Another set of reactions that result in the fusing of hydrogen into helium in the Sun and especially in hotter stars is called the carbon cycle. It is 12 C + 1 H → 13 N+ γ , 13 N → 13 C + e + + v e , 13 C + 1 H → 14 N + γ , 14 N + 1 H → 15 O + γ , 15 O → 15 N + e + + v e , 15 N + 1 H → 12 C + 4 He . Write down the overall effect at the carbon cycle (as was done for the proton−proton cycle in 2 e − + 4 1 H + 4 He + 2 v e + 6 γ . Note the number of protons ( l H) required and assume that the positrons (e + ) annihilate electrons to form more (rays.
Another set of reactions that result in the fusing of hydrogen into helium in the Sun and especially in hotter stars is called the carbon cycle. It is 12 C + 1 H → 13 N+ γ , 13 N → 13 C + e + + v e , 13 C + 1 H → 14 N + γ , 14 N + 1 H → 15 O + γ , 15 O → 15 N + e + + v e , 15 N + 1 H → 12 C + 4 He . Write down the overall effect at the carbon cycle (as was done for the proton−proton cycle in 2 e − + 4 1 H + 4 He + 2 v e + 6 γ . Note the number of protons ( l H) required and assume that the positrons (e + ) annihilate electrons to form more (rays.
Another set of reactions that result in the fusing of hydrogen into helium in the Sun and especially in hotter stars is called the carbon cycle. It is
12
C
+
1
H
→
13
N+
γ
,
13
N
→
13
C
+
e
+
+
v
e
,
13
C
+
1
H
→
14
N
+
γ
,
14
N
+
1
H
→
15
O
+
γ
,
15
O
→
15
N
+
e
+
+
v
e
,
15
N
+
1
H
→
12
C
+
4
He
.
Write down the overall effect at the carbon cycle (as was done for the proton−proton cycle in
2
e
−
+
4
1
H
+
4
He
+
2
v
e
+
6
γ
. Note the number of protons (lH) required and assume that the positrons (e+) annihilate electrons to form more (rays.
Another series of nuclear reactions that can produce energy in the interior of stars is the carbon cycle first proposed by Hans Bethe in 1939, leading to his Nobel Prize in Physics in 1967. This cycle is most efficient when the central temperature in a star is above 1.6 x 107 K. Because the temperature at the center of the Sun is only 1.5 x 107 K, the following cycle produces less than 10% of the Sun’s energy. (a) A high-energy proton is absorbed by 12C. Another nucleus, A, is produced in the reaction, along with a gamma ray. Identify nucleus A. (b) Nucleus A decays through positron emission to form nucleus B. Identify nucleus B. (c) Nucleus B absorbs a proton to produce nucleus C and a gamma ray. Identify nucleus C. (d) Nucleus C absorbs a proton to produce nucleus D and a gamma ray. Identify nucleus D. (e) Nucleus D decays through positron emission to produce nucleus E. Identify nucleus E. (f) Nucleus E absorbs a proton to produce nucleus F plus an alpha particle. Identify nucleus F.…
In a nuclear fusion reaction, 2 g of hydrogen is converted
into 1.985 g of helium. What is the energy released?
a. 4.5 × 103J
b. 4.5 × 106J
c. 1.35 × 1012 J
d. 1.35 × 1015 J
When the temperature is 300 K, the half-life of X is 21 days. If the temperature is increased to 600 K, the half-life is then
A.
42 days
B.
21 days
C.
need to know the mass
D.
4 weeks
E.
10.5 days
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