Chapter
stringclasses 18
values | sentence_range
stringlengths 3
9
| Text
stringlengths 7
7.34k
|
|---|---|---|
9 | 2939-2942 | 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 For
fusion to take place, the two nuclei must come close enough so that
attractive short-range nuclear force is able to affect them |
9 | 2940-2943 | In reaction
(13 13c), two deuterons combine to form a triton and a proton For
fusion to take place, the two nuclei must come close enough so that
attractive short-range nuclear force is able to affect them However,
since they are both positively charged particles, they experience coulomb
repulsion |
9 | 2941-2944 | 13c), two deuterons combine to form a triton and a proton For
fusion to take place, the two nuclei must come close enough so that
attractive short-range nuclear force is able to affect them However,
since they are both positively charged particles, they experience coulomb
repulsion They, therefore, must have enough energy to overcome this
coulomb barrier |
9 | 2942-2945 | For
fusion to take place, the two nuclei must come close enough so that
attractive short-range nuclear force is able to affect them However,
since they are both positively charged particles, they experience coulomb
repulsion They, therefore, must have enough energy to overcome this
coulomb barrier The height of the barrier depends on the charges and
radii of the two interacting nuclei |
9 | 2943-2946 | However,
since they are both positively charged particles, they experience coulomb
repulsion They, therefore, must have enough energy to overcome this
coulomb barrier The height of the barrier depends on the charges and
radii of the two interacting nuclei It can be shown, for example, that
the barrier height for two protons is ~ 400 keV, and is higher for nuclei
with higher charges |
9 | 2944-2947 | They, therefore, must have enough energy to overcome this
coulomb barrier The height of the barrier depends on the charges and
radii of the two interacting nuclei It can be shown, for example, that
the barrier height for two protons is ~ 400 keV, and is higher for nuclei
with higher charges We can estimate the temperature at which two
protons in a proton gas would (averagely) have enough energy to
overcome the coulomb barrier:
(3/2)k T = K ≃ 400 keV, which gives T ~ 3 × 109 K |
9 | 2945-2948 | The height of the barrier depends on the charges and
radii of the two interacting nuclei It can be shown, for example, that
the barrier height for two protons is ~ 400 keV, and is higher for nuclei
with higher charges We can estimate the temperature at which two
protons in a proton gas would (averagely) have enough energy to
overcome the coulomb barrier:
(3/2)k T = K ≃ 400 keV, which gives T ~ 3 × 109 K When fusion is achieved by raising the temperature of the system so
that particles have enough kinetic energy to overcome the coulomb
repulsive behaviour, it is called thermonuclear fusion |
9 | 2946-2949 | It can be shown, for example, that
the barrier height for two protons is ~ 400 keV, and is higher for nuclei
with higher charges We can estimate the temperature at which two
protons in a proton gas would (averagely) have enough energy to
overcome the coulomb barrier:
(3/2)k T = K ≃ 400 keV, which gives T ~ 3 × 109 K When fusion is achieved by raising the temperature of the system so
that particles have enough kinetic energy to overcome the coulomb
repulsive behaviour, it is called thermonuclear fusion Thermonuclear fusion is the source of energy output in the interior
of stars |
9 | 2947-2950 | We can estimate the temperature at which two
protons in a proton gas would (averagely) have enough energy to
overcome the coulomb barrier:
(3/2)k T = K ≃ 400 keV, which gives T ~ 3 × 109 K When fusion is achieved by raising the temperature of the system so
that particles have enough kinetic energy to overcome the coulomb
repulsive behaviour, it is called thermonuclear fusion Thermonuclear fusion is the source of energy output in the interior
of stars The interior of the sun has a temperature of 1 |
9 | 2948-2951 | When fusion is achieved by raising the temperature of the system so
that particles have enough kinetic energy to overcome the coulomb
