Chapter
stringclasses 18
values | sentence_range
stringlengths 3
9
| Text
stringlengths 7
7.34k
|
|---|---|---|
9 | 3039-3042 | The atomic mass
of an element is a weighted average of the masses of its isotopes and
calculated in accordance to the relative abundances of the isotopes 5 A nucleus can be considered to be spherical in shape and assigned a
radius Electron scattering experiments allow determination of the
nuclear radius; it is found that radii of nuclei fit the formula
R = R0 A1/3,
where R0 = a constant = 1 |
9 | 3040-3043 | 5 A nucleus can be considered to be spherical in shape and assigned a
radius Electron scattering experiments allow determination of the
nuclear radius; it is found that radii of nuclei fit the formula
R = R0 A1/3,
where R0 = a constant = 1 2 fm |
9 | 3041-3044 | A nucleus can be considered to be spherical in shape and assigned a
radius Electron scattering experiments allow determination of the
nuclear radius; it is found that radii of nuclei fit the formula
R = R0 A1/3,
where R0 = a constant = 1 2 fm This implies that the nuclear density
is independent of A |
9 | 3042-3045 | Electron scattering experiments allow determination of the
nuclear radius; it is found that radii of nuclei fit the formula
R = R0 A1/3,
where R0 = a constant = 1 2 fm This implies that the nuclear density
is independent of A It is of the order of 1017 kg/m3 |
9 | 3043-3046 | 2 fm This implies that the nuclear density
is independent of A It is of the order of 1017 kg/m3 6 |
9 | 3044-3047 | This implies that the nuclear density
is independent of A It is of the order of 1017 kg/m3 6 Neutrons and protons are bound in a nucleus by the short-range strong
nuclear force |
9 | 3045-3048 | It is of the order of 1017 kg/m3 6 Neutrons and protons are bound in a nucleus by the short-range strong
nuclear force The nuclear force does not distinguish between neutron
and proton |
9 | 3046-3049 | 6 Neutrons and protons are bound in a nucleus by the short-range strong
nuclear force The nuclear force does not distinguish between neutron
and proton Rationalised 2023-24
319
Nuclei
7 |
9 | 3047-3050 | Neutrons and protons are bound in a nucleus by the short-range strong
nuclear force The nuclear force does not distinguish between neutron
and proton Rationalised 2023-24
319
Nuclei
7 The nuclear mass M is always less than the total mass, Sm, of its
constituents |
9 | 3048-3051 | The nuclear force does not distinguish between neutron
and proton Rationalised 2023-24
319
Nuclei
7 The nuclear mass M is always less than the total mass, Sm, of its
constituents The difference in mass of a nucleus and its constituents
is called the mass defect,
DM = (Z mp + (A – Z )mn) – M
Using Einstein’s mass energy relation, we express this mass difference
in terms of energy as
DEb = DM c2
The energy DEb represents the binding energy of the nucleus |
9 | 3049-3052 | Rationalised 2023-24
319
Nuclei
7 The nuclear mass M is always less than the total mass, Sm, of its
constituents The difference in mass of a nucleus and its constituents
is called the mass defect,
DM = (Z mp + (A – Z )mn) – M
Using Einstein’s mass energy relation, we express this mass difference
in terms of energy as
DEb = DM c2
The energy DEb represents the binding energy of the nucleus In the
mass number range A = 30 to 170, the binding energy per nucleon is
nearly constant, about 8 MeV/nucleon |
9 | 3050-3053 | The nuclear mass M is always less than the total mass, Sm, of its
constituents The difference in mass of a nucleus and its constituents
is called the mass defect,
DM = (Z mp + (A – Z )mn) – M
Using Einstein’s mass energy relation, we express this mass difference
in terms of energy as
DEb = DM c2
The energy DEb represents the binding energy of the nucleus In the
mass number range A = 30 to 170, the binding energy per nucleon is
nearly constant, about 8 MeV/nucleon 8 |
9 | 3051-3054 | The difference in mass of a nucleus and its constituents
is called the mass defect,
DM = (Z mp + (A – Z )mn) – M
Using Einstein’s mass energy relation, we express this mass difference
in terms of energy as
