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CBSE Class 11 Physics Chapter 7 Gravitation Worksheet with Answers

Q: What is the difference between mass and weight in gravitation?

Mass is the amount of matter in an object, measured in kilograms, and remains constant everywhere. Weight is the gravitational force acting on that mass, given by W = mg, measured in Newtons, and varies with the local value of g. For example, a 60 kg person weighs 600 N on Earth but only 100 N on the Moon because the Moon's g is about 1.6 m/s².

Q: How do I calculate gravitational force between two objects?

Use Newton's law of universal gravitation: F = G(m₁m₂)/r². Identify the two masses (m₁, m₂ in kg), the distance between their centers (r in meters), and the gravitational constant G = 6.67×10⁻¹¹ N·m²/kg². Substitute these values, calculate the numerator (product of masses), the denominator (r squared), divide, and multiply by G to get force in Newtons.

Q: Why does acceleration due to gravity g vary with altitude?

Acceleration due to gravity g = GM/r², where r is the distance from Earth's center. As altitude h increases, r = R+h also increases, so g decreases following the inverse-square law. For small heights, g_h ≈ g(1 - 2h/R). This means objects weigh slightly less at mountain tops than at sea level, and satellites in orbit experience reduced g.

Q: What is escape velocity and how is it derived?

Escape velocity is the minimum speed needed to leave a planet's gravitational field without further propulsion. It is derived using energy conservation: initial kinetic energy ½mvₑ² must equal the gravitational potential energy GMm/R at the surface. Setting total energy to zero at infinity gives vₑ = √(2GM/R). For Earth, vₑ ≈ 11.2 km/s, independent of the object's mass.

Q: How is Kepler's third law derived from Newton's gravitation?

For a planet in circular orbit, gravitational force provides centripetal force: GMm/r² = mv²/r, so v = √(GM/r). Orbital velocity v = 2πr/T (circumference/period). Equate: √(GM/r) = 2πr/T, square both sides and rearrange: T² = (4π²/GM)r³. Since 4π²/GM is constant for a given central mass, T² ∝ r³, which is Kepler's third law.

Q: Why are astronauts weightless in orbit if gravity still acts on them?

Astronauts in orbit are in continuous free fall toward Earth while moving forward at high speed, creating a curved path (orbit). Both the spacecraft and astronaut fall together at the same rate, so there is no normal force between them—this absence of normal force is experienced as weightlessness. Earth's gravity is still present and provides the centripetal force keeping them in orbit.

Q: What is the universal gravitational constant G and why is it important?

The universal gravitational constant G ≈ 6.67×10⁻¹¹ N·m²/kg² is a fundamental constant that quantifies the strength of gravitational attraction between masses. It appears in Newton's law F = G(m₁m₂)/r² and allows us to calculate gravitational forces and accelerations anywhere in the universe. G is extremely small, which is why gravitational forces between everyday objects are negligible.

Q: How does CBSETUTOR.ai help with Chapter 7 Gravitation numericals?

CBSETUTOR.ai offers a 24×7 AI tutor for Classes 6-12 at ₹999/month (all classes included) with a 3-day free trial. Students can upload photos of gravitation problems and receive step-by-step solutions with explanations, practice additional MCQs and numericals, clarify doubts instantly, and access topic-wise notes and solved examples—perfect for mastering derivations, numerical problems, and conceptual questions from NCERT Class 11 Physics Chapter 7.

Q: What are common mistakes to avoid in gravitation numerical problems?

Common mistakes include: (1) confusing mass (kg) with weight (N); (2) forgetting to square the distance in F = G(m₁m₂)/r²; (3) using surface-to-surface distance instead of center-to-center separation; (4) incorrect unit conversions (km to m, g to kg); (5) mixing up g (9.8 m/s²) and G (6.67×10⁻¹¹); (6) not stating assumptions (uniform sphere, no air resistance). Always write given data, formula, substitution, and final answer with units.

Q: How much time should I spend on this gravitation worksheet?

Allocate 90 minutes to complete the entire worksheet in exam-like conditions. Spend about 1 minute per MCQ (6 min), 1 min per fill-in-the-blank (5 min), 1 min per true/false (6 min), 6-8 min per short-answer question (30-40 min), 10-12 min per long-answer question (30-36 min), and 4 min for the case study (total ~87-93 min). Use any remaining time to review calculations and check units.

