Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV
The ³⁶S(p,γ) ³⁷Cl reaction was investigated in the proton energy range Ep=1975-2190 keV. The observed resonance strengths were evaluated. The γ-decay schemes of the resonances at Ep=2037, 2058, 2069, 2080, 2122 and 2165 keV were constructed and the total γ-widths were determined. The astrophysical...
Saved in:
| Published in: | Вопросы атомной науки и техники |
|---|---|
| Date: | 2009 |
| Main Authors: | , , , , , , |
| Format: | Article |
| Language: | English |
| Published: |
Національний науковий центр «Харківський фізико-технічний інститут» НАН України
2009
|
| Online Access: | https://nasplib.isofts.kiev.ua/handle/123456789/96397 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| Journal Title: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Cite this: | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV / A.N. Vodin1, I.V. Ushakov, G.K. Khomyakov, G.E. Tuller, L.P. Korda, I.A. Shapoval, A.V. Tertichnyi // Вопросы атомной науки и техники. — 2009. — № 5. — С. 12-16. — Бібліогр.: 11 назв. — англ. |
Institution
Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1859640511633031168 |
|---|---|
| author | Vodin, A.N. Ushakov, I.V. Khomyakov, G.K. Tuller, G.E. Korda, L.P. Shapoval, I.A. Tertichnyi, A.V. |
| author_facet | Vodin, A.N. Ushakov, I.V. Khomyakov, G.K. Tuller, G.E. Korda, L.P. Shapoval, I.A. Tertichnyi, A.V. |
| citation_txt | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV / A.N. Vodin1, I.V. Ushakov, G.K. Khomyakov, G.E. Tuller, L.P. Korda, I.A. Shapoval, A.V. Tertichnyi // Вопросы атомной науки и техники. — 2009. — № 5. — С. 12-16. — Бібліогр.: 11 назв. — англ. |
| collection | DSpace DC |
| container_title | Вопросы атомной науки и техники |
| description | The ³⁶S(p,γ) ³⁷Cl reaction was investigated in the proton energy range Ep=1975-2190 keV. The observed resonance strengths were evaluated. The γ-decay schemes of the resonances at Ep=2037, 2058, 2069, 2080, 2122 and 2165 keV were constructed and the total γ-widths were determined. The astrophysical ³⁶S(p,γ) ³⁷Cl reaction rate was estimated.
Представлено результати дослiджень реакцiї ³⁶S(p,γ) ³⁷Cl в областi енергiй протонiв
Ep=1975...2190 кеВ. Оцiнено сили спостережуваних резонансiв. Побудовано схеми розпаду резо-
нансiв при Ep=2037, 2058, 2069, 2080, 2122 та 2165 кеВ. Розрахованi повнi радiацiйнi ширини розпаду резонансiв. Проведено оцiнку швидкостi астрофiзичної реакцiї ³⁶S(p,γ) ³⁷Cl.
Представлены результаты исследований реакции ³⁶S(p,γ) ³⁷Cl в области энергий протонов
Ep=1975...2190 кэВ. Оценены силы наблюдаемых резонансов. Построены схемы распада резонансов
при Ep=2037, 2058, 2069, 2080, 2122 и 2165 кэВ. Рассчитаны полные радиационные ширины распада резонансов. Проведена оценка скорости астрофизической реакции ³⁶S(p,γ) ³⁷Cl.
|
| first_indexed | 2025-12-07T13:21:23Z |
| format | Article |
| fulltext |
INVESTIGATION OF
THE ASTROPHYSICAL 36S(p,γ)37Cl REACTION
AT Ep=1975...2190 keV
A.N. Vodin1∗, I.V. Ushakov1, G.K. Khomyakov1, G.E. Tuller1,
L.P. Korda1, I.A. Shapoval1,2, A.V. Tertichnyi1,2
1National Science Center “Kharkov Institute of Physics and Technology”, 61108, Kharkov, Ukraine
2V.N. Karazin Kharkov National University, Kharkov, Ukraine
(Received July 15, 2009)
The 36S(p,γ)37Cl reaction was investigated in the proton energy range Ep=1975-2190 keV. The observed resonance
strengths were evaluated. The γ-decay schemes of the resonances at Ep=2037, 2058, 2069, 2080, 2122 and 2165 keV
were constructed and the total γ-widths were determined. The astrophysical 36S(p,γ)37Cl reaction rate was estimated.