DEb = DM c2
The energy DEb represents the binding energy of the nucleus In the
mass number range A = 30 to 170, the binding energy per nucleon is
nearly constant, about 8 MeV/nucleon 8 Energies associated with nuclear processes are about a million times
larger than chemical process |
9 | 3052-3055 | In the
mass number range A = 30 to 170, the binding energy per nucleon is
nearly constant, about 8 MeV/nucleon 8 Energies associated with nuclear processes are about a million times
larger than chemical process 9 |
9 | 3053-3056 | 8 Energies associated with nuclear processes are about a million times
larger than chemical process 9 The Q-value of a nuclear process is
Q = final kinetic energy – initial kinetic energy |
9 | 3054-3057 | Energies associated with nuclear processes are about a million times
larger than chemical process 9 The Q-value of a nuclear process is
Q = final kinetic energy – initial kinetic energy Due to conservation of mass-energy, this is also,
Q = (sum of initial masses – sum of final masses)c2
10 |
9 | 3055-3058 | 9 The Q-value of a nuclear process is
Q = final kinetic energy – initial kinetic energy Due to conservation of mass-energy, this is also,
Q = (sum of initial masses – sum of final masses)c2
10 Radioactivity is the phenomenon in which nuclei of a given species
transform by giving out a or b or g rays; a-rays are helium nuclei;
b-rays are electrons |
9 | 3056-3059 | The Q-value of a nuclear process is
Q = final kinetic energy – initial kinetic energy Due to conservation of mass-energy, this is also,
Q = (sum of initial masses – sum of final masses)c2
10 Radioactivity is the phenomenon in which nuclei of a given species
transform by giving out a or b or g rays; a-rays are helium nuclei;
b-rays are electrons g-rays are electromagnetic radiation of wavelengths
shorter than X-rays |
9 | 3057-3060 | Due to conservation of mass-energy, this is also,
Q = (sum of initial masses – sum of final masses)c2
10 Radioactivity is the phenomenon in which nuclei of a given species
transform by giving out a or b or g rays; a-rays are helium nuclei;
b-rays are electrons g-rays are electromagnetic radiation of wavelengths
shorter than X-rays 11 |
9 | 3058-3061 | Radioactivity is the phenomenon in which nuclei of a given species
transform by giving out a or b or g rays; a-rays are helium nuclei;
b-rays are electrons g-rays are electromagnetic radiation of wavelengths
shorter than X-rays 11 Energy is released when less tightly bound nuclei are transmuted into
more tightly bound nuclei |
9 | 3059-3062 | g-rays are electromagnetic radiation of wavelengths
shorter than X-rays 11 Energy is released when less tightly bound nuclei are transmuted into
more tightly bound nuclei In fission, a heavy nucleus like 235
92 U breaks
into two smaller fragments, e |
9 | 3060-3063 | 11 Energy is released when less tightly bound nuclei are transmuted into
more tightly bound nuclei In fission, a heavy nucleus like 235
92 U breaks
into two smaller fragments, e g |
9 | 3061-3064 | Energy is released when less tightly bound nuclei are transmuted into
more tightly bound nuclei In fission, a heavy nucleus like 235
92 U breaks
into two smaller fragments, e g , 235
1
133
99
1
92
0
51
41
0
U+ n
Sb
Nb + 4 n
→
+
12 |
9 | 3062-3065 | In fission, a heavy nucleus like 235
92 U breaks
into two smaller fragments, e g , 235
1
133
99
1
92
0
51
41
0
U+ n
Sb
Nb + 4 n
→
+
12 In fusion, lighter nuclei combine to form a larger nucleus |
9 | 3063-3066 | g , 235
1
133
99
1
92
0
51
41
0
U+ n
Sb
Nb + 4 n
→
+
12 In fusion, lighter nuclei combine to form a larger nucleus Fusion of
hydrogen nuclei into helium nuclei is the source of energy of all stars
including our sun |
9 | 3064-3067 | , 235
1
133
99
1
92
0
51
41
0
U+ n
Sb
Nb + 4 n
→
+
12 In fusion, lighter nuclei combine to form a larger nucleus Fusion of
hydrogen nuclei into helium nuclei is the source of energy of all stars
including our sun Physical Quantity
Symbol
Dimensions
Units
Remarks
Atomic mass unit
[M]
u
Unit of mass for
expressing atomic or
nuclear masses |