repulsive behaviour, it is called thermonuclear fusion Thermonuclear fusion is the source of energy output in the interior
of stars The interior of the sun has a temperature of 1 5×107 K, which
is considerably less than the estimated temperature required for fusion
of particles of average energy |
9 | 2949-2952 | Thermonuclear fusion is the source of energy output in the interior
of stars The interior of the sun has a temperature of 1 5×107 K, which
is considerably less than the estimated temperature required for fusion
of particles of average energy Clearly, fusion in the sun involves protons
whose energies are much above the average energy |
9 | 2950-2953 | The interior of the sun has a temperature of 1 5×107 K, which
is considerably less than the estimated temperature required for fusion
of particles of average energy Clearly, fusion in the sun involves protons
whose energies are much above the average energy The fusion reaction in the sun is a multi-step process in which the
hydrogen is burned into helium |
9 | 2951-2954 | 5×107 K, which
is considerably less than the estimated temperature required for fusion
of particles of average energy Clearly, fusion in the sun involves protons
whose energies are much above the average energy The fusion reaction in the sun is a multi-step process in which the
hydrogen is burned into helium Thus, the fuel in the sun is the hydrogen
in its core |
9 | 2952-2955 | Clearly, fusion in the sun involves protons
whose energies are much above the average energy The fusion reaction in the sun is a multi-step process in which the
hydrogen is burned into helium Thus, the fuel in the sun is the hydrogen
in its core The proton-proton (p, p) cycle by which this occurs is
represented by the following sets of reactions:
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 |
9 | 2953-2956 | The fusion reaction in the sun is a multi-step process in which the
hydrogen is burned into helium Thus, the fuel in the sun is the hydrogen
in its core The proton-proton (p, p) cycle by which this occurs is
represented by the following sets of reactions:
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 42 MeV
(i)
e + + e – ® g + g + 1 |
9 | 2954-2957 | Thus, the fuel in the sun is the hydrogen
in its core The proton-proton (p, p) cycle by which this occurs is
represented by the following sets of reactions:
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 42 MeV
(i)
e + + e – ® g + g + 1 02 MeV
(ii)
2
1
3
1
1
2
H
H
He
+
→
+ g + 5 |
9 | 2955-2958 | The proton-proton (p, p) cycle by which this occurs is
represented by the following sets of reactions:
1
1
2
1
1
1
H
H
H
+
→
+ e+ + n + 0 42 MeV
(i)
e + + e – ® g + g + 1 02 MeV
(ii)
2
1
3
1
1
2
H
H
He
+
→
+ g + 5 49 MeV
(iii)
+
→
+
+
3
3
4
1
1
2
2
2
1
1
He
He
He
H
H + 12 |
9 | 2956-2959 | 42 MeV
(i)
e + + e – ® g + g + 1 02 MeV
(ii)
2
1
3
1
1
2
H
H
He
+
→
+ g + 5 49 MeV
(iii)
+
→
+
+
3
3
4
1
1
2
2
2
1
1
He
He
He
H
H + 12 86 MeV (iv)
(13 |
9 | 2957-2960 | 02 MeV
(ii)
2
1
3
1
1
2
H
H
He
+
→
+ g + 5 49 MeV
(iii)
+
→
+
+
3
3
4
1
1
2
2
2
1
1
He
He
He
H
H + 12 86 MeV (iv)
(13 14)
For the fourth reaction to occur, the first three reactions must occur
twice, in which case two light helium nuclei unite to form ordinary helium
nucleus |
9 | 2958-2961 | 49 MeV
(iii)
+
→
+
+
3
3
4
1
1
2
2
2
1
1
He
He
He
H
H + 12 86 MeV (iv)
(13 14)
For the fourth reaction to occur, the first three reactions must occur
twice, in which case two light helium nuclei unite to form ordinary helium
nucleus If we consider the combination 2(i) + 2(ii) + 2(iii) +(iv), the net
effect is
1
4
1
2
4 H
2
He
2
6
26 |
9 | 2959-2962 | 86 MeV (iv)
(13 14)
For the fourth reaction to occur, the first three reactions must occur
twice, in which case two light helium nuclei unite to form ordinary helium
nucleus If we consider the combination 2(i) + 2(ii) + 2(iii) +(iv), the net
effect is
1
4
1
2
4 H
2
He
2
6
26 7 MeV
e
ν
γ
−
+
→
+
+
+
or
1
4
1
2
(4 H
4
)
( He
2
)
2
6
26 |
9 | 2960-2963 | 14)
For the fourth reaction to occur, the first three reactions must occur
twice, in which case two light helium nuclei unite to form ordinary helium
nucleus If we consider the combination 2(i) + 2(ii) + 2(iii) +(iv), the net
effect is
1
4
1
2
4 H
2
He
2
6