Gravitation is one of the four fundamental forces of nature and governs the motion of celestial bodies, satellites, and falling objects. This CBSE Class 11 Physics Chapter 7 worksheet provides a structured practice session aligned with NCERT syllabus, covering the universal law of gravitation, weight and mass distinctions, variation of g, planetary motion, and satellite dynamics. Each section progressively builds problem-solving skills—from conceptual MCQs to numerical HOTS questions—followed by a detailed answer key for self-correction.

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Key takeaways

✓Newton's law of universal gravitation states that every object attracts every other object with force F = G(m₁m₂)/r², where G ≈ 6.67×10⁻¹¹ N·m²/kg².
✓Weight (W = mg) is the gravitational force on an object and varies with location; mass remains constant everywhere.
✓Acceleration due to gravity (g ≈ 9.8 m/s² on Earth's surface) decreases with altitude and depth, following inverse-square law variations.
✓Free fall is motion under gravity alone; all objects fall at the same rate in a vacuum regardless of mass.
✓Kepler's three laws describe planetary motion: elliptical orbits, equal area in equal time, and T²∝r³.
✓Escape velocity (vₑ = √(2gR) ≈ 11.2 km/s for Earth) is the minimum speed needed to leave a planet's gravitational field without propulsion.
✓Orbital velocity for a satellite is v = √(GM/r); geostationary satellites orbit at ~36,000 km altitude with 24-hour period.

Quick Chapter Recap: Gravitation

Newton's law of universal gravitation is the foundation of this chapter: every mass attracts every other mass with a force proportional to the product of their masses and inversely proportional to the square of the distance between their centers. The universal gravitational constant G = 6.67×10⁻¹¹ N·m²/kg² appears in all gravitational force calculations. Weight is the gravitational force Earth exerts on an object (W = mg), measured in Newtons, while mass is an intrinsic property measured in kilograms and remains constant. Acceleration due to gravity g ≈ 9.8 m/s² on Earth's surface but varies with altitude and latitude. Free fall occurs when only gravity acts on an object; all objects accelerate equally in a vacuum. Kepler's laws describe planetary orbits: planets move in ellipses with the Sun at one focus, sweep equal areas in equal times, and their orbital period squared is proportional to the cube of the semi-major axis. Gravitational potential energy U = -GMm/r, and escape velocity vₑ = √(2GM/R) is the speed needed to break free from a planet's gravity. Satellites in circular orbits have velocity v = √(GM/r) and period T = 2π√(r³/GM). Geostationary satellites orbit at 36,000 km with 24-hour periods, appearing stationary above the equator.

Universal law: F = G(m₁m₂)/r² with G = 6.67×10⁻¹¹ N·m²/kg²
Weight W = mg varies with location; mass m is constant
g ≈ 9.8 m/s² on Earth; decreases with height and depth
Kepler's third law: T² ∝ r³ for planetary orbits
Escape velocity for Earth: vₑ ≈ 11.2 km/s
Orbital velocity: v = √(GM/r); geostationary orbit at ~36,000 km

Section A: Multiple Choice Questions (MCQs)

This section tests conceptual clarity and quick recall of formulae. Each MCQ has one correct answer. Choose the best option and mark it clearly. These questions reflect typical CBSE board exam patterns and cover the universal law of gravitation, differences between mass and weight, variation of g, satellite motion, and Kepler's laws. Pay attention to units: gravitational force is in Newtons, mass in kilograms, and distance in meters. Remember that gravitational force obeys the inverse-square law, so doubling the distance reduces force to one-fourth. Weight changes with location (Earth, Moon, or altitude), but mass does not. Escape velocity depends only on the planet's mass and radius, not on the object's mass.

Q1. The universal gravitational constant G has units: (a) N·m²/kg (b) N·m²/kg² (c) N/kg² (d) m/s²
Q2. If the distance between two objects is doubled, the gravitational force becomes: (a) half (b) one-fourth (c) double (d) four times
Q3. A body weighs 600 N on Earth. Its approximate weight on the Moon (g_Moon ≈ 1.6 m/s²) is: (a) 100 N (b) 60 N (c) 600 N (d) 300 N
Q4. Acceleration due to gravity at height h above Earth's surface (h << R) is: (a) g(1 + 2h/R) (b) g(1 - 2h/R) (c) g(1 + h/R) (d) g(1 - h/R)
Q5. Escape velocity from Earth is approximately: (a) 7.9 km/s (b) 11.2 km/s (c) 15 km/s (d) 9.8 m/s
Q6. According to Kepler's third law, if orbital radius is doubled, the period becomes: (a) 2 times (b) 4 times (c) 2√2 times (d) 8 times