9 | 3065-3068 | In fusion, lighter nuclei combine to form a larger nucleus Fusion of
hydrogen nuclei into helium nuclei is the source of energy of all stars
including our sun Physical Quantity
Symbol
Dimensions
Units
Remarks
Atomic mass unit
[M]
u
Unit of mass for
expressing atomic or
nuclear masses One
atomic mass unit equals
1/12th of the mass of 12C
atom |
9 | 3066-3069 | Fusion of
hydrogen nuclei into helium nuclei is the source of energy of all stars
including our sun Physical Quantity
Symbol
Dimensions
Units
Remarks
Atomic mass unit
[M]
u
Unit of mass for
expressing atomic or
nuclear masses One
atomic mass unit equals
1/12th of the mass of 12C
atom Disintegration or
l
[T –1]
s–1
decay constant
Half-life
T1/2
[T]
s
Time taken for the decay
of one-half of the initial
number of nuclei present
in a radioactive sample |
9 | 3067-3070 | Physical Quantity
Symbol
Dimensions
Units
Remarks
Atomic mass unit
[M]
u
Unit of mass for
expressing atomic or
nuclear masses One
atomic mass unit equals
1/12th of the mass of 12C
atom Disintegration or
l
[T –1]
s–1
decay constant
Half-life
T1/2
[T]
s
Time taken for the decay
of one-half of the initial
number of nuclei present
in a radioactive sample Mean life
t
[T]
s
Time at which number of
nuclei has been reduced to
e–1 of its initial value
Activity of a radio-
R
[ T–1]
Bq
Measure of the activity
active sample
of a radioactive source |
9 | 3068-3071 | One
atomic mass unit equals
1/12th of the mass of 12C
atom Disintegration or
l
[T –1]
s–1
decay constant
Half-life
T1/2
[T]
s
Time taken for the decay
of one-half of the initial
number of nuclei present
in a radioactive sample Mean life
t
[T]
s
Time at which number of
nuclei has been reduced to
e–1 of its initial value
Activity of a radio-
R
[ T–1]
Bq
Measure of the activity
active sample
of a radioactive source Rationalised 2023-24
Physics
320
POINTS TO PONDER
1 |
9 | 3069-3072 | Disintegration or
l
[T –1]
s–1
decay constant
Half-life
T1/2
[T]
s
Time taken for the decay
of one-half of the initial
number of nuclei present
in a radioactive sample Mean life
t
[T]
s
Time at which number of
nuclei has been reduced to
e–1 of its initial value
Activity of a radio-
R
[ T–1]
Bq
Measure of the activity
active sample
of a radioactive source Rationalised 2023-24
Physics
320
POINTS TO PONDER
1 The density of nuclear matter is independent of the size of the nucleus |
9 | 3070-3073 | Mean life
t
[T]
s
Time at which number of
nuclei has been reduced to
e–1 of its initial value
Activity of a radio-
R
[ T–1]
Bq
Measure of the activity
active sample
of a radioactive source Rationalised 2023-24
Physics
320
POINTS TO PONDER
1 The density of nuclear matter is independent of the size of the nucleus The mass density of the atom does not follow this rule |
9 | 3071-3074 | Rationalised 2023-24
Physics
320
POINTS TO PONDER
1 The density of nuclear matter is independent of the size of the nucleus The mass density of the atom does not follow this rule 2 |
9 | 3072-3075 | The density of nuclear matter is independent of the size of the nucleus The mass density of the atom does not follow this rule 2 The radius of a nucleus determined by electron scattering is found to
be slightly different from that determined by alpha-particle scattering |
9 | 3073-3076 | The mass density of the atom does not follow this rule 2 The radius of a nucleus determined by electron scattering is found to
be slightly different from that determined by alpha-particle scattering This is because electron scattering senses the charge distribution of
the nucleus, whereas alpha and similar particles sense the nuclear
matter |
9 | 3074-3077 | 2 The radius of a nucleus determined by electron scattering is found to
be slightly different from that determined by alpha-particle scattering This is because electron scattering senses the charge distribution of
the nucleus, whereas alpha and similar particles sense the nuclear
matter 3 |
9 | 3075-3078 | The radius of a nucleus determined by electron scattering is found to
be slightly different from that determined by alpha-particle scattering This is because electron scattering senses the charge distribution of