26 7 MeV
e
ν
γ
−
+
→
+
+
+
or
1
4
1
2
(4 H
4
)
( He
2
)
2
6
26 7MeV
e
e
ν
γ
−
−
+
→
+
+
+
+
(13 |
9 | 2961-2964 | If we consider the combination 2(i) + 2(ii) + 2(iii) +(iv), the net
effect is
1
4
1
2
4 H
2
He
2
6
26 7 MeV
e
ν
γ
−
+
→
+
+
+
or
1
4
1
2
(4 H
4
)
( He
2
)
2
6
26 7MeV
e
e
ν
γ
−
−
+
→
+
+
+
+
(13 15)
Thus, four hydrogen atoms combine to form an 4
2He atom with a
release of 26 |
9 | 2962-2965 | 7 MeV
e
ν
γ
−
+
→
+
+
+
or
1
4
1
2
(4 H
4
)
( He
2
)
2
6
26 7MeV
e
e
ν
γ
−
−
+
→
+
+
+
+
(13 15)
Thus, four hydrogen atoms combine to form an 4
2He atom with a
release of 26 7 MeV of energy |
9 | 2963-2966 | 7MeV
e
e
ν
γ
−
−
+
→
+
+
+
+
(13 15)
Thus, four hydrogen atoms combine to form an 4
2He atom with a
release of 26 7 MeV of energy Helium is not the only element that can be synthesized in the interior of
a star |
9 | 2964-2967 | 15)
Thus, four hydrogen atoms combine to form an 4
2He atom with a
release of 26 7 MeV of energy Helium is not the only element that can be synthesized in the interior of
a star As the hydrogen in the core gets depleted and becomes helium, the
core starts to cool |
9 | 2965-2968 | 7 MeV of energy Helium is not the only element that can be synthesized in the interior of
a star As the hydrogen in the core gets depleted and becomes helium, the
core starts to cool The star begins to collapse under its own gravity which
increases the temperature of the core |
9 | 2966-2969 | Helium is not the only element that can be synthesized in the interior of
a star As the hydrogen in the core gets depleted and becomes helium, the
core starts to cool The star begins to collapse under its own gravity which
increases the temperature of the core If this temperature increases to about
108 K, fusion takes place again, this time of helium nuclei into carbon |
9 | 2967-2970 | As the hydrogen in the core gets depleted and becomes helium, the
core starts to cool The star begins to collapse under its own gravity which
increases the temperature of the core If this temperature increases to about
108 K, fusion takes place again, this time of helium nuclei into carbon This kind of process can generate through fusion higher and higher mass
number elements |
9 | 2968-2971 | The star begins to collapse under its own gravity which
increases the temperature of the core If this temperature increases to about
108 K, fusion takes place again, this time of helium nuclei into carbon This kind of process can generate through fusion higher and higher mass
number elements But elements more massive than those near the peak of
the binding energy curve in Fig |
9 | 2969-2972 | If this temperature increases to about
108 K, fusion takes place again, this time of helium nuclei into carbon This kind of process can generate through fusion higher and higher mass
number elements But elements more massive than those near the peak of
the binding energy curve in Fig 13 |
9 | 2970-2973 | This kind of process can generate through fusion higher and higher mass
number elements But elements more massive than those near the peak of
the binding energy curve in Fig 13 1 cannot be so produced |
9 | 2971-2974 | But elements more massive than those near the peak of
the binding energy curve in Fig 13 1 cannot be so produced Rationalised 2023-24
317
Nuclei
The age of the sun is about 5×109 y and it is estimated that there is
enough hydrogen in the sun to keep it going for another 5 billion years |
9 | 2972-2975 | 13 1 cannot be so produced Rationalised 2023-24
317
Nuclei
The age of the sun is about 5×109 y and it is estimated that there is
enough hydrogen in the sun to keep it going for another 5 billion years After that, the hydrogen burning will stop and the sun will begin to cool
and will start to collapse under gravity, which will raise the core
temperature |
9 | 2973-2976 | 1 cannot be so produced Rationalised 2023-24
317
Nuclei
The age of the sun is about 5×109 y and it is estimated that there is
enough hydrogen in the sun to keep it going for another 5 billion years After that, the hydrogen burning will stop and the sun will begin to cool
and will start to collapse under gravity, which will raise the core
temperature The outer envelope of the sun will expand, turning it into