PACS: 24.30.-v, 25.40.Lw, 25.70.Ef, 25.70.Gh
1. INTRODUCTION
The experimental determination of nuclear reaction
effective cross-sections, which are necessary for the
creation of model representations of nucleosynthesis
in the process of stellar evolution, is one of the main
problems of astrophysics.
Special attention has been recently paid to the
problem of the rare isotope 36S (0.017%) generation
[1]. It is known [2],[3], that one of the sources is
the 36Cl(n,p)36S reaction, which goes through the
compound 37Cl nucleus. However, the data on spins
J and total radiation widths Γγ are missing for most
of the neutron resonances, which makes it impossible
to carry out a qualitative analysis of the resonance
curve shape observed in the 36Cl(n,p)36S reaction.
Meanwhile, the missing information on neutron res-
onances can be obtained with the help of additional
measurements that lead to the same compound 37Cl
nucleus (see Fig.1).
Fig.1. The 37Cl level scheme in the 36Cl(n,p)37Cl, 36Cl(n,α)33P and 36S(p,γ)37Cl reactions
∗Corresponding author. E-mail address: vodin@kipt.kharkov.ua
12 PROBLEMS OF ATOMIC SCIENCE AND TECHNOLOGY, 2009, N5.
Series: Nuclear Physics Investigations (52), p.12-16.
It appears from the experimental data [4], that
37Cl excited levels can be observed both in the
36Cl(n,p)36S reaction and in the 36S(p,γ)37Cl reac-
tion. In this context a series of researches was car-
ried out. The excitation function of the 36S(p,γ)37Cl
reaction was studied in the proton energy range
Ep =1975...2190 keV, which corresponds to excita-
tion of neutron resonances in the 36Cl(n,p)36S reac-
tion in En =0.5...250 keV (see Table 1). As a result,
we determined the energy positions and strengths S
of resonances observed in the specified range of pro-
ton energies. The γ-decay schemes of the most in-
tensive resonances at Ep=2037, 2058, 2069, 2080,
2122 and 2165 keV were constructed and the total
γ-widths were determined. Taking into account the
obtained data on the strengths, the astrophysical
36Cl(n,p)36S reaction rate was estimated.
Table 1. Resonances in the 36Cl(n,p)36S and 36S(p,γ)37Cl reactions
No. 36Cl(n,p)36S 36S(p,γ)37Cl
En, eV E∗, keV Ep, keV E∗, keV 2Jπ S, eV Γγ , eV
1 931(1) 10311.9 - - 1+
2 1341(2) 10312.3 1979.5 10312.3 (3,5)− 1.0 (0.3,0.2)
3 3570(50) 10314.4 1982.1 10314.9 (3,5)+ 5.0 (1.3,0.8)
4 7937(15) 10318.7 1986.2 10318.9 3+ 4.0 1.0
5 8400(20) 10319.1 - - (3,5)−
6 - - 1994.5 10326.9 0.69
7 21100(300) 10331.5 1997.6 10330.0 1+ 0.18 0.09
8 - - 2002.8 10335.0 0.09
9 34400(200) 10344.4 2012.1 10344.1 (3,5)− 3.3 (0.8,0.6)
10 37200(100) 10347.2 2014.2 10346.1 8.6
11 - - 2022.5 10354.2 1.4
12 50750(200) 10360.3 2028.8 10360.3 2.7
13 61700(200) 10371.0 2037.1 10368.4 3+ 40.3 10.0
14 - - 2041.8 10373.0 3.2
15 - - 2046.5 10377.5 0.08
16 - - 2050.7 10381.6 1.2
17 82700(800) 10391.4 2058.1 10388.8 (3,5)+ 16.9 (4.2,2.8)
18 - - 2065.4 10395.9 1.0
19 94400(800) 10402.8 2068.6 10399.0 (3,5)+ 11.6 (2.9,1.9)
20 - - 2073.9 10404.2 0.91
21 106500(500) 10414.6 2080.2 10414.6 3+ 19.9 5.0
22 112700(1000) 10420.6 2086.5 10416.4 2.1
23 - - 2092.9 10422.7 0.32
24 - - 2099.3 10428.9 0.21
25 - - 2101.4 10430.9 0.43
26 - - 2106.6 10436.0 1.9
27 - - 2112.0 10441.3 0.19
28 - - 2115.2 10444.4 0.15
29 151000(1500) 10457.9 2121.6 10450.6 3+ 22.9 5.7
30 - - 2125.5 10454.4 1.0
31 - - 2134.4 10463.1 0.91
32 - - 2137.3 10465.9 0.92
33 - - 2143.0 10471.4 2.4
34 - - 2149.4 10477.6 0.55
35 - - 2153.4 10481.5 0.09
36 - - 2156.6 10484.7 0.12
37 - - 2160.4 10488.4 1.2
38 196000(1500) 10501.7 2165.2 10493.0 3+ 23.2 5.8
39 - - 2171.0 10498.7 1.0
40 208500(3000) 10513.8 2176.0 10503.5 7.4
41 - - 2182.5 10509.9 0.06
42 - - 2184.6 10511.9 0.03
2. EXPERIMENTAL TECHNIQUE
The investigations were carried out using the pro-
ton beam of the ESA-5 electrostatic accelerator at
the Nuclear Spectroscopy Laboratory (NSC KIPT).
