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9 | 2839-2842 | 7 1 (iv) Consider two very light nuclei (A ≤ 10) joining to form a heavier
nucleus The binding energy per nucleon of the fused heavier nuclei
is more than the binding energy per nucleon of the lighter nuclei |
9 | 2840-2843 | 1 (iv) Consider two very light nuclei (A ≤ 10) joining to form a heavier
nucleus The binding energy per nucleon of the fused heavier nuclei
is more than the binding energy per nucleon of the lighter nuclei This means that the final system is more tightly bound than the initial
system |
9 | 2841-2844 | (iv) Consider two very light nuclei (A ≤ 10) joining to form a heavier
nucleus The binding energy per nucleon of the fused heavier nuclei
is more than the binding energy per nucleon of the lighter nuclei This means that the final system is more tightly bound than the initial
system Again energy would be released in such a process of
fusion |
9 | 2842-2845 | The binding energy per nucleon of the fused heavier nuclei
is more than the binding energy per nucleon of the lighter nuclei This means that the final system is more tightly bound than the initial
system Again energy would be released in such a process of
fusion This is the energy source of sun, to be discussed later in
Section 13 |
9 | 2843-2846 | This means that the final system is more tightly bound than the initial
system Again energy would be released in such a process of
fusion This is the energy source of sun, to be discussed later in
Section 13 7 |
9 | 2844-2847 | Again energy would be released in such a process of
fusion This is the energy source of sun, to be discussed later in
Section 13 7 2 |
9 | 2845-2848 | This is the energy source of sun, to be discussed later in
Section 13 7 2 13 |
9 | 2846-2849 | 7 2 13 5 NUCLEAR FORCE
The force that determines the motion of atomic electrons is the familiar
Coulomb force |
9 | 2847-2850 | 2 13 5 NUCLEAR FORCE
The force that determines the motion of atomic electrons is the familiar
Coulomb force In Section 13 |
9 | 2848-2851 | 13 5 NUCLEAR FORCE
The force that determines the motion of atomic electrons is the familiar
Coulomb force In Section 13 4, we have seen that for average mass
nuclei the binding energy per nucleon is approximately 8 MeV, which is
much larger than the binding energy in atoms |
9 | 2849-2852 | 5 NUCLEAR FORCE
The force that determines the motion of atomic electrons is the familiar
Coulomb force In Section 13 4, we have seen that for average mass
nuclei the binding energy per nucleon is approximately 8 MeV, which is
much larger than the binding energy in atoms Therefore, to bind a
nucleus together there must be a strong attractive force of a totally
different kind |
9 | 2850-2853 | In Section 13 4, we have seen that for average mass
nuclei the binding energy per nucleon is approximately 8 MeV, which is
much larger than the binding energy in atoms Therefore, to bind a
nucleus together there must be a strong attractive force of a totally
different kind It must be strong enough to overcome the repulsion
between the (positively charged) protons and to bind both protons and
neutrons into the tiny nuclear volume |
9 | 2851-2854 | 4, we have seen that for average mass
nuclei the binding energy per nucleon is approximately 8 MeV, which is
much larger than the binding energy in atoms Therefore, to bind a
nucleus together there must be a strong attractive force of a totally
different kind It must be strong enough to overcome the repulsion
between the (positively charged) protons and to bind both protons and
neutrons into the tiny nuclear volume We have already seen
that the constancy of binding energy per nucleon can be
understood in terms of its short-range |
9 | 2852-2855 | Therefore, to bind a
nucleus together there must be a strong attractive force of a totally
different kind It must be strong enough to overcome the repulsion
between the (positively charged) protons and to bind both protons and