the nucleus, whereas alpha and similar particles sense the nuclear
matter 3 After Einstein showed the equivalence of mass and energy, E = mc 2,
we cannot any longer speak of separate laws of conservation of mass
and conservation of energy, but we have to speak of a unified law of
conservation of mass and energy |
9 | 3076-3079 | This is because electron scattering senses the charge distribution of
the nucleus, whereas alpha and similar particles sense the nuclear
matter 3 After Einstein showed the equivalence of mass and energy, E = mc 2,
we cannot any longer speak of separate laws of conservation of mass
and conservation of energy, but we have to speak of a unified law of
conservation of mass and energy The most convincing evidence that
this principle operates in nature comes from nuclear physics |
9 | 3077-3080 | 3 After Einstein showed the equivalence of mass and energy, E = mc 2,
we cannot any longer speak of separate laws of conservation of mass
and conservation of energy, but we have to speak of a unified law of
conservation of mass and energy The most convincing evidence that
this principle operates in nature comes from nuclear physics It is
central to our understanding of nuclear energy and harnessing it as a
source of power |
9 | 3078-3081 | After Einstein showed the equivalence of mass and energy, E = mc 2,
we cannot any longer speak of separate laws of conservation of mass
and conservation of energy, but we have to speak of a unified law of
conservation of mass and energy The most convincing evidence that
this principle operates in nature comes from nuclear physics It is
central to our understanding of nuclear energy and harnessing it as a
source of power Using the principle, Q of a nuclear process (decay or
reaction) can be expressed also in terms of initial and final masses |
9 | 3079-3082 | The most convincing evidence that
this principle operates in nature comes from nuclear physics It is
central to our understanding of nuclear energy and harnessing it as a
source of power Using the principle, Q of a nuclear process (decay or
reaction) can be expressed also in terms of initial and final masses 4 |
9 | 3080-3083 | It is
central to our understanding of nuclear energy and harnessing it as a
source of power Using the principle, Q of a nuclear process (decay or
reaction) can be expressed also in terms of initial and final masses 4 The nature of the binding energy (per nucleon) curve shows that
exothermic nuclear reactions are possible, when two light nuclei fuse
or when a heavy nucleus undergoes fission into nuclei with intermediate
mass |
9 | 3081-3084 | Using the principle, Q of a nuclear process (decay or
reaction) can be expressed also in terms of initial and final masses 4 The nature of the binding energy (per nucleon) curve shows that
exothermic nuclear reactions are possible, when two light nuclei fuse
or when a heavy nucleus undergoes fission into nuclei with intermediate
mass 5 |
9 | 3082-3085 | 4 The nature of the binding energy (per nucleon) curve shows that
exothermic nuclear reactions are possible, when two light nuclei fuse
or when a heavy nucleus undergoes fission into nuclei with intermediate
mass 5 For fusion, the light nuclei must have sufficient initial energy to
overcome the coulomb potential barrier |
9 | 3083-3086 | The nature of the binding energy (per nucleon) curve shows that
exothermic nuclear reactions are possible, when two light nuclei fuse
or when a heavy nucleus undergoes fission into nuclei with intermediate
mass 5 For fusion, the light nuclei must have sufficient initial energy to
overcome the coulomb potential barrier That is why fusion requires
very high temperatures |
9 | 3084-3087 | 5 For fusion, the light nuclei must have sufficient initial energy to
overcome the coulomb potential barrier That is why fusion requires
very high temperatures 6 |
9 | 3085-3088 | For fusion, the light nuclei must have sufficient initial energy to
overcome the coulomb potential barrier That is why fusion requires
very high temperatures 6 Although the binding energy (per nucleon) curve is smooth and slowly