The proton current on the target was up to 10 µA.
The bombarding energy was calibrated with well-
13
known resonances of the 27Al(p,γ)28Si reaction
(ER=992 and 1317 keV). The energy spread was
0.4 keV. A target of approximately 4 keV thickness at
Ep=2 MeV consisting of Ag2S (81.1% 36S) was used.
The spectra of γ-rays, arising from the decay
of resonance states in 37Cl, were measured with
the 70 cm3 Ge(Li)-detector. The energy resolu-
tion was about 3.0 keV for 60Co γ-lines. The ef-
ficiency was determined with calibrated standard
sources and using relative γ-ray intensities in the
27Al(p,γ)28Si reaction. To reduce the low-energy γ-
background, we used a combined lead-copper protec-
tion of the Ge(Li)-detector.
To obtain a yield curve of the 36S(p,γ)37Cl reac-
tion as a function of proton energy a spectrometer
based on a 150×100 mm NaI(Tl) crystal were used.
The experiments were performed on the spectromet-
ric equipment designed in the CAMAC standard and
operating on-line with a personal computer.
3. RESULTS
The excitation function of the 36S(p,γ)37Cl reac-
tion was measured in the proton energy range
Ep=1965...2190 keV. We established the positions of
40 resonances, identified as the excited states of 37Cl
(see Table 1). In this case, Q of the reaction was
taken to be 8386.34(23) keV, according to [5]. The
results obtained are in good agreement with [6].
The γ-decay spectra were measured for the res-
onances at Ep=2037, 2058, 2069, 2080, 2122 and
2165 keV. The decay schemes of the resonances were
constructed on the basis of the balance of energies
and intensities for the observed transitions, taking
into account all the known data on the levels of 37Cl
[5]. The branching ratios bγ for all six resonances are
listed in Table 2.
4. DATA ANALYSIS
4.1. Resonance strengths and γ-widths
The radiative width Γγ of a resonant level was calcu-
lated on the basis of the data on the strength S and
the proton decay width Γp of the resonance. The
value of S was determined from the expression[7]:
S = (2J + 1)
ΓpΓγ
Γ
= (1)
= (2I + 1)
1
(πλ)2
M
mp + M
εNγ
b · f · E ·W (θ)
e
Q
,
where J is the spin of the resonant state; Γp and Γγ
are, respectively, the proton and radiative resonance
widths; Γ is the total resonance width; I is the target
nucleus spin; λ is the incident proton wavelength; M
is the mass number of a target nucleus; mp is the pro-
ton mass; ε is the bremsstrahlung loss in the target
(eV·cm2·atom−1); Nγ is the γ-yield; bγ is the branch-
ing ratio; f is the number of target nuclei per atom;
E is the absolute detector efficiency; W (θ) is the an-
gular distribution of γ-photons (see below); e is the
elementary charge; and Q is the integrator charge. To
avoid the errors related to the anisotropy of the an-
gular distribution of γ-photons, the γ-decay spectra
of resonances were measured at the angle θlab=55◦,
at which W (θ)≈1.