neutrons into the tiny nuclear volume We have already seen
that the constancy of binding energy per nucleon can be
understood in terms of its short-range Many features of the
nuclear binding force are summarised below |
9 | 2853-2856 | It must be strong enough to overcome the repulsion
between the (positively charged) protons and to bind both protons and
neutrons into the tiny nuclear volume We have already seen
that the constancy of binding energy per nucleon can be
understood in terms of its short-range Many features of the
nuclear binding force are summarised below These are
obtained from a variety of experiments carried out during 1930
to 1950 |
9 | 2854-2857 | We have already seen
that the constancy of binding energy per nucleon can be
understood in terms of its short-range Many features of the
nuclear binding force are summarised below These are
obtained from a variety of experiments carried out during 1930
to 1950 (i)
The nuclear force is much stronger than the Coulomb force
acting between charges or the gravitational forces between
masses |
9 | 2855-2858 | Many features of the
nuclear binding force are summarised below These are
obtained from a variety of experiments carried out during 1930
to 1950 (i)
The nuclear force is much stronger than the Coulomb force
acting between charges or the gravitational forces between
masses The nuclear binding force has to dominate over
the Coulomb repulsive force between protons inside the
nucleus |
9 | 2856-2859 | These are
obtained from a variety of experiments carried out during 1930
to 1950 (i)
The nuclear force is much stronger than the Coulomb force
acting between charges or the gravitational forces between
masses The nuclear binding force has to dominate over
the Coulomb repulsive force between protons inside the
nucleus This happens only because the nuclear force is
much stronger than the coulomb force |
9 | 2857-2860 | (i)
The nuclear force is much stronger than the Coulomb force
acting between charges or the gravitational forces between
masses The nuclear binding force has to dominate over
the Coulomb repulsive force between protons inside the
nucleus This happens only because the nuclear force is
much stronger than the coulomb force The gravitational
force is much weaker than even Coulomb force |
9 | 2858-2861 | The nuclear binding force has to dominate over
the Coulomb repulsive force between protons inside the
nucleus This happens only because the nuclear force is
much stronger than the coulomb force The gravitational
force is much weaker than even Coulomb force (ii) The nuclear force between two nucleons falls rapidly to
zero as their distance is more than a few femtometres |
9 | 2859-2862 | This happens only because the nuclear force is
much stronger than the coulomb force The gravitational
force is much weaker than even Coulomb force (ii) The nuclear force between two nucleons falls rapidly to
zero as their distance is more than a few femtometres This
leads to saturation of forces in a medium or a large-sized
nucleus, which is the reason for the constancy of the
binding energy per nucleon |
9 | 2860-2863 | The gravitational
force is much weaker than even Coulomb force (ii) The nuclear force between two nucleons falls rapidly to
zero as their distance is more than a few femtometres This
leads to saturation of forces in a medium or a large-sized
nucleus, which is the reason for the constancy of the
binding energy per nucleon A rough plot of the potential energy between two nucleons
as a function of distance is shown in the Fig |
9 | 2861-2864 | (ii) The nuclear force between two nucleons falls rapidly to
zero as their distance is more than a few femtometres This
leads to saturation of forces in a medium or a large-sized
nucleus, which is the reason for the constancy of the
binding energy per nucleon A rough plot of the potential energy between two nucleons
as a function of distance is shown in the Fig 13 |
9 | 2862-2865 | This
leads to saturation of forces in a medium or a large-sized
