colliding 
partners rests. 
We were interested in target-nuclei close in their charge to iron, inasmuch 
3s thcrc are very few parameters Pik o i  the heaviest component of cosmic rays. 
The methods of introduction into the emulsion of specific elements in the 
form of solutions of salts (during the preparation of the emulsion [lo-111 or 
by way of saturation of ready layers) may not be utilized, for they are most 
effective for the elements of the end of the periodical system. 
the fission of nuclei, attending most probably the nuclear reaction, permits a 
good indentification of the target-nucleus and the'detailed investigation of the 
interaction of various particles on these elements 112 - 141. 
In the last case 
4 
Uuring the introduction into the emulsion of specific elements in the 
form of suspension, one may observe the complete pattern of interaction for 
any elements. The possibility of introducing suspensions into the emulsion 
has been indicated in a series of works [15 - 211. 
ters Pik can be obtained only from the work by Zhdanov and Fedotov [7]. 
must be fulfilled, of which two are most essential. 
However, data on parame- 
When charging the emulsion by various elements a series of conditions 
1. The element introduced must not desensitize the emulsion and react 
with revealing and fixing solutions. 
2. A reliable identification of the interaction on the nuclei of the 
element introduced must be guaranteed. 
The second condition defines the requirements relative to the configura- 
tion and the optical properties of the particles introduced. 
presence of a zone of indiscernibility around a particle linked with emulsion 
settling, the identification of interactions on opaque particles with irregu- 
lar shape is very unreliable. (The probability of identification of the inter- 
action is less than 50 percent for particles of 9 m h  transverse dimensions 
and it decreases iapidly as the size of particles decreases). A more reliable 
identification is possible only when the element's particles introduced have 
a regular shape, the spherical one being the optimum case. 
Because of the 
The first condition diminishes significantly the number of elements that 
may be introduced into the emulsion in the region of interest to us, Z(3 5 2 8 ) .  
We investigated the influence on the emulsion of elements introduced in it, 
namely, iron, sulphur and nickel. The introduction of iron disrupts even the 
mechanical properties of the emulsion, without speaking about the sensitivity. 
The introduction into the emulsion of sulphur in the form of balls (spheres) 
leads to the disappearance of relativistic sensitivity in the neighborhood of 
the sphere at a distance of 20 - 30 mkm. Good results have been obtained with 
nickel, whose introduction does not disrupt the basic properties of the emulsion. 
(It should be noted that for the study of the fragmentation parameters Pik of 
heavy nuclei of group W(Z 2 20)'s cosmic rays, it is possible to introduce 
into the emulsion certain brands of stainless steel, of which the composition 
is very near the observed composition of cosmic rays of the group indicated). 
a) Method of Preparation of Layers with Nickel and Identification of 
Tnternctions. 
spark sputtering"(?) [17, 181 in distilled water(*). The mean diameter of 
balls introduced into the emulsion is 9.2 mkm. The scattering by diameter is 
from 5 to 13 mkm. 
the nickel introduced is found to be in one plane in the middle of the layer 
400 r n h  thick. 
The amount of nickel introduced in the layer is 0.2 mg/cm2. 
The nickel balls were prepared by the method of "electric 
Layers with nickel were so prepared that practically all 
This facilitates significantly the survey of the emulsion. 
(*) 'The purity of nickel utilized for sputtering in 99.7% by weight. 
111 connection with water electrolysis during sputtering and the formation of 
litomic oxygen the fonation of oxides is possible. Chemical analysis of the 
powdcr prepared has shown an insignificant admixture of oxygen (less than 0.1% 
hy weight). 
5 
The pellicle stack (chamber) made of 30 layers with nickel NIKFI BR-2 
emulsion (layer dimensions: 10 by 10 cm2, thickenss 400 mkm) was irradiated 
in the internal beam of the synchro-phasitron of the United Institute of 
Nuclear Investigations by protons with energy of 10 Bev in the form of a 
single impulse. The direction of proton flux was parallel to the emulsion 
plane. The variation of flux along the thiclmess bf  the pile was (2.5 + 0.8)- 
106 cm-2. 