the so called red giant |
9 | 2974-2977 | Rationalised 2023-24
317
Nuclei
The age of the sun is about 5×109 y and it is estimated that there is
enough hydrogen in the sun to keep it going for another 5 billion years After that, the hydrogen burning will stop and the sun will begin to cool
and will start to collapse under gravity, which will raise the core
temperature The outer envelope of the sun will expand, turning it into
the so called red giant 13 |
9 | 2975-2978 | After that, the hydrogen burning will stop and the sun will begin to cool
and will start to collapse under gravity, which will raise the core
temperature The outer envelope of the sun will expand, turning it into
the so called red giant 13 7 |
9 | 2976-2979 | The outer envelope of the sun will expand, turning it into
the so called red giant 13 7 3 Controlled thermonuclear fusion
The natural thermonuclear fusion process in a star is replicated in a
thermonuclear fusion device |
9 | 2977-2980 | 13 7 3 Controlled thermonuclear fusion
The natural thermonuclear fusion process in a star is replicated in a
thermonuclear fusion device In controlled fusion reactors, the aim is to
generate steady power by heating the nuclear fuel to a temperature in the
range of 108 K |
9 | 2978-2981 | 7 3 Controlled thermonuclear fusion
The natural thermonuclear fusion process in a star is replicated in a
thermonuclear fusion device In controlled fusion reactors, the aim is to
generate steady power by heating the nuclear fuel to a temperature in the
range of 108 K At these temperatures, the fuel is a mixture of positive
ions and electrons (plasma) |
9 | 2979-2982 | 3 Controlled thermonuclear fusion
The natural thermonuclear fusion process in a star is replicated in a
thermonuclear fusion device In controlled fusion reactors, the aim is to
generate steady power by heating the nuclear fuel to a temperature in the
range of 108 K At these temperatures, the fuel is a mixture of positive
ions and electrons (plasma) The challenge is to confine this plasma, since
no container can stand such a high temperature |
9 | 2980-2983 | In controlled fusion reactors, the aim is to
generate steady power by heating the nuclear fuel to a temperature in the
range of 108 K At these temperatures, the fuel is a mixture of positive
ions and electrons (plasma) The challenge is to confine this plasma, since
no container can stand such a high temperature Several countries
around the world including India are developing techniques in this
connection |
9 | 2981-2984 | At these temperatures, the fuel is a mixture of positive
ions and electrons (plasma) The challenge is to confine this plasma, since
no container can stand such a high temperature Several countries
around the world including India are developing techniques in this
connection If successful, fusion reactors will hopefully supply almost
unlimited power to humanity |
9 | 2982-2985 | The challenge is to confine this plasma, since
no container can stand such a high temperature Several countries
around the world including India are developing techniques in this
connection If successful, fusion reactors will hopefully supply almost
unlimited power to humanity Example 13 |
9 | 2983-2986 | Several countries
around the world including India are developing techniques in this
connection If successful, fusion reactors will hopefully supply almost
unlimited power to humanity Example 13 4 Answer the following questions:
(a) Are the equations of nuclear reactions (such as those given in
Section 13 |
9 | 2984-2987 | If successful, fusion reactors will hopefully supply almost
unlimited power to humanity Example 13 4 Answer the following questions:
(a) Are the equations of nuclear reactions (such as those given in
Section 13 7) ‘balanced’ in the sense a chemical equation (e |
9 | 2985-2988 | Example 13 4 Answer the following questions:
(a) Are the equations of nuclear reactions (such as those given in
Section 13 7) ‘balanced’ in the sense a chemical equation (e g |
9 | 2986-2989 | 4 Answer the following questions:
(a) Are the equations of nuclear reactions (such as those given in
Section 13 7) ‘balanced’ in the sense a chemical equation (e g ,
2H2 + O2® 2 H2O) is |
