Matières

Physique/Chimie

Propriétés physico-chimiques

Mouvements et interactions

Mouvement dans un champ de gravitation

Apprends le Mouvement Circulaire avec des Exercices et PDF!

Name: Knowunity
Brand: Knowunity

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Apprends le Mouvement Circulaire avec des Exercices et PDF!

Luna

@luna.mni

22 Abonnés

Suivre

Les mouvements circulaires uniformes physiques et les lois de Kepler pour trajectoires elliptiques sont des concepts fondamentaux en mécanique céleste. Ce document explore ces principes, en mettant l'accent sur les mouvements des satellites et des planètes.

Points clés :

Définition et caractéristiques du mouvement circulaire uniforme
Les trois lois de Kepler et leur application aux orbites planétaires
Étude des satellites terrestres, y compris les satellites géostationnaires à une altitude de 36000 km
Calculs de la force gravitationnelle, de la vitesse et de la période des satellites
Application pratique à l'étude des satellites de Jupiter

22/02/2023

356

Les Mouvements:
Mouvement wiculaire...
- Trajectoire
= arc de cercle de rayon R.
Repere de remet:olinu supidada
(, um UE): repère
mobile lié

Voir

Circular Motion and Newton's Second Law

This page introduces the concept of circular motion and its key components. It explains the trajectory and reference frame used in analyzing circular motion.

Vocabulary: Circular motion refers to the movement of an object in a circular path.

The page describes the unit vectors used in circular motion analysis:

Ut: Tangential unit vector
Un: Normal unit vector (perpendicular to the trajectory)

It also presents the velocity and acceleration formulas for circular motion:

v = v · ut
a = an · un + at · ut

Highlight: For uniform circular motion, velocity magnitude is constant, and acceleration is purely centripetal (a = v²/R · un).

The page concludes with a statement of Newton's Second Law, which is fundamental to understanding the forces involved in circular motion.

Definition: Newton's Second Law states that the sum of forces applied to a solid is equal to the product of its mass and acceleration.

Voir

Satellite Velocity and Period

This page continues the analysis of satellite motion, focusing on deriving expressions for satellite velocity and orbital period.

The velocity of a satellite in circular orbit is derived as: v = √(G · MT / R)

Where:

G is the gravitational constant
MT is the mass of Earth
R is the orbital radius

Highlight: This equation shows that satellite velocity depends on the mass of the central body and the orbital radius.

The page then derives the expression for the orbital period of a satellite, which is a direct application of Kepler's Third Law:

T = 2π · √(R³ / (G · MT))

Example: This formula is used to calculate the orbital periods of satellites and planets, demonstrating the practical application of Kepler's laws.

The derivation of these formulas provides a deep understanding of the relationship between a satellite's orbital characteristics and the properties of the central body it orbits.

Voir

Universal Law of Gravitation and Satellite Motion

This page focuses on the universal law of gravitation and its application to satellite motion around Earth.

Definition: The universal law of gravitation states that the gravitational force between two masses is proportional to the product of their masses and inversely proportional to the square of the distance between them.

The mathematical expression for the gravitational force is given as: F = G · (M1 · M2) / r²

Where:

G is the gravitational constant (6.67 × 10⁻¹¹ N·m²/kg²)
M1 and M2 are the masses of the two objects
r is the distance between their centers

The page then applies Newton's Second Law to derive the acceleration of a satellite orbiting Earth:

a = -G · MT / R² · ur

Where:

MT is the mass of Earth
R is the distance from the center of Earth to the satellite
ur is the radial unit vector

Example: This derivation is crucial for understanding the motion of artificial satellites and natural moons around planets.

Voir

Geostationary Satellite Altitude Calculation

This final page focuses on deriving and calculating the altitude of a geostationary satellite.

The derivation starts with Kepler's Third Law and the expression for orbital velocity:

R³ = (T² · G · MT) / (4π²)

Where:

R is the orbital radius
T is the orbital period (24 hours for a geostationary satellite)
G is the gravitational constant
MT is the mass of Earth

Highlight: The calculation demonstrates that the altitude of a geostationary satellite is approximately 36,000 km above Earth's surface.

Given:

Earth's radius: 6,371 km
Earth's mass: 6.0 × 10²⁴ kg

The page shows the step-by-step calculation to arrive at the final result:

h = R - RT ≈ 36,000 km

Example: This calculation is crucial for understanding the placement of communication satellites and other space-based technologies that require a fixed position relative to Earth's surface.

The derivation and calculation of geostationary satellite altitude serve as a practical application of Kepler's laws and orbital mechanics, demonstrating the power of these principles in modern space technology.

Voir

Kepler's Laws of Planetary Motion

This page delves into Kepler's three laws of planetary motion, providing a comprehensive overview of each law and its implications for celestial mechanics.

Highlight: Kepler's laws describe the motion of planets around the Sun and are crucial for understanding orbital dynamics.