varying, it shows peaks at nuclides like 4He, 16O etc |
9 | 3086-3089 | That is why fusion requires
very high temperatures 6 Although the binding energy (per nucleon) curve is smooth and slowly
varying, it shows peaks at nuclides like 4He, 16O etc This is considered
as evidence of atom-like shell structure in nuclei |
9 | 3087-3090 | 6 Although the binding energy (per nucleon) curve is smooth and slowly
varying, it shows peaks at nuclides like 4He, 16O etc This is considered
as evidence of atom-like shell structure in nuclei 7 |
9 | 3088-3091 | Although the binding energy (per nucleon) curve is smooth and slowly
varying, it shows peaks at nuclides like 4He, 16O etc This is considered
as evidence of atom-like shell structure in nuclei 7 Electrons and positron are a particle-antiparticle pair |
9 | 3089-3092 | This is considered
as evidence of atom-like shell structure in nuclei 7 Electrons and positron are a particle-antiparticle pair They are
identical in mass; their charges are equal in magnitude and opposite |
9 | 3090-3093 | 7 Electrons and positron are a particle-antiparticle pair They are
identical in mass; their charges are equal in magnitude and opposite (It is found that when an electron and a positron come together, they
annihilate each other giving energy in the form of gamma-ray photons |
9 | 3091-3094 | Electrons and positron are a particle-antiparticle pair They are
identical in mass; their charges are equal in magnitude and opposite (It is found that when an electron and a positron come together, they
annihilate each other giving energy in the form of gamma-ray photons )
8 |
9 | 3092-3095 | They are
identical in mass; their charges are equal in magnitude and opposite (It is found that when an electron and a positron come together, they
annihilate each other giving energy in the form of gamma-ray photons )
8 Radioactivity is an indication of the instability of nuclei |
9 | 3093-3096 | (It is found that when an electron and a positron come together, they
annihilate each other giving energy in the form of gamma-ray photons )
8 Radioactivity is an indication of the instability of nuclei Stability
requires the ratio of neutron to proton to be around 1:1 for light
nuclei |
9 | 3094-3097 | )
8 Radioactivity is an indication of the instability of nuclei Stability
requires the ratio of neutron to proton to be around 1:1 for light
nuclei This ratio increases to about 3:2 for heavy nuclei |
9 | 3095-3098 | Radioactivity is an indication of the instability of nuclei Stability
requires the ratio of neutron to proton to be around 1:1 for light
nuclei This ratio increases to about 3:2 for heavy nuclei (More
neutrons are required to overcome the effect of repulsion among the
protons |
9 | 3096-3099 | Stability
requires the ratio of neutron to proton to be around 1:1 for light
nuclei This ratio increases to about 3:2 for heavy nuclei (More
neutrons are required to overcome the effect of repulsion among the
protons ) Nuclei which are away from the stability ratio, i |
9 | 3097-3100 | This ratio increases to about 3:2 for heavy nuclei (More
neutrons are required to overcome the effect of repulsion among the
protons ) Nuclei which are away from the stability ratio, i e |
9 | 3098-3101 | (More
neutrons are required to overcome the effect of repulsion among the
protons ) Nuclei which are away from the stability ratio, i e , nuclei
which have an excess of neutrons or protons are unstable |
9 | 3099-3102 | ) Nuclei which are away from the stability ratio, i e , nuclei
which have an excess of neutrons or protons are unstable In fact,
only about 10% of knon isotopes (of all elements), are stable |
9 | 3100-3103 | e , nuclei
which have an excess of neutrons or protons are unstable In fact,
only about 10% of knon isotopes (of all elements), are stable Others
have been either artificially produced in the laboratory by bombarding
a, p, d, n or other particles on targets of stable nuclear species or
identified in astronomical observations of matter in the universe |
9 | 3101-3104 | , nuclei