9 | 2987-2990 | 7) ‘balanced’ in the sense a chemical equation (e g ,
2H2 + O2® 2 H2O) is If not, in what sense are they balanced on
both sides |
9 | 2988-2991 | g ,
2H2 + O2® 2 H2O) is If not, in what sense are they balanced on
both sides (b) If both the number of protons and the number of neutrons are
conserved in each nuclear reaction, in what way is mass converted
into energy (or vice-versa) in a nuclear reaction |
9 | 2989-2992 | ,
2H2 + O2® 2 H2O) is If not, in what sense are they balanced on
both sides (b) If both the number of protons and the number of neutrons are
conserved in each nuclear reaction, in what way is mass converted
into energy (or vice-versa) in a nuclear reaction (c) A general impression exists that mass-energy interconversion
takes place only in nuclear reaction and never in chemical
reaction |
9 | 2990-2993 | If not, in what sense are they balanced on
both sides (b) If both the number of protons and the number of neutrons are
conserved in each nuclear reaction, in what way is mass converted
into energy (or vice-versa) in a nuclear reaction (c) A general impression exists that mass-energy interconversion
takes place only in nuclear reaction and never in chemical
reaction This is strictly speaking, incorrect |
9 | 2991-2994 | (b) If both the number of protons and the number of neutrons are
conserved in each nuclear reaction, in what way is mass converted
into energy (or vice-versa) in a nuclear reaction (c) A general impression exists that mass-energy interconversion
takes place only in nuclear reaction and never in chemical
reaction This is strictly speaking, incorrect Explain |
9 | 2992-2995 | (c) A general impression exists that mass-energy interconversion
takes place only in nuclear reaction and never in chemical
reaction This is strictly speaking, incorrect Explain Solution
(a) A chemical equation is balanced in the sense that the number of
atoms of each element is the same on both sides of the equation |
9 | 2993-2996 | This is strictly speaking, incorrect Explain Solution
(a) A chemical equation is balanced in the sense that the number of
atoms of each element is the same on both sides of the equation A chemical reaction merely alters the original combinations of
atoms |
9 | 2994-2997 | Explain Solution
(a) A chemical equation is balanced in the sense that the number of
atoms of each element is the same on both sides of the equation A chemical reaction merely alters the original combinations of
atoms In a nuclear reaction, elements may be transmuted |
9 | 2995-2998 | Solution
(a) A chemical equation is balanced in the sense that the number of
atoms of each element is the same on both sides of the equation A chemical reaction merely alters the original combinations of
atoms In a nuclear reaction, elements may be transmuted Thus,
the number of atoms of each element is not necessarily conserved
in a nuclear reaction |
9 | 2996-2999 | A chemical reaction merely alters the original combinations of
atoms In a nuclear reaction, elements may be transmuted Thus,
the number of atoms of each element is not necessarily conserved
in a nuclear reaction However, the number of protons and the
number of neutrons are both separately conserved in a nuclear
reaction |
9 | 2997-3000 | In a nuclear reaction, elements may be transmuted Thus,
the number of atoms of each element is not necessarily conserved
in a nuclear reaction However, the number of protons and the
number of neutrons are both separately conserved in a nuclear
reaction [Actually, even this is not strictly true in the realm of
very high energies – what is strictly conserved is the total charge
and total ‘baryon number’ |
9 | 2998-3001 | Thus,
the number of atoms of each element is not necessarily conserved
in a nuclear reaction However, the number of protons and the
number of neutrons are both separately conserved in a nuclear
reaction [Actually, even this is not strictly true in the realm of
very high energies – what is strictly conserved is the total charge
and total ‘baryon number’ We need not pursue this matter here |
9 | 2999-3002 | However, the number of protons and the
number of neutrons are both separately conserved in a nuclear
reaction [Actually, even this is not strictly true in the realm of