Table 2. γ-Decay schemes of high excited states in 37Cl
Ep(keV), E∗
i (MeV), 2Jπ
i
E∗
f , 2Jπ
f 2037 2058 2069 2080 2122 2165
MeV 10.368 10.389 10.399 10.410 10451 10.493
3+ (3,5)+ (3,5)+ 3+ 3+ 3+
0 3+ 25 26 11 98 55 37
1.727 1+ 66 27 22 35
3.086 5+ 18 1 4
3.104 7− 11
3.708 3(+) 6 10
4.016 3+ 4
4.177 3− 2 10
4.273 7− 19
4.396 5 2
4.801 5+ 2 1
4.854 3 2
4.961 3 20
5.059 (3−-7+) 6
5.373 (1-5) 10 9
5.406 (1,3) 1
5.617 (1-5) 2
5.944 29
6.488 18
6.669 (3,5)+ 9 3
14
The strength of the resonance under study, Si,
is determined through the calibration resonance
strength Sk at Ep=1887 keV, which is equal to
31.0(3) eV [8]. For the case Qk = Qi, the quantities
Si and Sk are related by a relatively simple expres-
sion:
Si = Sk
λ2
k
λ2
i
εiN
i
γbkEk
εkNk
γ biEi
, (2)
where the indices ”k” and ”i” correspond to the
calibration and investigated resonances, respectively.
The thus obtained values of S for the resonances un-
der study are listed in Table 1.
The radiation widths Γγ were definitely obtained
only for the resonances at Ep=2037, 2058, 2069, 2080,
2122 and 2165 keV, for which spin values were estab-
lished in [9]. The Γγ value was calculated with the
data on resonance strengths S, under the assumption
that Γp >> Γγ . In this case
S ≈ (2J + 1)Γγ , (3)
and the resonance strength is completely defined by
Γγ . The obtained results are listed in Table 1.
4.2. Reaction rate
One of the main characteristics of the astrophysical
(p,n) or (p,γ)-reactions is the total rate, that can be
expressed via the temperature as following (in units
of cm3·s−1·mole−1) [10]:
NA〈σν〉=3.731·1010µ−
1
2T
− 3
2
9
∫ ∞
0
σ(E)Ee−11.605 E
T9 dE,
(4)
where E is the incident particle energy in the center-
of-mass system in MeV, T9 is the temperature in GK,
µ is the reduced mass in a.m.u. The total reaction
cross-section σ(in barn) is determined by the sum
of resonance and non-resonance contributions to a
mechanism of the nuclear reaction. Meanwhile the
contribution of isolated and narrow resonances into
the total astrophysical reaction rate can be calculated
by [10]:
NA〈σν〉r =1.540·1011(µT9)−
3
2
∑
i
ωγie
−11.605
ERi
T9 ,
(5)
where ERi are the resonance energies and ωγi is
the resonance strengths in MeV. The 36S(p,γ)37Cl,
36S(p,n)36Cl and 36S(p,α)33P reaction rate curves,
calculated according to [11] and the 36S(p,γ)37Cl re-
action rate with taking into account the obtained
experimental data on the strengths are shown in
Fig.2. It can be seen that contribution of the stud-
ied resonances to the total astrophysical 36S(p,γ)37Cl
reaction rate in the stellar temperature range of
(0.01-1)T9 is insignificant. However at temperatures
higher than 1T9 it becomes comparable with the
36S(p,α)33P reaction contribution to the total pro-
ton reaction rate on the 36S nuclei.
Fig.2. The 36S(p,γ)37Cl, 36S(p,n)36Cl and
36S(p,α)33P reaction rates
5. CONCLUSIONS
In this paper we obtained the radiation decay
widths for the neutron resonances observed in the
36Cl(n,p)36S reaction by using the 36S(p,γ)37Cl re-
action. In this context, the 36S(p,γ)37Cl reaction
yield was measured in the accelerated proton en-
ergy range Ep=1975...2190 keV, where we estab-
lished the positions of 40 resonances and determined
their strengths. This allowed to evaluate the con-
tribution of the resonances in the total rate of the
astrophysical 36S(p,γ)37Cl reaction.
The obtained radiation widths for the resonances
at Ep=2037, 2058, 2069, 2080, 2122 and 2165 keV can
be used as input parameters while analyzing a reso-
nance curve shape of the 36Cl(n,p)36S reaction, which
is of interest to astrophysics in solving the problem
of 36S isotope generation.
References
1. P. Shalanski et al. About Possibilities of Nucle-
osynthesis Modeling Using Computer Systems.