which have an excess of neutrons or protons are unstable In fact,
only about 10% of knon isotopes (of all elements), are stable Others
have been either artificially produced in the laboratory by bombarding
a, p, d, n or other particles on targets of stable nuclear species or
identified in astronomical observations of matter in the universe Rationalised 2023-24
321
Nuclei
EXERCISES
You may find the following data useful in solving the exercises:
e = 1 |
9 | 3102-3105 | In fact,
only about 10% of knon isotopes (of all elements), are stable Others
have been either artificially produced in the laboratory by bombarding
a, p, d, n or other particles on targets of stable nuclear species or
identified in astronomical observations of matter in the universe Rationalised 2023-24
321
Nuclei
EXERCISES
You may find the following data useful in solving the exercises:
e = 1 6×10–19C
N
= 6 |
9 | 3103-3106 | Others
have been either artificially produced in the laboratory by bombarding
a, p, d, n or other particles on targets of stable nuclear species or
identified in astronomical observations of matter in the universe Rationalised 2023-24
321
Nuclei
EXERCISES
You may find the following data useful in solving the exercises:
e = 1 6×10–19C
N
= 6 023×1023 per mole
1/(4pe0) = 9 × 109 N m2/C2
k
= 1 |
9 | 3104-3107 | Rationalised 2023-24
321
Nuclei
EXERCISES
You may find the following data useful in solving the exercises:
e = 1 6×10–19C
N
= 6 023×1023 per mole
1/(4pe0) = 9 × 109 N m2/C2
k
= 1 381×10–23J K–1
1 MeV = 1 |
9 | 3105-3108 | 6×10–19C
N
= 6 023×1023 per mole
1/(4pe0) = 9 × 109 N m2/C2
k
= 1 381×10–23J K–1
1 MeV = 1 6×10–13J
1 u = 931 |
9 | 3106-3109 | 023×1023 per mole
1/(4pe0) = 9 × 109 N m2/C2
k
= 1 381×10–23J K–1
1 MeV = 1 6×10–13J
1 u = 931 5 MeV/c2
1 year = 3 |
9 | 3107-3110 | 381×10–23J K–1
1 MeV = 1 6×10–13J
1 u = 931 5 MeV/c2
1 year = 3 154×107 s
mH = 1 |
9 | 3108-3111 | 6×10–13J
1 u = 931 5 MeV/c2
1 year = 3 154×107 s
mH = 1 007825 u
mn = 1 |
9 | 3109-3112 | 5 MeV/c2
1 year = 3 154×107 s
mH = 1 007825 u
mn = 1 008665 u
m( 4
2He ) = 4 |
9 | 3110-3113 | 154×107 s
mH = 1 007825 u
mn = 1 008665 u
m( 4
2He ) = 4 002603 u
me = 0 |
9 | 3111-3114 | 007825 u
mn = 1 008665 u
m( 4
2He ) = 4 002603 u
me = 0 000548 u
13 |
9 | 3112-3115 | 008665 u
m( 4
2He ) = 4 002603 u
me = 0 000548 u
13 1
Obtain the binding energy (in MeV) of a nitrogen nucleus (
)
14
7 N ,
given m (
)
14
7 N =14 |
9 | 3113-3116 | 002603 u
me = 0 000548 u
13 1
Obtain the binding energy (in MeV) of a nitrogen nucleus (
)
14
7 N ,
given m (
)
14
7 N =14 00307 u
13 |
9 | 3114-3117 | 000548 u
13 1
Obtain the binding energy (in MeV) of a nitrogen nucleus (
)
14
7 N ,
given m (
)
14
7 N =14 00307 u
13 2
Obtain the binding energy of the nuclei 56
26Fe and 209
83 Bi in units of
MeV from the following data:
m ( 56
26Fe ) = 55 |
9 | 3115-3118 | 1
Obtain the binding energy (in MeV) of a nitrogen nucleus (
)
14
7 N ,
given m (
)
14
7 N =14 00307 u
13 2
Obtain the binding energy of the nuclei 56
26Fe and 209
83 Bi in units of
MeV from the following data:
m ( 56
26Fe ) = 55 934939 u m ( 209
83 Bi ) = 208 |
9 | 3116-3119 | 00307 u
13 2
Obtain the binding energy of the nuclei 56
26Fe and 209
83 Bi in units of
MeV from the following data:
m ( 56
26Fe ) = 55 934939 u m ( 209
83 Bi ) = 208 980388 u
13 |
9 | 3117-3120 | 2
Obtain the binding energy of the nuclei 56
26Fe and 209
83 Bi in units of
MeV from the following data:
m ( 56
26Fe ) = 55 934939 u m ( 209
83 Bi ) = 208 980388 u
13 3
A given coin has a mass of 3 |
9 | 3118-3121 | 934939 u m ( 209
83 Bi ) = 208 980388 u
13 3
A given coin has a mass of 3 0 g |
9 | 3119-3122 | 980388 u
13 3
A given coin has a mass of 3 0 g Calculate the nuclear energy that
would be required to separate all the neutrons and protons from
each other |
9 | 3120-3123 | 3
A given coin has a mass of 3 0 g Calculate the nuclear energy that
would be required to separate all the neutrons and protons from
each other For simplicity assume that the coin is entirely made of
63
29Cu atoms (of mass 62 |
9 | 3121-3124 | 0 g Calculate the nuclear energy that