nucleus, which is the reason for the constancy of the
binding energy per nucleon A rough plot of the potential energy between two nucleons
as a function of distance is shown in the Fig 13 2 |
9 | 2863-2866 | A rough plot of the potential energy between two nucleons
as a function of distance is shown in the Fig 13 2 The
potential energy is a minimum at a distance r0 of about
0 |
9 | 2864-2867 | 13 2 The
potential energy is a minimum at a distance r0 of about
0 8 fm |
9 | 2865-2868 | 2 The
potential energy is a minimum at a distance r0 of about
0 8 fm This means that the force is attractive for distances larger
than 0 |
9 | 2866-2869 | The
potential energy is a minimum at a distance r0 of about
0 8 fm This means that the force is attractive for distances larger
than 0 8 fm and repulsive if they are separated by distances less
than 0 |
9 | 2867-2870 | 8 fm This means that the force is attractive for distances larger
than 0 8 fm and repulsive if they are separated by distances less
than 0 8 fm |
9 | 2868-2871 | This means that the force is attractive for distances larger
than 0 8 fm and repulsive if they are separated by distances less
than 0 8 fm FIGURE 13 |
9 | 2869-2872 | 8 fm and repulsive if they are separated by distances less
than 0 8 fm FIGURE 13 2 Potential energy
of a pair of nucleons as a
function of their separation |
9 | 2870-2873 | 8 fm FIGURE 13 2 Potential energy
of a pair of nucleons as a
function of their separation For a separation greater
than r0, the force is attractive
and for separations less
than r0, the force is
strongly repulsive |
9 | 2871-2874 | FIGURE 13 2 Potential energy
of a pair of nucleons as a
function of their separation For a separation greater
than r0, the force is attractive
and for separations less
than r0, the force is
strongly repulsive Rationalised 2023-24
Physics
314
(iii) The nuclear force between neutron-neutron, proton-neutron and
proton-proton is approximately the same |
9 | 2872-2875 | 2 Potential energy
of a pair of nucleons as a
function of their separation For a separation greater
than r0, the force is attractive
and for separations less
than r0, the force is
strongly repulsive Rationalised 2023-24
Physics
314
(iii) The nuclear force between neutron-neutron, proton-neutron and
proton-proton is approximately the same The nuclear force does not
depend on the electric charge |
9 | 2873-2876 | For a separation greater
than r0, the force is attractive
and for separations less
than r0, the force is
strongly repulsive Rationalised 2023-24
Physics
314
(iii) The nuclear force between neutron-neutron, proton-neutron and
proton-proton is approximately the same The nuclear force does not
depend on the electric charge Unlike Coulomb’s law or the Newton’s law of gravitation there is no
simple mathematical form of the nuclear force |
9 | 2874-2877 | Rationalised 2023-24
Physics
314
(iii) The nuclear force between neutron-neutron, proton-neutron and
proton-proton is approximately the same The nuclear force does not
depend on the electric charge Unlike Coulomb’s law or the Newton’s law of gravitation there is no
simple mathematical form of the nuclear force 13 |
9 | 2875-2878 | The nuclear force does not
depend on the electric charge Unlike Coulomb’s law or the Newton’s law of gravitation there is no
simple mathematical form of the nuclear force 13 6 RADIOACTIVITY
A |
9 | 2876-2879 | Unlike Coulomb’s law or the Newton’s law of gravitation there is no
simple mathematical form of the nuclear force 13 6 RADIOACTIVITY
A H |
9 | 2877-2880 | 13 6 RADIOACTIVITY
A H Becquerel discovered radioactivity in 1896 purely by accident |
9 | 2878-2881 | 6 RADIOACTIVITY
A H Becquerel discovered radioactivity in 1896 purely by accident While
studying the fluorescence and phosphorescence of compounds irradiated
with visible light, Becquerel observed an interesting phenomenon |
9 | 2879-2882 | H Becquerel discovered radioactivity in 1896 purely by accident While