very high energies – what is strictly conserved is the total charge
and total ‘baryon number’ We need not pursue this matter here ]
In nuclear reactions (e |
9 | 3000-3003 | [Actually, even this is not strictly true in the realm of
very high energies – what is strictly conserved is the total charge
and total ‘baryon number’ We need not pursue this matter here ]
In nuclear reactions (e g |
9 | 3001-3004 | We need not pursue this matter here ]
In nuclear reactions (e g , Eq |
9 | 3002-3005 | ]
In nuclear reactions (e g , Eq 13 |
9 | 3003-3006 | g , Eq 13 10), the number of protons and
the number of neutrons are the same on the two sides of the equation |
9 | 3004-3007 | , Eq 13 10), the number of protons and
the number of neutrons are the same on the two sides of the equation (b) We know that the binding energy of a nucleus gives a negative
contribution to the mass of the nucleus (mass defect) |
9 | 3005-3008 | 13 10), the number of protons and
the number of neutrons are the same on the two sides of the equation (b) We know that the binding energy of a nucleus gives a negative
contribution to the mass of the nucleus (mass defect) Now, since
proton number and neutron number are conserved in a nuclear
reaction, the total rest mass of neutrons and protons is the same
on either side of a reaction |
9 | 3006-3009 | 10), the number of protons and
the number of neutrons are the same on the two sides of the equation (b) We know that the binding energy of a nucleus gives a negative
contribution to the mass of the nucleus (mass defect) Now, since
proton number and neutron number are conserved in a nuclear
reaction, the total rest mass of neutrons and protons is the same
on either side of a reaction But the total binding energy of nuclei
on the left side need not be the same as that on the right hand
side |
9 | 3007-3010 | (b) We know that the binding energy of a nucleus gives a negative
contribution to the mass of the nucleus (mass defect) Now, since
proton number and neutron number are conserved in a nuclear
reaction, the total rest mass of neutrons and protons is the same
on either side of a reaction But the total binding energy of nuclei
on the left side need not be the same as that on the right hand
side The difference in these binding energies appears as energy
released or absorbed in a nuclear reaction |
9 | 3008-3011 | Now, since
proton number and neutron number are conserved in a nuclear
reaction, the total rest mass of neutrons and protons is the same
on either side of a reaction But the total binding energy of nuclei
on the left side need not be the same as that on the right hand
side The difference in these binding energies appears as energy
released or absorbed in a nuclear reaction Since binding energy
EXAMPLE 13 |
9 | 3009-3012 | But the total binding energy of nuclei
on the left side need not be the same as that on the right hand
side The difference in these binding energies appears as energy
released or absorbed in a nuclear reaction Since binding energy
EXAMPLE 13 4
Rationalised 2023-24
Physics
318
EXAMPLE 13 |
9 | 3010-3013 | The difference in these binding energies appears as energy
released or absorbed in a nuclear reaction Since binding energy
EXAMPLE 13 4
Rationalised 2023-24
Physics
318
EXAMPLE 13 4
contributes to mass, we say that the difference in the total mass
of nuclei on the two sides get converted into energy or vice-versa |
9 | 3011-3014 | Since binding energy
EXAMPLE 13 4
Rationalised 2023-24
Physics
318
EXAMPLE 13 4
contributes to mass, we say that the difference in the total mass
of nuclei on the two sides get converted into energy or vice-versa It is in these sense that a nuclear reaction is an example of mass-
energy interconversion |
9 | 3012-3015 | 4
Rationalised 2023-24
Physics
318
EXAMPLE 13 4
contributes to mass, we say that the difference in the total mass
of nuclei on the two sides get converted into energy or vice-versa It is in these sense that a nuclear reaction is an example of mass-
energy interconversion (c) From the point of view of mass-energy interconversion, a chemical
reaction is similar to a nuclear reaction in principle |
9 | 3013-3016 | 4
contributes to mass, we say that the difference in the total mass