would be required to separate all the neutrons and protons from
each other For simplicity assume that the coin is entirely made of
63
29Cu atoms (of mass 62 92960 u) |
9 | 3122-3125 | Calculate the nuclear energy that
would be required to separate all the neutrons and protons from
each other For simplicity assume that the coin is entirely made of
63
29Cu atoms (of mass 62 92960 u) 13 |
9 | 3123-3126 | For simplicity assume that the coin is entirely made of
63
29Cu atoms (of mass 62 92960 u) 13 4
Obtain approximately the ratio of the nuclear radii of the gold isotope
197
79 Au and the silver isotope 107
47 Ag |
9 | 3124-3127 | 92960 u) 13 4
Obtain approximately the ratio of the nuclear radii of the gold isotope
197
79 Au and the silver isotope 107
47 Ag 13 |
9 | 3125-3128 | 13 4
Obtain approximately the ratio of the nuclear radii of the gold isotope
197
79 Au and the silver isotope 107
47 Ag 13 5
The Q value of a nuclear reaction A + b ® C + d is defined by
Q = [ mA + mb – mC – md]c2
where the masses refer to the respective nuclei |
9 | 3126-3129 | 4
Obtain approximately the ratio of the nuclear radii of the gold isotope
197
79 Au and the silver isotope 107
47 Ag 13 5
The Q value of a nuclear reaction A + b ® C + d is defined by
Q = [ mA + mb – mC – md]c2
where the masses refer to the respective nuclei Determine from the
given data the Q-value of the following reactions and state whether
the reactions are exothermic or endothermic |
9 | 3127-3130 | 13 5
The Q value of a nuclear reaction A + b ® C + d is defined by
Q = [ mA + mb – mC – md]c2
where the masses refer to the respective nuclei Determine from the
given data the Q-value of the following reactions and state whether
the reactions are exothermic or endothermic (i) 1
3
2
2
1
1
1
1
H+ H
H+ H
→
(ii) 12
12
20
4
6
6
10
2
C+ C
Ne+ He
→
Atomic masses are given to be
m ( 2
m ( 31 H ) = 2 |
9 | 3128-3131 | 5
The Q value of a nuclear reaction A + b ® C + d is defined by
Q = [ mA + mb – mC – md]c2
where the masses refer to the respective nuclei Determine from the
given data the Q-value of the following reactions and state whether
the reactions are exothermic or endothermic (i) 1
3
2
2
1
1
1
1
H+ H
H+ H
→
(ii) 12
12
20
4
6
6
10
2
C+ C
Ne+ He
→
Atomic masses are given to be
m ( 2
m ( 31 H ) = 2 014102 u
1 H) = 3 |
9 | 3129-3132 | Determine from the
given data the Q-value of the following reactions and state whether
the reactions are exothermic or endothermic (i) 1
3
2
2
1
1
1
1
H+ H
H+ H
→
(ii) 12
12
20
4
6
6
10
2
C+ C
Ne+ He
→
Atomic masses are given to be
m ( 2
m ( 31 H ) = 2 014102 u
1 H) = 3 016049 u
m ( 12
m ( 206 C ) = 12 |
9 | 3130-3133 | (i) 1
3
2
2
1
1
1
1
H+ H
H+ H
→
(ii) 12
12
20
4
6
6
10
2
C+ C
Ne+ He
→
Atomic masses are given to be
m ( 2
m ( 31 H ) = 2 014102 u
1 H) = 3 016049 u
m ( 12
m ( 206 C ) = 12 000000 u
10 Ne ) = 19 |
9 | 3131-3134 | 014102 u
1 H) = 3 016049 u
m ( 12
m ( 206 C ) = 12 000000 u
10 Ne ) = 19 992439 u
13 |
9 | 3132-3135 | 016049 u
m ( 12
m ( 206 C ) = 12 000000 u
10 Ne ) = 19 992439 u
13 6
Suppose, we think of fission of a 56
26Fe nucleus into two equal
fragments, 28
13 Al |
9 | 3133-3136 | 000000 u
10 Ne ) = 19 992439 u
13 6
Suppose, we think of fission of a 56
26Fe nucleus into two equal
fragments, 28
13 Al Is the fission energetically possible |
9 | 3134-3137 | 992439 u
13 6
Suppose, we think of fission of a 56
26Fe nucleus into two equal
fragments, 28
13 Al Is the fission energetically possible Argue by
working out Q of the process |
9 | 3135-3138 | 6
Suppose, we think of fission of a 56
26Fe nucleus into two equal
fragments, 28
13 Al Is the fission energetically possible Argue by
working out Q of the process Given m ( 56
26Fe ) = 55 |
9 | 3136-3139 | Is the fission energetically possible Argue by
working out Q of the process Given m ( 56
26Fe ) = 55 93494 u and
m ( 28
13 Al ) = 27 |
9 | 3137-3140 | Argue by
working out Q of the process Given m ( 56
26Fe ) = 55 93494 u and
m ( 28
13 Al ) = 27 98191 u |
9 | 3138-3141 | Given m ( 56
26Fe ) = 55 93494 u and
m ( 28
13 Al ) = 27 98191 u Rationalised 2023-24
Physics
322
13 |
Subsets and Splits