Name: newton’s law behind planet motion
Uploaded: 2023-05-16T08:18:41.000Z
Duration: 1 min 16 s
Channel: JoVE

K12 Standards

north-carolina-k-12-science-standard-course-of-study

North Carolina K-12 Science Standard Course of Study

9-12

Physics

motion-and-stability-forces-and-interactions

Motion and Stability- Forces and Interactions

PS.Phy.2.4

Gravitation

يشير دوران القمر حول الأرض إلى وجود قوة تجذبه نحو مركز المدار.
اقترح إسحاق نيوتن أن هذه القوة الجذابة هي نفسها التي تسحب تفاحة نحو الأرض.
لقد كانت فكرة ثورية ، حيث كان يعتقد أن الأجرام السماوية والأجسام الموجودة على الأرض تتبع قواعد مختلفة.
يستغرق القمر 27.3 يوما للدوران حول الأرض. بالنظر إلى متوسط المسافة إلى القمر ، يمكن تقدير تسارعه. 
تشير نسبة التسارع القمري إلى تسارع الجسم الساقط على الأرض إلى أن التسارع يتناسب عكسيا مع المسافة المربعة.
نظرا لأن القوة هي الكتلة مضروبة في التسارع ، فإن قوة الجاذبية تتناسب طرديا مع الكتلة وتتناسب عكسيا مع المسافة المربعة.
لاحظ نيوتن أن تسارع الكواكب يتناقص عكسيا مع بعدها عن الشمس ، وتوقع أن قوة الجاذبية تعمل بين الشمس والكواكب وأقمارها.
بتوسيع هذه الحجة لتشمل جميع الأجسام في الكون ، صاغ نيوتن قانون الجاذبية الكونية.

<ol>
	<li>فيرما ، إتش سي (2008). مفاهيم الفيزياء. المجلد 1 ، Bharati Bhawan Pub. & Dis.: القسمان 11.1 و 11.2 ؛ الصفحات 203-204.</li>
</ol>

الجاذبية

<div style="direction:rtl">في السنوات التي سبقت نيوتن، ساد اعتقاد عام بأن القوانين التي تحكم الأجسام الموجودة في السماء تختلف عن تلك الموجودة على الأرض. عندما كتب كيبلر القوانين الثلاثة لحركة الكواكب، موضحًا بالتفصيل الخصائص الهندسية لمدارات الكواكب حول الشمس، لم تكن هناك فكرة فورية لتمييز ارتباطها بقوانين أكثر أساسية. كان إسحاق نيوتن هو الذي اكتشف في عامي 1665 و1666 العلاقة بين حركة الكواكب وحركة القمر حول الأرض والظاهرة اليومية لسقوط الأجسام على سطح الأرض. تُعرف هذه الظاهرة العالمية اليوم بالجاذبية. على الرغم من أن الأمر يبدو شائعًا اليوم، إلا أن القول بأن الظاهرة نفسها تحكم حركة الأجسام على الأرض وحركة القمر حول الأرض كان ثوريًا في زمن نيوتن. لقد اكتشف أن تسارع القمر الجاذب المركزي حول الأرض وتسارع الجاذبية لهما نسبة تتناسب عكسيًا مع مربع بعد الجسم المعني عن الأرض. وبما أن التسارع لا يعتمد على الكتلة، فإنه وفقًا لقوانين الحركة، يجب أن تكون القوة متناسبة مع الكتلة. وقد قادته هذه الرؤية إلى صياغة قانون الجاذبية الذي سمي باسمه. هناك معلومة أخرى مطلوبة لإكمال قانون نيوتن للجاذبية وهو ثابت الجاذبية، والذي تم استخلاصه تجريبيًا. أول تجربة ناجحة لقياس الثابت أجراها هنري كافنديش. وبمجرد معرفة قيمة هذا الثابت، بالإضافة إلى قوانين نيوتن للحركة، أصبح من الممكن استخلاص قوانين كبلر لحركة الكواكب.</div>

في السنوات التي سبقت نيوتن ، ساد اعتقاد عام بأن قوانين مختلفة تحكم الأجسام في السماء عن الأجسام الموجودة على الأرض. عندما كتب كبلر ...

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Education

JoVE Core

الفيزياء

Unit 1

الوحدة الأولى

KEY TERMS AND CONCEPTS

المصطلحات والمفاهيم الأساسية

newton’s law behind planet motion

Newton’s law of gravitation links falling objects, the Moon’s orbit, and planetary motion. Before Newton, many people thought the sky and Earth followed different laws. Kepler later described the three laws of planetary motion, but their connection to a deeper force was still unclear.

Isaac Newton made that connection in 1665 to 1666. He showed that the same phenomenon explains why objects fall to Earth and why the Moon moves around Earth. He also found that the Moon’s centripetal acceleration and the acceleration due to gravity follow an inverse-square relationship with distance from Earth.

Newton used this idea with his laws of motion to build the law of gravitation. Because acceleration does not depend on mass, the force must be proportional to mass. The law also needs the gravitational constant, which was measured experimentally.