First Law of Kepler (Law of Ellipses):

Definition: In the heliocentric reference frame, the trajectory of a planet's or satellite's center around a celestial body is an ellipse with the Sun at one of its foci.

Second Law of Kepler (Law of Equal Areas):

Definition: The line segment connecting the Sun to a planet sweeps out equal areas during equal intervals of time.

This law implies that planets move faster when they are closer to the Sun (perihelion) and slower when they are farther away (aphelion).

Third Law of Kepler (Law of Periods):

Definition: The ratio of the square of the orbital period to the cube of the semi-major axis is constant for all planets.

The page provides the mathematical formulation of the third law: T² / a³ = 4π² / (G · Ms)

Where:

T is the orbital period
a is the semi-major axis
G is the gravitational constant
Ms is the mass of the Sun

Voir

Geostationary Satellites and Planetary Motion

This page discusses the characteristics of geostationary satellites and applies Kepler's laws to planetary motion.

Definition: A geostationary satellite is a satellite that remains stationary relative to Earth's surface, orbiting in the equatorial plane with the same rotational period as Earth.

Key characteristics of geostationary satellites:

Orbital plane coincides with Earth's equatorial plane
Rotates in the same direction as Earth
Orbital period equals Earth's rotational period (24 hours)
Altitude is approximately 36,000 km

Example: The page provides a practical application by calculating the mass of Jupiter using the orbital period of one of its moons.

Given:

Jupiter's radius: 69,911 km
Satellite's orbital period: 1 day, 18 hours, 20 minutes

Using Kepler's Third Law, the mass of Jupiter is calculated to be approximately 1.94 × 10²⁷ kg.

This example demonstrates how Kepler's laws can be applied to determine the properties of celestial bodies based on the motion of their satellites.

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Knowunity est la meilleure application scolaire dans cinq pays européens.

Knowunity a été mis en avant par Apple et a toujours été en tête des classements de l'App Store dans la catégorie Éducation en Allemagne, en Italie, en Pologne, en Suisse et au Royaume-Uni. Rejoins Knowunity aujourd'hui et aide des millions d'étudiants à travers le monde.

Chargement dans le

Google Play

Chargement dans le

App Store

Knowunity est la meilleure application scolaire dans cinq pays européens.

4.9+

Note moyenne de l'appli

13 M

Les élèsves utilisent Knowunity

#1

Dans les palmarès des applications scolaires de 12 pays

950 K+

Les élèves publient leurs fiches de cours

Tu n'es toujours pas convaincu ? Regarde ce que disent les autres élèves ...

Louis B., utilisateur iOS

J'aime tellement cette application [...] Je recommande Knowunity à tout le monde ! !! Je suis passé de 11 à 16 grâce à elle :D

Stefan S., utilisateur iOS

L'application est très simple à utiliser et bien faite. Jusqu'à présent, j'ai trouvé tout ce que je cherchais :D

Lola, utilisatrice iOS

J'adore cette application ❤️ Je l'utilise presque tout le temps pour réviser.

Matières

Physique/Chimie

Propriétés physico-chimiques

Mouvements et interactions

Mouvement dans un champ de gravitation

Apprends le Mouvement Circulaire avec des Exercices et PDF!

Luna

@luna.mni

22 Abonnés

Suivre

Points clés :

Définition et caractéristiques du mouvement circulaire uniforme
Les trois lois de Kepler et leur application aux orbites planétaires
Étude des satellites terrestres, y compris les satellites géostationnaires à une altitude de 36000 km
Calculs de la force gravitationnelle, de la vitesse et de la période des satellites
Application pratique à l'étude des satellites de Jupiter

22/02/2023

356

Tle

Physique/Chimie

Circular Motion and Newton's Second Law

This page introduces the concept of circular motion and its key components. It explains the trajectory and reference frame used in analyzing circular motion.

Vocabulary: Circular motion refers to the movement of an object in a circular path.

The page describes the unit vectors used in circular motion analysis:

Ut: Tangential unit vector
Un: Normal unit vector (perpendicular to the trajectory)

It also presents the velocity and acceleration formulas for circular motion:

v = v · ut
a = an · un + at · ut

Highlight: For uniform circular motion, velocity magnitude is constant, and acceleration is purely centripetal (a = v²/R · un).

The page concludes with a statement of Newton's Second Law, which is fundamental to understanding the forces involved in circular motion.

Definition: Newton's Second Law states that the sum of forces applied to a solid is equal to the product of its mass and acceleration.

Satellite Velocity and Period

This page continues the analysis of satellite motion, focusing on deriving expressions for satellite velocity and orbital period.

The velocity of a satellite in circular orbit is derived as: v = √(G · MT / R)

Where:

G is the gravitational constant
MT is the mass of Earth
R is the orbital radius

Highlight: This equation shows that satellite velocity depends on the mass of the central body and the orbital radius.

The page then derives the expression for the orbital period of a satellite, which is a direct application of Kepler's Third Law:

T = 2π · √(R³ / (G · MT))

Example: This formula is used to calculate the orbital periods of satellites and planets, demonstrating the practical application of Kepler's laws.