Section B: Fill in the Blanks

Complete each statement with the correct term, formula, or numerical value. These questions reinforce terminology and key relationships from NCERT Class 11 Physics Chapter 7. Write answers in the spaces provided. Remember that weight is a force (measured in Newtons), while mass is measured in kilograms. The value of G is a universal constant that applies to all gravitational interactions, from apples falling to galaxies attracting each other. Free fall means acceleration is g downward, with no air resistance or other forces. Geostationary satellites remain fixed above one point on the equator because their orbital period matches Earth's rotation period of 24 hours. Gravitational potential energy is negative because the reference point (U = 0) is taken at infinite separation.

Q7. The force of attraction between any two masses is called ________.
Q8. Weight of a body is given by the formula W = ________.
Q9. The value of acceleration due to gravity on Earth's surface is approximately ________ m/s².
Q10. The universal gravitational constant G is approximately ________ N·m²/kg².
Q11. A geostationary satellite has an orbital period of ________ hours.
Q12. Escape velocity from a planet is independent of the ________ of the object.

Section C: True or False Statements

Determine whether each statement is true or false. Write 'T' for true and 'F' for false. Justify your answer in one sentence where indicated. This section checks common misconceptions and precise understanding of gravitation concepts. Many students confuse mass with weight, or think gravity vanishes in orbit (it does not—astronauts are in continuous free fall). Gravitational force acts between all masses, no matter how small, but is only noticeable when at least one mass is very large like Earth. The inverse-square law means that gravitational force decreases rapidly with distance, becoming negligible at astronomical separations for everyday objects. Satellites in lower orbits move faster than those in higher orbits because orbital velocity v = √(GM/r) decreases with increasing r. Remember that Kepler's laws apply to any central force following inverse-square law, not just the Sun-planet system—they work for moons orbiting planets too.

Q13. Mass and weight are the same physical quantity. (True / False)
Q14. The value of g is the same at all points on Earth's surface. (True / False)
Q15. Gravitational force between two objects becomes zero when they are far apart. (True / False)
Q16. A satellite in orbit around Earth is in a state of continuous free fall. (True / False)
Q17. Escape velocity depends on the mass of the object trying to escape. (True / False)
Q18. The orbital speed of a satellite increases as its altitude increases. (True / False)

Section D: Short Answer Questions (3 Marks Each)

Answer each question in 50-80 words or show the necessary calculation steps. These questions are typical 3-mark CBSE board questions requiring conceptual explanation, derivation sketches, or numerical problem-solving. For numerical questions, always write the given data, formula, substitution, and final answer with units. When asked to state a law, give both the statement and the mathematical form. Explain differences clearly: mass is intrinsic and constant; weight is gravitational force and varies. Show that g varies inversely with the square of distance from Earth's center. For orbital velocity, derive or state v = √(GM/r) and explain that it decreases with altitude. Remember that gravitational potential energy is always negative for bound systems and zero at infinity. In problems involving gravitational force, ensure you use the distance between centers of mass, not surface-to-surface separation unless explicitly stated.

Q19. State Newton's law of universal gravitation and write its mathematical form. Define each symbol.
Q20. Distinguish between mass and weight. Why does weight vary from place to place while mass remains constant?
Q21. Derive the relation between gravitational acceleration g and universal gravitational constant G for an object on Earth's surface.
Q22. Calculate the gravitational force between two masses of 40 kg and 60 kg separated by 0.5 m. (G = 6.67×10⁻¹¹ N·m²/kg²)
Q23. Explain why astronauts in the International Space Station experience weightlessness even though Earth's gravity acts on them.

Section E: Long Answer and HOTS Questions (5 Marks Each)

These questions demand deeper conceptual reasoning, multi-step derivations, or application of multiple concepts. Allocate 10-12 minutes per question. For derivations, start from fundamental principles (Newton's laws, energy conservation, or Kepler's laws) and show every algebraic step clearly. For numerical problems, draw diagrams where helpful, list all given data, choose the correct formula, substitute carefully, and state the final answer with proper units and significant figures. HOTS (Higher Order Thinking Skills) questions may ask you to apply gravitation concepts to unfamiliar scenarios—such as comparing gravitational fields on different planets, analyzing satellite orbits, or calculating escape velocities. When deriving Kepler's third law from Newton's gravitation, equate centripetal force to gravitational force and express period T in terms of orbital radius r. For escape velocity derivation, use energy conservation: kinetic energy at surface equals gravitational potential energy change from surface to infinity. Clearly state assumptions (uniform spherical mass distribution, no air resistance, etc.) where relevant.