studying the fluorescence and phosphorescence of compounds irradiated
with visible light, Becquerel observed an interesting phenomenon After
illuminating some pieces of uranium-potassium sulphate with visible
light, he wrapped them in black paper and separated the package from a
photographic plate by a piece of silver |
9 | 2880-2883 | Becquerel discovered radioactivity in 1896 purely by accident While
studying the fluorescence and phosphorescence of compounds irradiated
with visible light, Becquerel observed an interesting phenomenon After
illuminating some pieces of uranium-potassium sulphate with visible
light, he wrapped them in black paper and separated the package from a
photographic plate by a piece of silver When, after several hours of
exposure, the photographic plate was developed, it showed blackening
due to something that must have been emitted by the compound and
was able to penetrate both black paper and the silver |
9 | 2881-2884 | While
studying the fluorescence and phosphorescence of compounds irradiated
with visible light, Becquerel observed an interesting phenomenon After
illuminating some pieces of uranium-potassium sulphate with visible
light, he wrapped them in black paper and separated the package from a
photographic plate by a piece of silver When, after several hours of
exposure, the photographic plate was developed, it showed blackening
due to something that must have been emitted by the compound and
was able to penetrate both black paper and the silver Experiments performed subsequently showed that radioactivity was
a nuclear phenomenon in which an unstable nucleus undergoes a decay |
9 | 2882-2885 | After
illuminating some pieces of uranium-potassium sulphate with visible
light, he wrapped them in black paper and separated the package from a
photographic plate by a piece of silver When, after several hours of
exposure, the photographic plate was developed, it showed blackening
due to something that must have been emitted by the compound and
was able to penetrate both black paper and the silver Experiments performed subsequently showed that radioactivity was
a nuclear phenomenon in which an unstable nucleus undergoes a decay This is referred to as radioactive decay |
9 | 2883-2886 | When, after several hours of
exposure, the photographic plate was developed, it showed blackening
due to something that must have been emitted by the compound and
was able to penetrate both black paper and the silver Experiments performed subsequently showed that radioactivity was
a nuclear phenomenon in which an unstable nucleus undergoes a decay This is referred to as radioactive decay Three types of radioactive decay
occur in nature :
(i) a-decay in which a helium nucleus
4
2He is emitted;
(ii) b-decay in which electrons or positrons (particles with the same mass
as electrons, but with a charge exactly opposite to that of electron)
are emitted;
(iii) g-decay in which high energy (hundreds of keV or more) photons are
emitted |
9 | 2884-2887 | Experiments performed subsequently showed that radioactivity was
a nuclear phenomenon in which an unstable nucleus undergoes a decay This is referred to as radioactive decay Three types of radioactive decay
occur in nature :
(i) a-decay in which a helium nucleus
4
2He is emitted;
(ii) b-decay in which electrons or positrons (particles with the same mass
as electrons, but with a charge exactly opposite to that of electron)
are emitted;
(iii) g-decay in which high energy (hundreds of keV or more) photons are
emitted Each of these decay will be considered in subsequent sub-sections |
9 | 2885-2888 | This is referred to as radioactive decay Three types of radioactive decay
occur in nature :
(i) a-decay in which a helium nucleus
4
2He is emitted;
(ii) b-decay in which electrons or positrons (particles with the same mass
as electrons, but with a charge exactly opposite to that of electron)
are emitted;
(iii) g-decay in which high energy (hundreds of keV or more) photons are