The derivation of these formulas provides a deep understanding of the relationship between a satellite's orbital characteristics and the properties of the central body it orbits.

Universal Law of Gravitation and Satellite Motion

This page focuses on the universal law of gravitation and its application to satellite motion around Earth.

Definition: The universal law of gravitation states that the gravitational force between two masses is proportional to the product of their masses and inversely proportional to the square of the distance between them.

The mathematical expression for the gravitational force is given as: F = G · (M1 · M2) / r²

Where:

G is the gravitational constant (6.67 × 10⁻¹¹ N·m²/kg²)
M1 and M2 are the masses of the two objects
r is the distance between their centers

The page then applies Newton's Second Law to derive the acceleration of a satellite orbiting Earth:

a = -G · MT / R² · ur

Where:

MT is the mass of Earth
R is the distance from the center of Earth to the satellite
ur is the radial unit vector

Example: This derivation is crucial for understanding the motion of artificial satellites and natural moons around planets.

Geostationary Satellite Altitude Calculation

This final page focuses on deriving and calculating the altitude of a geostationary satellite.

The derivation starts with Kepler's Third Law and the expression for orbital velocity:

R³ = (T² · G · MT) / (4π²)

Where:

R is the orbital radius
T is the orbital period (24 hours for a geostationary satellite)
G is the gravitational constant
MT is the mass of Earth

Highlight: The calculation demonstrates that the altitude of a geostationary satellite is approximately 36,000 km above Earth's surface.

Given:

Earth's radius: 6,371 km
Earth's mass: 6.0 × 10²⁴ kg

The page shows the step-by-step calculation to arrive at the final result:

h = R - RT ≈ 36,000 km

Example: This calculation is crucial for understanding the placement of communication satellites and other space-based technologies that require a fixed position relative to Earth's surface.

Kepler's Laws of Planetary Motion

This page delves into Kepler's three laws of planetary motion, providing a comprehensive overview of each law and its implications for celestial mechanics.

Highlight: Kepler's laws describe the motion of planets around the Sun and are crucial for understanding orbital dynamics.

First Law of Kepler (Law of Ellipses):

Definition: In the heliocentric reference frame, the trajectory of a planet's or satellite's center around a celestial body is an ellipse with the Sun at one of its foci.

Second Law of Kepler (Law of Equal Areas):

Definition: The line segment connecting the Sun to a planet sweeps out equal areas during equal intervals of time.

This law implies that planets move faster when they are closer to the Sun (perihelion) and slower when they are farther away (aphelion).

Third Law of Kepler (Law of Periods):

Definition: The ratio of the square of the orbital period to the cube of the semi-major axis is constant for all planets.

The page provides the mathematical formulation of the third law: T² / a³ = 4π² / (G · Ms)

Where:

T is the orbital period
a is the semi-major axis
G is the gravitational constant
Ms is the mass of the Sun

Geostationary Satellites and Planetary Motion

This page discusses the characteristics of geostationary satellites and applies Kepler's laws to planetary motion.

Definition: A geostationary satellite is a satellite that remains stationary relative to Earth's surface, orbiting in the equatorial plane with the same rotational period as Earth.

Key characteristics of geostationary satellites:

Orbital plane coincides with Earth's equatorial plane
Rotates in the same direction as Earth
Orbital period equals Earth's rotational period (24 hours)
Altitude is approximately 36,000 km

Example: The page provides a practical application by calculating the mass of Jupiter using the orbital period of one of its moons.

Given:

Jupiter's radius: 69,911 km
Satellite's orbital period: 1 day, 18 hours, 20 minutes

Using Kepler's Third Law, the mass of Jupiter is calculated to be approximately 1.94 × 10²⁷ kg.

This example demonstrates how Kepler's laws can be applied to determine the properties of celestial bodies based on the motion of their satellites.

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Rien ne te convient ? Explore d'autres matières.

Knowunity est la meilleure application scolaire dans cinq pays européens.

Knowunity a été mis en avant par Apple et a toujours été en tête des classements de l'App Store dans la catégorie Éducation en Allemagne, en Italie, en Pologne, en Suisse et au Royaume-Uni. Rejoins Knowunity aujourd'hui et aide des millions d'étudiants à travers le monde.

Chargement dans le

Google Play

Chargement dans le

App Store

4.9+

Note moyenne de l'appli

13 M

Les élèsves utilisent Knowunity

#1

Dans les palmarès des applications scolaires de 12 pays

950 K+

Les élèves publient leurs fiches de cours

Tu n'es toujours pas convaincu ? Regarde ce que disent les autres élèves ...

Louis B., utilisateur iOS

J'aime tellement cette application [...] Je recommande Knowunity à tout le monde ! !! Je suis passé de 11 à 16 grâce à elle :D

Stefan S., utilisateur iOS

L'application est très simple à utiliser et bien faite. Jusqu'à présent, j'ai trouvé tout ce que je cherchais :D

Lola, utilisatrice iOS