of nuclei on the two sides get converted into energy or vice-versa It is in these sense that a nuclear reaction is an example of mass-
energy interconversion (c) From the point of view of mass-energy interconversion, a chemical
reaction is similar to a nuclear reaction in principle The energy
released or absorbed in a chemical reaction can be traced to the
difference in chemical (not nuclear) binding energies of atoms
and molecules on the two sides of a reaction |
9 | 3014-3017 | It is in these sense that a nuclear reaction is an example of mass-
energy interconversion (c) From the point of view of mass-energy interconversion, a chemical
reaction is similar to a nuclear reaction in principle The energy
released or absorbed in a chemical reaction can be traced to the
difference in chemical (not nuclear) binding energies of atoms
and molecules on the two sides of a reaction Since, strictly
speaking, chemical binding energy also gives a negative
contribution (mass defect) to the total mass of an atom or molecule,
we can equally well say that the difference in the total mass of
atoms or molecules, on the two sides of the chemical reaction
gets converted into energy or vice-versa |
9 | 3015-3018 | (c) From the point of view of mass-energy interconversion, a chemical
reaction is similar to a nuclear reaction in principle The energy
released or absorbed in a chemical reaction can be traced to the
difference in chemical (not nuclear) binding energies of atoms
and molecules on the two sides of a reaction Since, strictly
speaking, chemical binding energy also gives a negative
contribution (mass defect) to the total mass of an atom or molecule,
we can equally well say that the difference in the total mass of
atoms or molecules, on the two sides of the chemical reaction
gets converted into energy or vice-versa However, the mass
defects involved in a chemical reaction are almost a million times
smaller than those in a nuclear reaction |
9 | 3016-3019 | The energy
released or absorbed in a chemical reaction can be traced to the
difference in chemical (not nuclear) binding energies of atoms
and molecules on the two sides of a reaction Since, strictly
speaking, chemical binding energy also gives a negative
contribution (mass defect) to the total mass of an atom or molecule,
we can equally well say that the difference in the total mass of
atoms or molecules, on the two sides of the chemical reaction
gets converted into energy or vice-versa However, the mass
defects involved in a chemical reaction are almost a million times
smaller than those in a nuclear reaction This is the reason for
the general impression, (which is incorrect) that mass-energy
interconversion does not take place in a chemical reaction |
9 | 3017-3020 | Since, strictly
speaking, chemical binding energy also gives a negative
contribution (mass defect) to the total mass of an atom or molecule,
we can equally well say that the difference in the total mass of
atoms or molecules, on the two sides of the chemical reaction
gets converted into energy or vice-versa However, the mass
defects involved in a chemical reaction are almost a million times
smaller than those in a nuclear reaction This is the reason for
the general impression, (which is incorrect) that mass-energy
interconversion does not take place in a chemical reaction SUMMARY
1 |
9 | 3018-3021 | However, the mass
defects involved in a chemical reaction are almost a million times
smaller than those in a nuclear reaction This is the reason for
the general impression, (which is incorrect) that mass-energy
interconversion does not take place in a chemical reaction SUMMARY
1 An atom has a nucleus |
9 | 3019-3022 | This is the reason for
the general impression, (which is incorrect) that mass-energy
interconversion does not take place in a chemical reaction SUMMARY
1 An atom has a nucleus The nucleus is positively charged |
9 | 3020-3023 | SUMMARY
1 An atom has a nucleus The nucleus is positively charged The radius
of the nucleus is smaller than the radius of an atom by a factor of
104 |
9 | 3021-3024 | An atom has a nucleus The nucleus is positively charged The radius
of the nucleus is smaller than the radius of an atom by a factor of