emitted Each of these decay will be considered in subsequent sub-sections 13 |
9 | 2886-2889 | Three types of radioactive decay
occur in nature :
(i) a-decay in which a helium nucleus
4
2He is emitted;
(ii) b-decay in which electrons or positrons (particles with the same mass
as electrons, but with a charge exactly opposite to that of electron)
are emitted;
(iii) g-decay in which high energy (hundreds of keV or more) photons are
emitted Each of these decay will be considered in subsequent sub-sections 13 7 NUCLEAR ENERGY
The curve of binding energy per nucleon Ebn, given in Fig |
9 | 2887-2890 | Each of these decay will be considered in subsequent sub-sections 13 7 NUCLEAR ENERGY
The curve of binding energy per nucleon Ebn, given in Fig 13 |
9 | 2888-2891 | 13 7 NUCLEAR ENERGY
The curve of binding energy per nucleon Ebn, given in Fig 13 1, has
a long flat middle region between A = 30 and A = 170 |
9 | 2889-2892 | 7 NUCLEAR ENERGY
The curve of binding energy per nucleon Ebn, given in Fig 13 1, has
a long flat middle region between A = 30 and A = 170 In this region
the binding energy per nucleon is nearly constant (8 |
9 | 2890-2893 | 13 1, has
a long flat middle region between A = 30 and A = 170 In this region
the binding energy per nucleon is nearly constant (8 0 MeV) |
9 | 2891-2894 | 1, has
a long flat middle region between A = 30 and A = 170 In this region
the binding energy per nucleon is nearly constant (8 0 MeV) For
the lighter nuclei region, A < 30, and for the heavier nuclei region,
A > 170, the binding energy per nucleon is less than 8 |
9 | 2892-2895 | In this region
the binding energy per nucleon is nearly constant (8 0 MeV) For
the lighter nuclei region, A < 30, and for the heavier nuclei region,
A > 170, the binding energy per nucleon is less than 8 0 MeV, as we
have noted earlier |
9 | 2893-2896 | 0 MeV) For
the lighter nuclei region, A < 30, and for the heavier nuclei region,
A > 170, the binding energy per nucleon is less than 8 0 MeV, as we
have noted earlier Now, the greater the binding energy, the less is the
total mass of a bound system, such as a nucleus |
9 | 2894-2897 | For
the lighter nuclei region, A < 30, and for the heavier nuclei region,
A > 170, the binding energy per nucleon is less than 8 0 MeV, as we
have noted earlier Now, the greater the binding energy, the less is the
total mass of a bound system, such as a nucleus Consequently, if nuclei
with less total binding energy transform to nuclei with greater binding
energy, there will be a net energy release |
9 | 2895-2898 | 0 MeV, as we
have noted earlier Now, the greater the binding energy, the less is the
total mass of a bound system, such as a nucleus Consequently, if nuclei
with less total binding energy transform to nuclei with greater binding
energy, there will be a net energy release This is what happens when a
heavy nucleus decays into two or more intermediate mass fragments
(fission) or when light nuclei fuse into a havier nucleus (fusion |
9 | 2896-2899 | Now, the greater the binding energy, the less is the
total mass of a bound system, such as a nucleus Consequently, if nuclei
with less total binding energy transform to nuclei with greater binding
energy, there will be a net energy release This is what happens when a
heavy nucleus decays into two or more intermediate mass fragments
(fission) or when light nuclei fuse into a havier nucleus (fusion )
Exothermic chemical reactions underlie conventional energy sources
such as coal or petroleum |
9 | 2897-2900 | Consequently, if nuclei
with less total binding energy transform to nuclei with greater binding
energy, there will be a net energy release This is what happens when a
heavy nucleus decays into two or more intermediate mass fragments
(fission) or when light nuclei fuse into a havier nucleus (fusion )
Exothermic chemical reactions underlie conventional energy sources
such as coal or petroleum Here the energies involved are in the range of
electron volts |