Henry Cavendish carried out the first successful experiment to measure that constant. Once its value was known, Newton’s laws of motion could be combined with gravitation to derive Kepler’s laws of planetary motion. This made gravitation a key link between everyday motion and the motion of the planets.

Newton’s Law Behind Planet Motion

gravitation

Newton’s law of gravitation links falling objects, the Moon’s orbit, and planetary motion. Before Newton, many people thought the sky and Earth followed different laws. Kepler later described the three laws of planetary motion, but their connection to a deeper force was still unclear. Isaac Newton made that connection in 1665 to 1666. He showed that the same phenomenon explains why objects fall to Earth and why the Moon moves around Earth. He also found that the Moon’s centripetal acceleration...

newton's law of gravitation

Newton's Gravity and the Motion of Bodies

Newton's gravity links the fall of objects on Earth with the motion of the Moon and planets. People once thought the downward pull seen near Earth was unique to our planet. Later, Nicolaus Copernicus proposed the heliocentric theory, which placed Earth and the other planets around the Sun, with the Moon orbiting Earth. Isaac Newton connected these motions in the 17th century. He reasoned that the same attraction that keeps the Moon on its path around Earth also makes an apple fall from a tree.

gravitation between spherically symmetric masses

gravitation-between-spherically-symmetric-masses

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Gravitational potential energy for spherically symmetric bodies depends on their masses and the distance between them. The idea is to treat each body as if its mass were concentrated at its center of mass. This makes the calculation easier for high school physics. A spherically symmetric mass can be thought of as many concentric spherical shells. Now place a point mass at a distance r from the center of one shell. Every particle on a given spherical ring is the same distance from that point...

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gravity between spherical bodies

Point-Mass Approximation in Spherical Gravity

Newton’s law of gravitation gives the force between two point masses. For large spherical objects, such as the Earth, the Moon, and other planets, the same law can be used by treating each body as if its mass were concentrated at its center. This idea can be proven by comparing gravitational potential energy. The transcript shows that a hollow sphere of mass M and a point mass m give the same energy result as two extended solid spherical objects. To set up the proof, a tiny ring on the shell...

reduced mass coordinates: isolated two-body problem

reduced-mass-coordinates-isolated-two-body-problem

Center of Mass in the Two-Body Problem

Reduced mass coordinates help simplify the classical two-body problem. In classical mechanics, this problem describes the motion of two interacting bodies under gravity or another central force. The key idea is that the system can be treated like a single-body problem when reduced mass is used. For this description, one body is imagined to move with the reduced mass while the other body is fixed in place with infinite mass. The reduced mass is a property of the two-body system and is defined...

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acceleration due to gravity on earth

Gravity on Earth: Mass, Direction, and Value

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acceleration due to gravity on other planets

acceleration-due-to-gravity-on-other-planets

Measuring Gravity on Distant Planets

Gravity near Earth’s surface is measured as acceleration due to gravity. On Earth, students can test it with simple experiments. On other planets, that kind of direct experiment is not possible. Instead, astronomers use observations to find a planet’s gravity. They study how the planet affects nearby objects, especially its satellite. The key idea is that the acceleration depends on the planet’s gravity, not on the object’s mass. To make the calculation, scientists track a satellite’s path...

apparent weight and the earth's rotation

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variation in acceleration due to gravity near the earth's surface

variation-in-acceleration-due-to-gravity-near-the-earth-s-surface

How Earth’s Shape Affects Apparent Weight

Apparent weight changes slightly on Earth because of rotation and the planet’s shape. Apparent weight is the weight measured by a spring balance at a location. It is different from true weight, which is the force Earth pulls on an object with. Earth’s rotation reduces apparent weight by adding a centripetal force. Centripetal force is the inward force that keeps an object moving in a circle. The apparent weight equals the true weight minus this force. The difference depends on the square of...

potential energy due to gravitation

Gravitational Binding and Potential Energy

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the principle of superposition and the gravitational field

the-principle-of-superposition-and-the-gravitational-field

Adding Gravitational Forces with Superposition

Gravitational forces can be added using the principle of superposition. For objects that are sufficiently far apart, the net gravitational force on a point object is the vector sum of the forces from each mass. This means each force is found first, and then the forces are added as vectors. Superposition is useful because gravity from more than one object can combine in ways that are not always easy to see. One force may be increased or reduced by another force, or the final effect may be a...