Q24. Derive an expression for escape velocity from the surface of a planet of mass M and radius R. Calculate escape velocity for Earth (M = 6×10²⁴ kg, R = 6.4×10⁶ m, G = 6.67×10⁻¹¹ N·m²/kg²).
Q25. State Kepler's three laws of planetary motion. Using Newton's law of gravitation, derive Kepler's third law (T² ∝ r³) for a planet in circular orbit around the Sun.
Q26. The acceleration due to gravity at height h above Earth's surface is 4.9 m/s². If Earth's radius is 6400 km and g at surface is 9.8 m/s², find the height h. Also explain why g decreases with altitude.

Section F: Case-Study Based Question

Read the passage carefully and answer the sub-questions. This format mirrors the CBSE board exam case-study pattern introduced in recent years. The passage provides real-world context—such as satellite launches, planetary exploration, or gravitational effects on Earth—and tests your ability to apply Chapter 7 concepts to interpret data, make calculations, and draw conclusions. Each sub-question is worth 1 mark. Show working for numerical parts. Pay attention to units given in the passage and convert if necessary. Use g = 10 m/s² unless specified otherwise. The passage integrates multiple topics: orbital mechanics, gravitational force, energy, and Kepler's laws, so revise these thoroughly before attempting this section.

Complete Answer Key with Explanations

Below are the answers to all questions in this worksheet, with brief explanations to aid understanding. Use this key for self-assessment after attempting the worksheet honestly. For MCQs and fill-in-the-blanks, only the correct answer is given. For short and long questions, model answers or solution outlines are provided—your answer may be worded differently but should contain the same key points and correct numerical results. Cross-check your steps, formula usage, and units carefully. If you scored below 70 percent, revisit the NCERT Class 11 Physics Chapter 7 text and solved examples, then re-attempt the worksheet. For personalized doubt-clearing and step-by-step solutions with photo uploads, CBSETUTOR.ai offers a 24×7 AI tutor for Classes 6-12 at a flat ₹999/month with a 3-day free trial—ideal for mastering gravitation numericals and conceptual questions at your own pace.