104 More than 99 |
9 | 3022-3025 | The nucleus is positively charged The radius
of the nucleus is smaller than the radius of an atom by a factor of
104 More than 99 9% mass of the atom is concentrated in the nucleus |
9 | 3023-3026 | The radius
of the nucleus is smaller than the radius of an atom by a factor of
104 More than 99 9% mass of the atom is concentrated in the nucleus 2 |
9 | 3024-3027 | More than 99 9% mass of the atom is concentrated in the nucleus 2 On the atomic scale, mass is measured in atomic mass units (u) |
9 | 3025-3028 | 9% mass of the atom is concentrated in the nucleus 2 On the atomic scale, mass is measured in atomic mass units (u) By
definition, 1 atomic mass unit (1u) is 1/12th mass of one atom of 12C;
1u = 1 |
9 | 3026-3029 | 2 On the atomic scale, mass is measured in atomic mass units (u) By
definition, 1 atomic mass unit (1u) is 1/12th mass of one atom of 12C;
1u = 1 660563 × 10–27 kg |
9 | 3027-3030 | On the atomic scale, mass is measured in atomic mass units (u) By
definition, 1 atomic mass unit (1u) is 1/12th mass of one atom of 12C;
1u = 1 660563 × 10–27 kg 3 |
9 | 3028-3031 | By
definition, 1 atomic mass unit (1u) is 1/12th mass of one atom of 12C;
1u = 1 660563 × 10–27 kg 3 A nucleus contains a neutral particle called neutron |
9 | 3029-3032 | 660563 × 10–27 kg 3 A nucleus contains a neutral particle called neutron Its mass is almost
the same as that of proton
4 |
9 | 3030-3033 | 3 A nucleus contains a neutral particle called neutron Its mass is almost
the same as that of proton
4 The atomic number Z is the number of protons in the atomic nucleus
of an element |
9 | 3031-3034 | A nucleus contains a neutral particle called neutron Its mass is almost
the same as that of proton
4 The atomic number Z is the number of protons in the atomic nucleus
of an element The mass number A is the total number of protons and
neutrons in the atomic nucleus; A = Z+N; Here N denotes the number
of neutrons in the nucleus |
9 | 3032-3035 | Its mass is almost
the same as that of proton
4 The atomic number Z is the number of protons in the atomic nucleus
of an element The mass number A is the total number of protons and
neutrons in the atomic nucleus; A = Z+N; Here N denotes the number
of neutrons in the nucleus A nuclear species or a nuclide is represented as
ZAX
, where X is the
chemical symbol of the species |
9 | 3033-3036 | The atomic number Z is the number of protons in the atomic nucleus
of an element The mass number A is the total number of protons and
neutrons in the atomic nucleus; A = Z+N; Here N denotes the number
of neutrons in the nucleus A nuclear species or a nuclide is represented as
ZAX
, where X is the
chemical symbol of the species Nuclides with the same atomic number Z, but different neutron number
N are called isotopes |
9 | 3034-3037 | The mass number A is the total number of protons and
neutrons in the atomic nucleus; A = Z+N; Here N denotes the number
of neutrons in the nucleus A nuclear species or a nuclide is represented as
ZAX
, where X is the
chemical symbol of the species Nuclides with the same atomic number Z, but different neutron number
N are called isotopes Nuclides with the same A are isobars and those
with the same N are isotones |
9 | 3035-3038 | A nuclear species or a nuclide is represented as
ZAX
, where X is the
chemical symbol of the species Nuclides with the same atomic number Z, but different neutron number
N are called isotopes Nuclides with the same A are isobars and those
with the same N are isotones Most elements are mixtures of two or more isotopes |
9 | 3036-3039 | Nuclides with the same atomic number Z, but different neutron number
N are called isotopes Nuclides with the same A are isobars and those
with the same N are isotones Most elements are mixtures of two or more isotopes 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 |
9 | 3037-3040 | Nuclides with the same A are isobars and those
with the same N are isotones Most elements are mixtures of two or more isotopes 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 |
9 | 3038-3041 | Most elements are mixtures of two or more isotopes 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 |
Subsets and Splits