System of Particles and Rotational Motion Centre of Mass and Rotational Motion

because each of the objects displaced the water by 1 mL, their mass over that mL is their density.

The general and widespread acceptance of Sir Isaac Newton’s models and laws may often be taken for granted, but this has not always been so. Throughout history, scientists and philosophers have built on each other’s theories to create improved and often revolutionary models. Although Newton was neither the first nor the last to bring major innovations to society, he was one of the most notable ones; many of his contributions are still in use today. With the formulation of his laws of motion, Sir Isaac Newton contributed to the downfall of Aristotelianism and provided a universal quantitative system for approximating and explaining a wide range of phenomena of space and the physics of motion, revolutionizing the study and understanding

the planets fall around the Sun. Each of these objects balances the Sun 's force of gravity

6.2) If the mass of Body 2 was increased, then other bodies would be attracted to it and would change their orbits to come closer to Body 2. This would also affect the central star’s orbit because it is attracted to another mass of relatively large size. This occurs because there is a stronger gravitational pull because the object is now more massive and F_g= (Gm_1 m_2)/r^2

where max power could be produced. Then “critical instant”, where the ball is pushed with great

Document 2 2a) The sun stood in the center of the universe and different planets revolved around the

This will lead to an explanation of motion, the development of the calculus, and the establishment of basic laws of modern physics.

To begin the experiment, we measured the masses of the two stoppers and the eye bolt used to secure the stoppers that we were using in our apparatus. The mass of the first stopper was 18.8 grams and the mass of the second stopper was 50.5 grams. The mass of the eye bolt was 11.6 grams. The mass of the screw and bolt that secured our hanging mass was given to us as 25 grams. After, we chose six different hanging masses based on stopper mass. We made sure that the hanging mass was always larger than the stopper mass or else we would not be able to get the stopper to spin at a constant velocity. The first three mass ratios we chose was using the stopper with the mass of 18.8 grams and then we used a hanging mass (the mass of the screw and bolt is included) of 65 grams, 85 grams, and 105 grams. This gave the three mass

Introduction: The acceleration toward the center that keeps objects in uniform circular motion (circular motion at a constant speed) is called centripetal acceleration. An understanding of centripetal acceleration was one of the key elements that led to Newton’s formulation of the law of universal gravitation.

To investigate and observe how the acceleration of a mass depends on the resultant forces acting on it, along with its mass, and to furthermore define the relationship between acceleration, net force, and mass as a single equation.

It is easy to flip to the index of an astronomy textbook to discover that, say, the Sun lies 150 million kilometers away from Earth. It is far more difficult (if not impossible), however, to picture this distance in our mind. In this exercise, we will learn to access the often unpalatable distances encountered in astronomy by simply scaling the huge distances to more recognizable, familiar numbers. So long as every distance within the system of interest is scaled by the same

Mass of the Fulcrum Clamp: _________________(grams) Mass of Clamp with V-wire: ________________(grams) Mass of Weight Hanger: __________________(grams) Balancing point (center of mass) of meter stick, x0 = ____________(cm) Values Case 1 m1 = 100 g m2 = 200 g x1 = 15 cm x2 =_________ Moment (lever) arms r1 = ___________ r2 = ___________ Results *(see note above) τcc = ___________ τcw = ___________ % Diff. __________ Case 2 m1 = 100 g m2 = 200 g m3 = 50 g

Before Newton talked about gravitation the main knowledge of scientists was a elementary knowledge of optics, mechanics and astronomy.Copernicus Kepler and Galileo provided the background knowledge of the stars and planets, but Newton used their data to discover the whole gravitational system.10Newton reasoned that the planets and all other physical objects in the universe moved through mutual attraction of gravity.Newton said that every other object in the universe affected every other object through gravity.This explained why the planets move in an orderly fashion. Newton found that “the force of gravity towards the whole planet did arise from and was compounded of the forces of gravity towards all it’s parts, and towards every one part was in the inverse proportion of the squares of the distances from this part.”Newton proves all of this mathematically. This was known to be the single most important contribution to physics that ever has been made.11

The discovery of these laws, laid down a basic foundation for the physics of motion. Newton's three laws of gravity changed the way in which the world was perceived, because of their accuracy in describing many unexplained phenomenons.3 They explained what happens as a result of different variables, but most importantly, they explained why and how these actions happen. Like many of Isaac Newtons ideas and theories, the three laws of motion had a profound impact on the scientific community. The three laws of motions provided an explanation for almost everything in macro physics. Macro Physics is the branch of physics that deals with physical objects large enough to be observed and treated directly.4 This allowed for many new advancements in physics because the foundation had been build for others to develop upon. Isaac Newton published these findings in his revolutionary book “The Principa”. The Principa was revolutionary book because it organized the bulk of his life’s work, More importantly the

Johannes Kepler was a German astronomer and mathematician who lived between 1671-1630. Kepler was a Copernican and initially believed that planets should follow perfectly circular orbits (“Johan Kepler” 1). During this time period, Ptolemy’s geocentric theory of the solar system was accepted. Ptolemy’s theory stated that Earth is at the center of the universe and stationary; closest to Earth is the Moon, and beyond it, expanding towards the outside, are Mercury, Venus, and the Sun in a straight line, followed by Mars, Jupiter, Saturn, and the “fixed stars”. The Ptolemaic system explained the numerous observed motions of the planets as having small spherical orbits called epicycles (“Astronomy” 2). Kepler is best known for introducing three