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### Gravitation 1

• 1.
• 2.
• 3. • The motion of stars, the Moon, and the planets are always wonderful. • From Aristotle to Stephen Hawking, great minds have tried to understand the movement of celestial objects in space and what causes their motion. • The ‘Theory of Gravitation’ was developed by Newton in the late 17th century to explain the motion of celestial objects and terrestrial objects
• 4.
• 5. • In 2017, the Nobel Prize in Physics was given for the detection of ‘Gravitational waves’ which was theoretically predicted by Albert Einstein in the year 1915.
• 6.
• 7. • Understanding planetary motion, the formation of stars and galaxies, and recently massive objects like black holes and their life cycle have remained the focus of study for the past few centuries in physics.
• 8. Geocentric Model of Solar System In the second century, Claudius Ptolemy, a famous Greco-Roman astronomer developed a theory to explain the motion of celestial objects like the Sun, the Moon, Mars, Jupiter etc. This theory was called the geocentric model.
• 9. • According to the geocentric model, the Earth is at the center of the universe and all celestial objects including the Sun, the Moon, and other planets orbit the Earth.
• 10.
• 11. • Ptolemy’s model closely matched with the observations of the sky with our naked eye. • But later, astronomers found that even though Ptolemy’s model successfully explained the motion of the Sun and the Moon up to a certain level, the motion of Mars and Jupiter could not be explained effectively
• 12. Heliocentric Model of Nicholas Copernicus In the 15th century, a Polish astronomer, Nicholas Copernicus (1473-1543) proposed a new model called the ‘Heliocentric model’
• 13. • Sun was considered to be at the center of the solar system and all planets including the Earth orbited the Sun in circular orbits. • .
• 14. Galileo, a famous Italian physicist discovered that all objects close to Earth were accelerated toward the Earth at the same rate.
• 15. Tycho Brahe (1546-1601) spent his entire lifetime in recording the observations of the stellar and planetary positions with his naked eye.
• 16. The data that Tycho Brahe compiled were analyzed later by his assistant Johannes Kepler (1571–1630) and eventually the analysis led to the deduction of the laws of the planetary motion.
• 17.
• 18.
• 19. Kepler’s Laws of Planetary Motion
• 20. • The closest point of approach of the planet to the Sun ‘P’ is called perihelion and the farthest point ‘A’ is called aphelion • The semi-major axis is ‘a’ and semi-minor axis is ‘b’. • In fact, both Copernicus and Ptolemy considered planetary orbits to be circular, but Kepler discovered that the actual orbits of the planets are elliptical.
• 21.
• 22.
• 23. • The white shaded portion is the area DA swept in a small interval of time Dt, by a planet around the Sun. • Since the Sun is not at the center of the ellipse, the planets travel faster when they are nearer to the Sun and slower when they are farther from it, to cover equal area in equal intervals of time. • Kepler discovered the law of area by carefully noting the variation in the speed of planets
• 24.
• 25. The time period of revolution of the planets revolving around the Sun and their semi-major axes.
• 26. Law of Gravitation Universal Law of Gravitation
• 27.
• 28.
• 29.
• 30.
• 31.
• 32.
• 33.
• 34.
• 35.
• 36.
• 37.
• 38.
• 39.
• 40.
• 41.
• 42.
• 44.
• 45.
• 46.
• 47. • To calculate force of attraction between a hollow sphere of mass M with uniform density and point mass m kept outside the hollow sphere, we can replace the hollow sphere of mass M as equivalent to a point mass M located at the center of the hollow sphere. • The force of attraction between the hollow sphere of mass M and point mass m can be calculated by treating the hollow sphere also as another point mass. • Essentially the entire mass of the hollow sphere appears to be concentrated at the center of the hollow sphere
• 48.
• 49. • consider a hollow sphere of mass M. If we place another object of mass ‘m’ inside this hollow sphere , the force experienced by this mass ‘m’ will be zero.
• 50. • The triumph of the law of gravitation is that it concludes that the mango that is falling down and the Moon orbiting the Earth are due to the same gravitational force.
• 52. Newton’s inverse square Law • Newton considered the orbits of the planets as circular. For circular orbit of radius r, the centripetal acceleration towards the center is • Here v is the velocity and r, the distance of the planet from the center of the orbit
• 53. Point mass orbiting in a circular orbit.
• 54. • The velocity in terms of known quantities r and T, is • Here T is the time period of revolution of the planet.
• 55. • Substituting the value of ‘a’ in Newton’s second law, , where ‘m’ is the mass of the planet. • From Kepler’s third law,
• 56. • we can arrive at the law of gravitation. • Here negative sign implies that the force is attractive and it acts towards the center
• 57. • But Newton strongly felt that according to his third law, if Earth is attracted by the Sun, then the Sun must also be attracted by the Earth with the same magnitude of force. So he felt that the Sun’s mass (M) should also occur explicitly in the expression for force • From this insight, he equated the constant which turned out to be the law of gravitation • Again the negative sign in the above equation implies that the gravitational force is attractive.
• 58. • we assumed that the orbit of the planet to be circular which is not true as the orbit of the planet around the Sun is elliptical. • But this circular orbit assumption is justifiable because planet’s orbit is very close to being circular and there is only a very small deviation from the circular shape.
• 59.
• 60.
• 61.
• 62.
• 63.
• 64. • Th e above calculation depends on knowing the distance between the Earth and the Moon and the radius of the Earth. • Th e radius of the Earth was measured by Greek librarian Eratosthenes and distance between the Earth and the Moon was measured by Greek astronomer Hipparchrus 2400 years ago. • It is very interesting to note that in order to measure these distances he used only high school geometry and trigonometry.
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