. I  
i 
I 
. 1 )  t is optimum. The losses of short-range tracks :ybS'i s'b. The mean diameter of the ball (9.2 mkm) chosen for the introduction into the emulsion, 
paratively small, ( ~3%). On the other hand, 
the ball's diamter decreases. We understand 
in the ball, in which the interaction of the 
incident particle may be identified with a 
probability of 100 percent. The radius of 
than the observed ( 1 mkm is the measurement 
precision of the vertical coordinate in the 
microscope). Interaction of the proton 
splitting is induced by a proton with 10 Rev 
energy only in the case when it takes place 
in the effective volume of the ball and when 
the entering relativistic track of the pro- 
ton is not continuing (the angle with the 
primary direction is greater than 30 min). 
proton track, lying in the emulsion plane, and the geometry of splitting par- 
&: L1L:':s - allow us t o  detem,irie preclseljj the paint of interaction in the giver: 
ball. 
on account of absorption in the ball are com- ** . \ r  i 
volume the number of the of ball interactions is sharply in decreases the ff ctive as + -  \r. 
here by effective volume the sphere's volume .< 
the effective sphere is by one micron less . ' a .  , ' /  . .  . ~ 
F i g .  1 
with energy of 10 Bev with 
the nickel ball 
The ingressing proton is in- 
dicated by the arrow. The 
diameter of the ball is 8.5 mkm 
It was estimated that the nickel nucleus' 
The observation of the entering 
A microphotograph of interaction on the nickel ball, induced by a proton 
of 10 Bev energy, is shown in Fig.1. 
arrow. Of the total number of found interactions on nickel balls (% 700 cases) 
thirty-five percent (35%) of events satisfy the chosen criterion. 
remaining cases the interaction took place either in the superficial layer 
1 mkm thick or was not attended by the entering relativistic track, or still 
the entering relativistic track did not change its direction. 
groups oE interactions were apparently induced by secondary particles (710, T , 
p, nJ, 
emulsion. 
The ingressing proton is shown by the 
In  the 
f 
The last two 
arising from interactions of primary protons with the nuclei of the 
From the numbers brought out it is clear that for the study of splittings 
on suspension particles and at specific energy of incident particles it is 
necessary t o  utilize only the relativistic emulsion. (Follows Table 2). 
T A B L E  2 
ANNOTATION . The values in parentheses were obtained after introduction 
of corrections for the effectiveness of detection of interactions on nickel with 
different number of black and gray rays. 
b) Results o r  Measurements. The review of plates was conducted by areas. 
After careful analysis 255 cases were referred to interactions on nickel nuclei. 
The entering primary proton was registered in each interaction and the number 
of black, gray and thin tracks was determined. Among black tracks all fragments 
with Z z 3 were separated and investigated. 
rays are related to the target-nucleus, and taking into account, according tn 
theory of evaporation, t h e  percentage of a-particles among the evaporative or 
black particles, it was possible to compute for each case the charge of the 
residual nucleus and, consequently, have all the data for the derermination of 
Pik for the given parent nucleus. 
Considering that black and gray 
When determining Pik corrections were introduced, taking into account the 
omission of interactions with small number of gray and black rays ( 62) and the 
sion plane. 
characterizing the transition of the parent nucleus Z = 28 into the group H 
(Z The group H may be divided into 
sub-groups: I i , ( Z  = 20 : 28),  H, (Z  = 16 I 19) and H, (Z = 10 I E), for which 
data can also be obtained. 
di f f icu l t ) )  of identification of gragKznts e s q i z g  a t  mgles  > 60° t o  the e n l -  
We conpiled in Table 2 all the fragmentation parameters measured by us-and 
l o ) ,  M (Z = 6 : 9) and L (Z = 3 : 5) .  
There is no information in literature on the experimental data on Pik pa- 
rameters for  very heavy nuclei (Z > 20). This is why our own data may be only 
compared with the results of calculations by Badhwar et a1 [8] and Aizu et a1 
[ 21 , based upon available radiochemical data. Note the satisfactory agreement 
wuth the Badhwar results [ S I ,  though the latter are quite approximate and they 
utilize the arbitrary assumption on the Constance of Pik, beginning with energy 
of 300 Mev/nucleon. 
In the following works the values of Pik will be utilized at consideration 
of charged spectruni of cosmic rays' transformation. 
7 
In conclusion the authors express their gratitude to N. L. Grigorov, 
I. A. Savenko and D. A. Zhuravlev for their cooperation during the arrange- 
ment of  the experiment. 
Lyubomilov and V. I. Baranov in processing the emulsion piles. 
titude goes also to I. G. Khilyuto, N. N. Kotlov, Z. G. Laptev and L. A. 
Stekol'shchikov for their participation in the cumbersome work of surveying 
the emulsion. 
They also acknowledge the cooperation of s. I. 
Their gra- 
T H E  E N D  
Manuscript received on 
5 September 1966 
CONTlWCT NO. NAS- 5 - 1 248 7 Translated by ANDRE L. BRICHANT 
VOLT TECIINICAL COOPERATION 
1145- 19th St. NW on 12 - 13 October 1967 
WASHINGTON D. C. 20036. 
Telephone : 223-6700 ( Ext. 36, 37) 
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Determination of the Fragmentation Parameters of the Multi-charge Component of Primary Cosmic Rays

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