9 | 2898-2901 | This is what happens when a
heavy nucleus decays into two or more intermediate mass fragments
(fission) or when light nuclei fuse into a havier nucleus (fusion )
Exothermic chemical reactions underlie conventional energy sources
such as coal or petroleum Here the energies involved are in the range of
electron volts On the other hand, in a nuclear reaction, the energy release
is of the order of MeV |
9 | 2899-2902 | )
Exothermic chemical reactions underlie conventional energy sources
such as coal or petroleum Here the energies involved are in the range of
electron volts On the other hand, in a nuclear reaction, the energy release
is of the order of MeV Thus for the same quantity of matter, nuclear
sources produce a million times more energy than a chemical source |
9 | 2900-2903 | Here the energies involved are in the range of
electron volts On the other hand, in a nuclear reaction, the energy release
is of the order of MeV Thus for the same quantity of matter, nuclear
sources produce a million times more energy than a chemical source Fission of 1 kg of uranium, for example, generates 1014 J of energy;
compare it with burning of 1 kg of coal that gives 107 J |
9 | 2901-2904 | On the other hand, in a nuclear reaction, the energy release
is of the order of MeV Thus for the same quantity of matter, nuclear
sources produce a million times more energy than a chemical source Fission of 1 kg of uranium, for example, generates 1014 J of energy;
compare it with burning of 1 kg of coal that gives 107 J Rationalised 2023-24
315
Nuclei
13 |
9 | 2902-2905 | Thus for the same quantity of matter, nuclear
sources produce a million times more energy than a chemical source Fission of 1 kg of uranium, for example, generates 1014 J of energy;
compare it with burning of 1 kg of coal that gives 107 J Rationalised 2023-24
315
Nuclei
13 7 |
9 | 2903-2906 | Fission of 1 kg of uranium, for example, generates 1014 J of energy;
compare it with burning of 1 kg of coal that gives 107 J Rationalised 2023-24
315
Nuclei
13 7 1 Fission
New possibilities emerge when we go beyond natural radioactive decays
and study nuclear reactions by bombarding nuclei with other nuclear
particles such as proton, neutron, a-particle, etc |
9 | 2904-2907 | Rationalised 2023-24
315
Nuclei
13 7 1 Fission
New possibilities emerge when we go beyond natural radioactive decays
and study nuclear reactions by bombarding nuclei with other nuclear
particles such as proton, neutron, a-particle, etc A most important neutron-induced nuclear reaction is fission |
9 | 2905-2908 | 7 1 Fission
New possibilities emerge when we go beyond natural radioactive decays
and study nuclear reactions by bombarding nuclei with other nuclear
particles such as proton, neutron, a-particle, etc A most important neutron-induced nuclear reaction is fission An
example of fission is when a uranium isotope 235
92 U bombarded with a
neutron breaks into two intermediate mass nuclear fragments
1
235
236
144
89
1
0
92
92
56
36
0
n
U
U
Ba
Kr
3 n
+
→
→
+
+
(13 |
9 | 2906-2909 | 1 Fission
New possibilities emerge when we go beyond natural radioactive decays
and study nuclear reactions by bombarding nuclei with other nuclear
particles such as proton, neutron, a-particle, etc A most important neutron-induced nuclear reaction is fission An
example of fission is when a uranium isotope 235
92 U bombarded with a
neutron breaks into two intermediate mass nuclear fragments
1
235
236
144
89
1
0
92
92
56
36
0
n
U
U
Ba
Kr
3 n
+
→
→
+
+
(13 10)
The same reaction can produce other pairs of intermediate mass
fragments
1
235
236
133
99
1
0
92
92
51
41
0
n
U
U
Sb
Nb
4 n
+
→
→
+
+
(13 |
9 | 2907-2910 | A most important neutron-induced nuclear reaction is fission An
example of fission is when a uranium isotope 235
92 U bombarded with a
neutron breaks into two intermediate mass nuclear fragments
1
235
236
144
89
1
0
92
92
56
36
0
n
U
U
Ba
Kr
3 n
+
→
→
+
+
(13 10)
The same reaction can produce other pairs of intermediate mass