A1. (b) N·m²/kg² — The unit of G follows from F = G(m₁m₂)/r², rearranging gives G = Fr²/(m₁m₂).
A2. (b) one-fourth — Gravitational force F ∝ 1/r²; doubling r makes F become F/4.
A3. (a) 100 N — W_Earth = 600 N, so m = 600/10 = 60 kg. W_Moon = 60×1.6 ≈ 96 N ≈ 100 N.
A4. (b) g(1 - 2h/R) — For small h, g_h ≈ g(1 - 2h/R) from binomial approximation of (R/(R+h))².
A5. (b) 11.2 km/s — Escape velocity for Earth is vₑ = √(2gR) ≈ 11.2 km/s.
A6. (c) 2√2 times — T² ∝ r³, so if r → 2r, then T² → 8T², hence T → √8 T = 2√2 T.
A7. gravitation (or gravitational force)
A8. mg (where m = mass, g = acceleration due to gravity)
A9. 9.8 (accept 10)
A10. 6.67×10⁻¹¹
A11. 24
A12. mass
A13. False — Mass is the amount of matter (kg); weight is gravitational force (N). They have different units and meanings.
A14. False — g varies slightly with latitude (lower at equator) and altitude (decreases with height).
A15. False — Gravitational force becomes very small but never exactly zero; it decreases as 1/r² and approaches zero only at infinite separation.
A16. True — Satellite and Earth attract each other; satellite continuously falls toward Earth but also moves forward, resulting in circular orbit (free fall).
A17. False — Escape velocity vₑ = √(2GM/R) depends only on planet's mass M and radius R, not on the escaping object's mass.
A18. False — Orbital speed v = √(GM/r); as altitude (r) increases, v decreases.
A19. Newton's law of universal gravitation: Every particle attracts every other particle with a force proportional to the product of their masses and inversely proportional to the square of the distance between them. F = G(m₁m₂)/r², where F = force, G = gravitational constant, m₁, m₂ = masses, r = separation.
A20. Mass is the quantity of matter in a body, measured in kg, and is constant everywhere. Weight is the gravitational force on the body, W = mg, measured in Newtons, and varies with g. Since g differs on Earth, Moon, or at altitude, weight changes but mass does not.
A21. (See example above.) On Earth's surface: F = GMm/R² and F = mg, so mg = GMm/R² → g = GM/R².
A22. Given: m₁=40 kg, m₂=60 kg, r=0.5 m, G=6.67×10⁻¹¹. F = G(m₁m₂)/r² = 6.67×10⁻¹¹×(40×60)/(0.5)² = 6.67×10⁻¹¹×2400/0.25 = 6.67×10⁻¹¹×9600 = 6.4×10⁻⁷ N.
A23. Astronauts in ISS are in continuous free fall toward Earth while moving tangentially at high speed, so they orbit Earth. Both astronaut and station fall together, eliminating normal force—hence they feel weightless. Earth's gravity still acts; it provides the centripetal force for orbit.
A24. (See example above.) Derivation: Energy at surface = ½mvₑ² - GMm/R; at infinity = 0. Equate: vₑ = √(2GM/R). For Earth: vₑ = √(2×6.67×10⁻¹¹×6×10²⁴/6.4×10⁶) ≈ 11.2 km/s.
A25. Kepler's laws: (i) Planets move in ellipses with Sun at one focus. (ii) A line joining planet and Sun sweeps equal areas in equal times. (iii) T² ∝ r³. Derivation of (iii): For circular orbit, gravitational force = centripetal force: GMm/r² = mv²/r, so v = √(GM/r). Period T = 2πr/v = 2πr/√(GM/r) = 2π√(r³/GM), hence T² = (4π²/GM)r³ → T² ∝ r³.
A26. Given: g_h = 4.9 m/s², g = 9.8 m/s², R = 6400 km. g_h/g = R²/(R+h)² → 4.9/9.8 = 1/2 = [R/(R+h)]². Take square root: R/(R+h) = 1/√2, so R+h = R√2, h = R(√2 - 1) = 6400×0.414 ≈ 2650 km. g decreases with altitude because gravitational force F = GMm/r² falls as r increases.
A27(a). Orbital radius r = Earth's radius + altitude = 6400 + 36000 = 42400 km = 4.24×10⁷ m.
A27(b). v = √(gR²/r) = √(10×(6.4×10⁶)²/(4.24×10⁷)) = √(10×4.096×10¹³/4.24×10⁷) = √(9.66×10⁶) ≈ 3108 m/s ≈ 3.1 km/s.
A27(c). The satellite's orbital period is 24 hours, matching Earth's rotation period, so it remains above the same point on the equator—appearing stationary to an observer on Earth.
A27(d). T² ∝ r³. If altitude doubles, new r' ≈ 2r (approximately, ignoring Earth radius for simplicity of proportionality). Then T'² ∝ (2r)³ = 8r³, so T'² = 8T² → T' = 2√2 T ≈ 2.83 T. Period increases by factor 2√2.

How to Use This Worksheet Effectively

Set a timer for 90 minutes and attempt the worksheet in exam-like conditions—no textbook, no phone, just a pen and calculator. Start with Section A to build confidence, then move through Sections B, C, and D before tackling the longer Section E and case study. Write neatly and show all working for numerical questions; CBSE awards partial marks for correct method even if the final answer is wrong. After completing, use the answer key to mark your work honestly—give yourself 1 mark per MCQ/fill-blank/true-false, 3 marks per short question, and 5 marks per long question. A score above 75 percent indicates good preparation; 50-75 percent means you need focused revision of weak areas; below 50 percent suggests revisiting NCERT chapter text and solved examples thoroughly. For topics where you struggled, make brief notes summarizing formulae, definitions, and common mistakes. Reattempt incorrect questions after 2-3 days to check retention. Practicing multiple worksheets builds speed and accuracy—essential for board exams. If you need instant doubt resolution or step-by-step guidance on tricky numericals, CBSETUTOR.ai provides 24×7 AI-powered tutoring with photo-upload problem solving for all CBSE classes 6-12 at just ₹999/month, with a 3-day free trial to explore the platform.