Elements Production in the S-Cl Region During
Helium Burning in 25M¯ Stars: Preprint JINR,
P10-2001-161. Dubna, 2001(in Russian).
2. Y.M. Gledenov, Y.P. Popov and V.I. Salatsky
Study of the 36Cl(n,p)36S reaction in the neutron
energy range up to 10 keV//Z. Phys. A. 1985,
v.322, p.685.
3. P.E. Koehleret et al. 36Cl(n,p)36S cross section
from 25 meV to 800 keV and the nucleosynthesis
of the rare isotope 36S//Phys. Rev. C. 1993, v.47,
p.2107.
4. L. De Smetet et al. Experimental determination
of the 36Cl(n,p)36S and 36Cl(n,α)33P reaction
cross sections and the consequences on the ori-
gin of 36S//Phys. Rev. C. 2007, v.75, p.034617.
5. P.M. Endt. Energy levels of A=21-44 nuclei
(VlI)//Nucl. Phys. A. 1990, v.521, p.1.
15
6. G.J.L. Nooren and C. Van der Leun The reaction
36S(p,γ)37Cl (I)//Nucl. Phys. A. 1984, v.423,
p.197.
7. A. Anttila, J. Keinonen, M. Hauntala and I. Fors-
blom. Use of the 27Al(p,γ)28Si, Ep=992 keV reso-
nance as a gamma-ray intensity standard//Nucl.
Instrum. Methods. 1977, v.147, p.501.
8. A.N. Vodin, A.S. Kachan and V.M. Mischenko.
The f7/2 analog resonances in odd nuclei of
the 1d2s-shell//Izv. RAN. Ser. Phys. 2002,
v.66(1), p.40.
9. A.S. Kachan et al. Resonance-like structure in
the 36S(p,γ)37Cl reaction//Probl. At. Sc. and
Techn. Ser. Nucl. Phys. Invest. 2004, v.5(44),
p.39.
10. C. Iliadis et al. Proton-induced thermonuclear re-
action rates for A=20-40 nuclei//The Astrophys.
J. Sup. Series. 2001, v.134, p.151.
11. http://nucastro.org/reaclib.html
ИССЛЕДОВАНИЕ АСТРОФИЗИЧЕСКОЙ РЕАКЦИИ 36S(p,γ)37Cl
ПРИ Ep=1975...2190 кэВ
А.Н. Водин, И.В. Ушаков, Г.К. Хомяков, Г.Э. Туллер,
Л.П. Корда, И.А. Шаповал, А.В. Тертичный
Представлены результаты исследований реакции 36S(p,γ)37Cl в области энергий протонов
Ep=1975...2190 кэВ. Оценены силы наблюдаемых резонансов. Построены схемы распада резонансов
при Ep=2037, 2058, 2069, 2080, 2122 и 2165 кэВ. Рассчитаны полные радиационные ширины распада
резонансов. Проведена оценка скорости астрофизической реакции 36S(p,γ)37Cl.
ДОСЛIДЖЕННЯ АСТРОФIЗИЧНОЇ РЕАКЦIЇ 36S(p,γ)37Cl
ПРИ Ep=1975...2190 кэВ
О.М. Водiн, I.В. Ушаков, Г.К. Хомяков, Г.Е. Туллер,
Л.П. Корда, I.А. Шаповал, А.В. Тертичний
Представлено результати дослiджень реакцiї 36S(p,γ)37Cl в областi енергiй протонiв
Ep=1975...2190 кеВ. Оцiнено сили спостережуваних резонансiв. Побудовано схеми розпаду резо-
нансiв при Ep=2037, 2058, 2069, 2080, 2122 та 2165 кеВ. Розрахованi повнi радiацiйнi ширини розпаду
резонансiв. Проведено оцiнку швидкостi астрофiзичної реакцiї 36S(p,γ)37Cl.