fragments
1
235
236
133
99
1
0
92
92
51
41
0
n
U
U
Sb
Nb
4 n
+
→
→
+
+
(13 11)
Or, as another example,
1
235
140
94
1
0
92
54
38
0
n
U
Xe
Sr
2 n
+
→
+
+
(13 |
9 | 2908-2911 | An
example of fission is when a uranium isotope 235
92 U bombarded with a
neutron breaks into two intermediate mass nuclear fragments
1
235
236
144
89
1
0
92
92
56
36
0
n
U
U
Ba
Kr
3 n
+
→
→
+
+
(13 10)
The same reaction can produce other pairs of intermediate mass
fragments
1
235
236
133
99
1
0
92
92
51
41
0
n
U
U
Sb
Nb
4 n
+
→
→
+
+
(13 11)
Or, as another example,
1
235
140
94
1
0
92
54
38
0
n
U
Xe
Sr
2 n
+
→
+
+
(13 12)
The fragment products are radioactive nuclei; they emit b particles in
succession to achieve stable end products |
9 | 2909-2912 | 10)
The same reaction can produce other pairs of intermediate mass
fragments
1
235
236
133
99
1
0
92
92
51
41
0
n
U
U
Sb
Nb
4 n
+
→
→
+
+
(13 11)
Or, as another example,
1
235
140
94
1
0
92
54
38
0
n
U
Xe
Sr
2 n
+
→
+
+
(13 12)
The fragment products are radioactive nuclei; they emit b particles in
succession to achieve stable end products The energy released (the Q value ) in the fission reaction of nuclei like
uranium is of the order of 200 MeV per fissioning nucleus |
9 | 2910-2913 | 11)
Or, as another example,
1
235
140
94
1
0
92
54
38
0
n
U
Xe
Sr
2 n
+
→
+
+
(13 12)
The fragment products are radioactive nuclei; they emit b particles in
succession to achieve stable end products The energy released (the Q value ) in the fission reaction of nuclei like
uranium is of the order of 200 MeV per fissioning nucleus This is
estimated as follows:
Let us take a nucleus with A = 240 breaking into two fragments each
of A = 120 |
9 | 2911-2914 | 12)
The fragment products are radioactive nuclei; they emit b particles in
succession to achieve stable end products The energy released (the Q value ) in the fission reaction of nuclei like
uranium is of the order of 200 MeV per fissioning nucleus This is
estimated as follows:
Let us take a nucleus with A = 240 breaking into two fragments each
of A = 120 Then
Ebn for A = 240 nucleus is about 7 |
9 | 2912-2915 | The energy released (the Q value ) in the fission reaction of nuclei like
uranium is of the order of 200 MeV per fissioning nucleus This is
estimated as follows:
Let us take a nucleus with A = 240 breaking into two fragments each
of A = 120 Then
Ebn for A = 240 nucleus is about 7 6 MeV,
Ebn for the two A = 120 fragment nuclei is about 8 |
9 | 2913-2916 | This is
estimated as follows:
Let us take a nucleus with A = 240 breaking into two fragments each
of A = 120 Then
Ebn for A = 240 nucleus is about 7 6 MeV,
Ebn for the two A = 120 fragment nuclei is about 8 5 MeV |
9 | 2914-2917 | Then
Ebn for A = 240 nucleus is about 7 6 MeV,
Ebn for the two A = 120 fragment nuclei is about 8 5 MeV \
Gain in binding energy for nucleon is about 0 |
9 | 2915-2918 | 6 MeV,
Ebn for the two A = 120 fragment nuclei is about 8 5 MeV \
Gain in binding energy for nucleon is about 0 9 MeV |
9 | 2916-2919 | 5 MeV \
Gain in binding energy for nucleon is about 0 9 MeV Hence the total gain in binding energy is 240×0 |
9 | 2917-2920 | \
Gain in binding energy for nucleon is about 0 9 MeV Hence the total gain in binding energy is 240×0 9 or 216 MeV |
9 | 2918-2921 | 9 MeV Hence the total gain in binding energy is 240×0 9 or 216 MeV The disintegration energy in fission events first appears as the kinetic
energy of the fragments and neutrons |
9 | 2919-2922 | Hence the total gain in binding energy is 240×0 9 or 216 MeV The disintegration energy in fission events first appears as the kinetic
energy of the fragments and neutrons Eventually it is transferred to the
surrounding matter appearing as heat |
9 | 2920-2923 | 9 or 216 MeV The disintegration energy in fission events first appears as the kinetic
energy of the fragments and neutrons Eventually it is transferred to the
surrounding matter appearing as heat The source of energy in nuclear
reactors, which produce electricity, is nuclear fission |