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escape velocity

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circular orbits and critical velocity for satellites

circular-orbits-and-critical-velocity-for-satellites

Orbital Speed and Period in Circular Paths

Orbital speed and period in circular paths explain how the Moon, planets, and satellites stay in motion around larger bodies. The Moon orbits Earth. Earth and the other planets orbit the Sun. The space above our atmosphere also contains many artificial satellites. A circular orbit is the simplest orbit to study. It helps show how an object’s speed and its period, or the time for one full orbit, depend on where it is and what it circles. Nicolaus Copernicus first suggested that Earth and the...

energy of a satellite in a circular orbit

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Satellite Orbits and Energy in Space

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kepler's first law of planetary motion

Planet Orbits as Ellipses

Planet orbits are not perfect circles. Johannes Kepler used planet data from Tycho Brahe to show that each planet follows an ellipse, with the Sun at one focus. This idea came from studying Mars, which did not fit the circular path expected in the Copernican heliocentric model. Copernicus had proposed that the solar system is heliocentric, meaning the Sun is at the center and the planets, including Earth, move around it. His model treated those paths as circles. Brahe later recorded the...

kepler's second law of planetary motion

Kepler's Equal-Area Planet Motion

Kepler's second law explains how a planet moves faster and slower in its orbit around the Sun. Johannes Kepler, a German astronomer and mathematician in the early 17th century, developed three laws for planetary motion. His first law says that planets travel in elliptical orbits, with the Sun at one focus of the ellipse. Because the planet-Sun distance changes during the orbit, the planet does not move at the same speed all the time. In an elliptical orbit, the total energy of the planet is...

kepler's third law of planetary motion

Kepler’s Planet Distance Law

Kepler’s third law links a planet’s average distance from the Sun to the time it takes to orbit the Sun. This rule gives a clear mathematical relationship between orbital distance and orbital period, which is the time for one full revolution. Johannes Kepler developed this law in the early 17th century after building on the observations of Nicolaus Copernicus and Tycho Brahe. Kepler first formed his first two laws from those earlier observations. He later published the third law of planetary...

tidal forces

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schwarzschild radius and event horizon

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key terms and concepts

Learn how Newton connected falling objects, the Moon’s orbit, and planetary motion with gravitation, the inverse-square law, and Cavendish’s measurement.

Newton’s Law Behind Planet Motion | JoVE K12

physics

JoVE Core Physics introduces the theory and application of fundamental physics topics, including kinematics, dynamics, fluid mechanics, statics, waves, and acoustics, with concise and easy-to-understand animated videos. Additionally, the scientist-in-action videos demonstrate the application of related concepts in classical and original research experiments performed in today's laboratories worldwide.

Pennsylvania State Academic Standards

Physical Science

Forces and Interactions

3.2.9-12.L

3.2.9-12.M

Louisiana Student Standards for Science

High School

Earth Science

Earth’s Place In The Universe

HS-ESS1-4

Motion And Stability: Forces And Interactions

HS-PS2-5

HS-PS2-4

ohios-learning-standards-and-model-curriculum

Ohio’s Learning Standards and Model Curriculum

Forces, Momentum And Motion

Gravitational force and fields

Energy

Gravitational potential energy

Tennessee Academic Standards

Motion and Stability: Forces and Interactions

PHYS.PS2.5

PHYS.PS2.9

Virginia  Standards of Learning

HIgh School

ES.3

ES.3.b

PH.3

PH.3.b

PH.7

PH.7.a

PH.7.b

Minnesota Academic Standards in Science

2.2.1 9P.1.2.1.2

Arizona Science Standards

Earth and Space Science

HS.E2

HS.E2U1.16

HS+E.E2

HS+E.E2U1.13

new-jersey-student-learning-standards-for-science

New Jersey Student Learning Standards for Science

HS.P2

HS.P2U1.5

Alabama Course of Study Science

waves-and-their-applications-in-technologies-for-information-transfer

Waves and Their Applications in Technologies for Information Transfer

9-12.PS.2.3.a

9-12.P.1.2.d

9-12.P.1.5.b

Texas Essential Knowledge and Skills

Astronomy

112.48.c.11.

112.48.c.11.D.

Next Generation Science Standards

Earth’s Place in the Universe

Florida Department of Education

SC.912.E.5

SC.912.E.5.6

SC.912.E.5.10

SC.912.E.5.11

SC.912.P.10

SC.912.P.10.10

SC.912.P.12

SC.912.P.12.4

PHYS.5

PHYS.5.F

PHYS.5.H

south-carolina-college-and-career-ready-science-standards

South Carolina College and Career Ready Science Standards

P-PS2-4

Earth and Space Science (ESS)

E-ESS1-6.

new-york-state-science-learning-standards

New York State Science Learning Standards

HS. Forces and Interactions

HS-PS2-4.

Earth and Space Sciences

Space Systems

HS-ESS1-4.

Georgia Standards of Excellence

SPS8.

Gravitational Force

SP2.

Common Forces

SP5.

Gravitational Forces

Position and Displacement

The position of an object defines its location relative to a convenient frame of reference at any particular time. A frame of reference is an arbitrary ...

Average Velocity

To calculate the other physical quantities in kinematics, we must introduce the time variable. The time variable allows us not only to state the position ...

Instantaneous Velocity - I

The average velocity during a time interval cannot tell us how fast or in what direction a particle is moving at any given time during the interval. To ...

Instantaneous Velocity - II

Instantaneous velocity is the quantity that measures how fast an object is moving along its path. In other words, the instantaneous velocity of an object ...

Use models (graphs, equations, diagrams) to infer motion in one dimension.

PS.Phy.1.1

Analyze the motion of objects using time, distance, displacement, speed, velocity, and acceleration.

Newton’s Law Behind Planet Motion

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Transcript

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