16
|
| id | nasplib_isofts_kiev_ua-123456789-96397 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 1562-6016 |
| language | English |
| last_indexed | 2025-12-07T13:21:23Z |
| publishDate | 2009 |
| publisher | Національний науковий центр «Харківський фізико-технічний інститут» НАН України |
| record_format | dspace |
| spelling | Vodin, A.N. Ushakov, I.V. Khomyakov, G.K. Tuller, G.E. Korda, L.P. Shapoval, I.A. Tertichnyi, A.V. 2016-03-15T21:29:04Z 2016-03-15T21:29:04Z 2009 Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV / A.N. Vodin1, I.V. Ushakov, G.K. Khomyakov, G.E. Tuller, L.P. Korda, I.A. Shapoval, A.V. Tertichnyi // Вопросы атомной науки и техники. — 2009. — № 5. — С. 12-16. — Бібліогр.: 11 назв. — англ. 1562-6016 PACS: 24.30.-v, 25.40.Lw, 25.70.Ef, 25.70.Gh https://nasplib.isofts.kiev.ua/handle/123456789/96397 The ³⁶S(p,γ) ³⁷Cl reaction was investigated in the proton energy range Ep=1975-2190 keV. The observed resonance strengths were evaluated. The γ-decay schemes of the resonances at Ep=2037, 2058, 2069, 2080, 2122 and 2165 keV were constructed and the total γ-widths were determined. The astrophysical ³⁶S(p,γ) ³⁷Cl reaction rate was estimated. Представлено результати дослiджень реакцiї ³⁶S(p,γ) ³⁷Cl в областi енергiй протонiв Ep=1975...2190 кеВ. Оцiнено сили спостережуваних резонансiв. Побудовано схеми розпаду резо- нансiв при Ep=2037, 2058, 2069, 2080, 2122 та 2165 кеВ. Розрахованi повнi радiацiйнi ширини розпаду резонансiв. Проведено оцiнку швидкостi астрофiзичної реакцiї ³⁶S(p,γ) ³⁷Cl. Представлены результаты исследований реакции ³⁶S(p,γ) ³⁷Cl в области энергий протонов Ep=1975...2190 кэВ. Оценены силы наблюдаемых резонансов. Построены схемы распада резонансов при Ep=2037, 2058, 2069, 2080, 2122 и 2165 кэВ. Рассчитаны полные радиационные ширины распада резонансов. Проведена оценка скорости астрофизической реакции ³⁶S(p,γ) ³⁷Cl. en Національний науковий центр «Харківський фізико-технічний інститут» НАН України Вопросы атомной науки и техники Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV Дослiдження астрофiзичної реакцiї ³⁶S(p,γ) ³⁷Cl при Ep=1975...2190 кэВ Исследование астрофизической реакции ³⁶S(p,γ) ³⁷Cl при Ep=1975...2190 кэВ Article published earlier |
| spellingShingle | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV Vodin, A.N. Ushakov, I.V. Khomyakov, G.K. Tuller, G.E. Korda, L.P. Shapoval, I.A. Tertichnyi, A.V. |
| title | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV |
| title_alt | Дослiдження астрофiзичної реакцiї ³⁶S(p,γ) ³⁷Cl при Ep=1975...2190 кэВ Исследование астрофизической реакции ³⁶S(p,γ) ³⁷Cl при Ep=1975...2190 кэВ |
| title_full | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV |
| title_fullStr | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV |
| title_full_unstemmed | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV |
| title_short | Investigation of the astrophysical ³⁶S(p,γ) ³⁷Cl reaction AT Ep=1975...2190 keV |
| title_sort | investigation of the astrophysical ³⁶s(p,γ) ³⁷cl reaction at ep=1975...2190 kev |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/96397 |
| work_keys_str_mv | AT vodinan investigationoftheastrophysical36spγ37clreactionatep19752190kev AT ushakoviv investigationoftheastrophysical36spγ37clreactionatep19752190kev AT khomyakovgk investigationoftheastrophysical36spγ37clreactionatep19752190kev AT tullerge investigationoftheastrophysical36spγ37clreactionatep19752190kev AT kordalp investigationoftheastrophysical36spγ37clreactionatep19752190kev AT shapovalia investigationoftheastrophysical36spγ37clreactionatep19752190kev AT tertichnyiav investigationoftheastrophysical36spγ37clreactionatep19752190kev AT vodinan doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT ushakoviv doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT khomyakovgk doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT tullerge doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT kordalp doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT shapovalia doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT tertichnyiav doslidžennâastrofizičnoíreakcií36spγ37clpriep19752190kév AT vodinan issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév AT ushakoviv issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév AT khomyakovgk issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév AT tullerge issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév AT kordalp issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév AT shapovalia issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév AT tertichnyiav issledovanieastrofizičeskoireakcii36spγ37clpriep19752190kév |