9 | 2921-2924 | The disintegration energy in fission events first appears as the kinetic
energy of the fragments and neutrons Eventually it is transferred to the
surrounding matter appearing as heat The source of energy in nuclear
reactors, which produce electricity, is nuclear fission The enormous
energy released in an atom bomb comes from uncontrolled nuclear
fission |
9 | 2922-2925 | Eventually it is transferred to the
surrounding matter appearing as heat The source of energy in nuclear
reactors, which produce electricity, is nuclear fission The enormous
energy released in an atom bomb comes from uncontrolled nuclear
fission 13 |
9 | 2923-2926 | The source of energy in nuclear
reactors, which produce electricity, is nuclear fission The enormous
energy released in an atom bomb comes from uncontrolled nuclear
fission 13 7 |
9 | 2924-2927 | The enormous
energy released in an atom bomb comes from uncontrolled nuclear
fission 13 7 2 Nuclear fusion – energy generation in stars
When two light nuclei fuse to form a larger nucleus, energy is released,
since the larger nucleus is more tightly bound, as seen from the binding
energy curve in Fig |
9 | 2925-2928 | 13 7 2 Nuclear fusion – energy generation in stars
When two light nuclei fuse to form a larger nucleus, energy is released,
since the larger nucleus is more tightly bound, as seen from the binding
energy curve in Fig 13 |
9 | 2926-2929 | 7 2 Nuclear fusion – energy generation in stars
When two light nuclei fuse to form a larger nucleus, energy is released,
since the larger nucleus is more tightly bound, as seen from the binding
energy curve in Fig 13 1 |
9 | 2927-2930 | 2 Nuclear fusion – energy generation in stars
When two light nuclei fuse to form a larger nucleus, energy is released,
since the larger nucleus is more tightly bound, as seen from the binding
energy curve in Fig 13 1 Some examples of such energy liberating nuclear
fusion reactions are :
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 |
9 | 2928-2931 | 13 1 Some examples of such energy liberating nuclear
fusion reactions are :
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 42 MeV
[13 |
9 | 2929-2932 | 1 Some examples of such energy liberating nuclear
fusion reactions are :
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 42 MeV
[13 13(a)]
2
2
3
1
1
2
H
H
He
+
→
+ n + 3 |
9 | 2930-2933 | Some examples of such energy liberating nuclear
fusion reactions are :
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 42 MeV
[13 13(a)]
2
2
3
1
1
2
H
H
He
+
→
+ n + 3 27 MeV
[13 |
9 | 2931-2934 | 42 MeV
[13 13(a)]
2
2
3
1
1
2
H
H
He
+
→
+ n + 3 27 MeV
[13 13(b)]
2
2
3
1
1
1
1
1
H
H
H
H
+
→
+
+ 4 |
9 | 2932-2935 | 13(a)]
2
2
3
1
1
2
H
H
He
+
→
+ n + 3 27 MeV
[13 13(b)]
2
2
3
1
1
1
1
1
H
H
H
H
+
→
+
+ 4 03 MeV
[13 |
9 | 2933-2936 | 27 MeV
[13 13(b)]
2
2
3
1
1
1
1
1
H
H
H
H
+
→
+
+ 4 03 MeV
[13 13(c)]
In the first reaction, two protons combine to form a deuteron and
a positron with a release of 0 |
9 | 2934-2937 | 13(b)]
2
2
3
1
1
1
1
1
H
H
H
H
+
→
+
+ 4 03 MeV
[13 13(c)]
In the first reaction, two protons combine to form a deuteron and
a positron with a release of 0 42 MeV energy |
9 | 2935-2938 | 03 MeV
[13 13(c)]
In the first reaction, two protons combine to form a deuteron and
a positron with a release of 0 42 MeV energy In reaction [13 |
9 | 2936-2939 | 13(c)]
In the first reaction, two protons combine to form a deuteron and
a positron with a release of 0 42 MeV energy In reaction [13 13(b)], two
Rationalised 2023-24
Physics
316
deuterons combine to form the light isotope of helium |
9 | 2937-2940 | 42 MeV energy In reaction [13 13(b)], two
Rationalised 2023-24
Physics
316
deuterons combine to form the light isotope of helium In reaction
(13 |
9 | 2938-2941 | In reaction [13 13(b)], two
Rationalised 2023-24
Physics
316
deuterons combine to form the light isotope of helium In reaction
(13 13c), two deuterons combine to form a triton and a proton |
Subsets and Splits