Time limit: 90 minutes; attempt in one sitting for realistic exam practice
Show all steps in numerical problems to earn partial marks even if final answer is incorrect
Use the answer key immediately after completion to identify knowledge gaps
Score interpretation: >75% excellent, 50-75% good (needs focused revision), <50% revisit NCERT text
Reattempt weak questions after revision to reinforce learning and improve retention

Frequently asked questions

What is the difference between mass and weight in gravitation?+

Mass is the amount of matter in an object, measured in kilograms, and remains constant everywhere. Weight is the gravitational force acting on that mass, given by W = mg, measured in Newtons, and varies with the local value of g. For example, a 60 kg person weighs 600 N on Earth but only 100 N on the Moon because the Moon's g is about 1.6 m/s².

How do I calculate gravitational force between two objects?+

Use Newton's law of universal gravitation: F = G(m₁m₂)/r². Identify the two masses (m₁, m₂ in kg), the distance between their centers (r in meters), and the gravitational constant G = 6.67×10⁻¹¹ N·m²/kg². Substitute these values, calculate the numerator (product of masses), the denominator (r squared), divide, and multiply by G to get force in Newtons.

Why does acceleration due to gravity g vary with altitude?+

Acceleration due to gravity g = GM/r², where r is the distance from Earth's center. As altitude h increases, r = R+h also increases, so g decreases following the inverse-square law. For small heights, g_h ≈ g(1 - 2h/R). This means objects weigh slightly less at mountain tops than at sea level, and satellites in orbit experience reduced g.

What is escape velocity and how is it derived?+

Escape velocity is the minimum speed needed to leave a planet's gravitational field without further propulsion. It is derived using energy conservation: initial kinetic energy ½mvₑ² must equal the gravitational potential energy GMm/R at the surface. Setting total energy to zero at infinity gives vₑ = √(2GM/R). For Earth, vₑ ≈ 11.2 km/s, independent of the object's mass.

How is Kepler's third law derived from Newton's gravitation?+

For a planet in circular orbit, gravitational force provides centripetal force: GMm/r² = mv²/r, so v = √(GM/r). Orbital velocity v = 2πr/T (circumference/period). Equate: √(GM/r) = 2πr/T, square both sides and rearrange: T² = (4π²/GM)r³. Since 4π²/GM is constant for a given central mass, T² ∝ r³, which is Kepler's third law.

Why are astronauts weightless in orbit if gravity still acts on them?+

Astronauts in orbit are in continuous free fall toward Earth while moving forward at high speed, creating a curved path (orbit). Both the spacecraft and astronaut fall together at the same rate, so there is no normal force between them—this absence of normal force is experienced as weightlessness. Earth's gravity is still present and provides the centripetal force keeping them in orbit.

What is the universal gravitational constant G and why is it important?+

The universal gravitational constant G ≈ 6.67×10⁻¹¹ N·m²/kg² is a fundamental constant that quantifies the strength of gravitational attraction between masses. It appears in Newton's law F = G(m₁m₂)/r² and allows us to calculate gravitational forces and accelerations anywhere in the universe. G is extremely small, which is why gravitational forces between everyday objects are negligible.

How does CBSETUTOR.ai help with Chapter 7 Gravitation numericals?+

CBSETUTOR.ai offers a 24×7 AI tutor for Classes 6-12 at ₹999/month (all classes included) with a 3-day free trial. Students can upload photos of gravitation problems and receive step-by-step solutions with explanations, practice additional MCQs and numericals, clarify doubts instantly, and access topic-wise notes and solved examples—perfect for mastering derivations, numerical problems, and conceptual questions from NCERT Class 11 Physics Chapter 7.

What are common mistakes to avoid in gravitation numerical problems?+

Common mistakes include: (1) confusing mass (kg) with weight (N); (2) forgetting to square the distance in F = G(m₁m₂)/r²; (3) using surface-to-surface distance instead of center-to-center separation; (4) incorrect unit conversions (km to m, g to kg); (5) mixing up g (9.8 m/s²) and G (6.67×10⁻¹¹); (6) not stating assumptions (uniform sphere, no air resistance). Always write given data, formula, substitution, and final answer with units.

How much time should I spend on this gravitation worksheet?+

Allocate 90 minutes to complete the entire worksheet in exam-like conditions. Spend about 1 minute per MCQ (6 min), 1 min per fill-in-the-blank (5 min), 1 min per true/false (6 min), 6-8 min per short-answer question (30-40 min), 10-12 min per long-answer question (30-36 min), and 4 min for the case study (total ~87-93 min). Use any remaining time to review calculations and check units.

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