Name: how the moon shapes earth’s tides
Uploaded: 2023-04-30T11:07:23.000Z
Duration: 1 min 6 s
Channel: JoVE

K12 Standards

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

NC K-12 Science Standard Course of Study

9-12

Earth and Environmental Science

Earth's Place in the Universe

ESS.EES.1.1

Tidal Forces

Yerçekimi kuvvetleri, iki nokta kütlesi arasındaki mesafeye bağlıdır. Bununla birlikte, Dünya gibi genişlemiş bir nesne için, Güneş'in Güneş'e bakan tarafa etki eden yerçekimi kuvveti, diğer taraftakinden daha yüksektir.
Fg, Dünya'nın merkezine etki eden ortalama yerçekimi kuvveti ise, kuvvetlerdeki fark gelgit kuvvetlerine yol açar. A ve B'deki bileşke kuvvetler Dünya'nın merkezinden uzağa yönlendirilir.
C ve D'ye etki eden kuvvetlerin farklı yönleri vardır. Dolayısıyla, bu iki noktadaki bileşke kuvvetler Dünya'nın merkezine doğru yönlendirilir.
Bu nedenle, ortaya çıkan artık kuvvetler Dünya'yı şişirilmiş bir küre haline getirir. Dünya yüzeyinin çoğu okyanuslardan oluştuğundan, bu etki belirgin bir şekilde bir çift yüksek gelgit ve düşük gelgit olarak görülür.
Ay'dan kaynaklanan gelgit kuvvetlerinin Dünya üzerindeki etkisi, Ay'ın yakınlığı ve karşılaştırılabilir boyutu nedeniyle Güneş'ten yaklaşık 2,2 kat daha güçlüdür.

gelgit kuvvetleri

Dünya'nın okyanus gelgiti kökeni, sürekli olarak 2000 yılı aşkın süredir araştırma konusu olmuştur. Ancak, Newton'ın çalışması olayın doğru anlaşılmasının başlangıcı olarak kabul edilir. Okyanus gelgiti, yerçekimi gelgit kuvvetlerinin bir sonucudur. Bu aynı gelgit kuvvetleri, herhangi bir gök cisminde mevcuttur; bunlar, Jüpiter'in uydularından biri olan Io'da volkanik aktivite yaratan içsel ısıdan ve siyah deliklere çok yaklaşan yıldızların parçalanmasından sorumludur.

Newton'ın yerçekimi yasası, yerçekimi kuvvetinin iki nokta kütlesi arasındaki mesafenin karesine ters orantılı olduğunu belirtir. Ancak, Dünya gibi geniş bir nesne için, Güneş'e bakan taraf üzerinde etki eden yerçekimi kuvveti diğer taraf üzerinde etki eden yerçekimi kuvvetinden çok daha yüksektir. Farklı konumlardaki bu kuvvet farkı, iki kütlenin arasındaki mesafenin kübüne ters orantılı olan gelgit kuvvetlerinin ortaya çıkmasına neden olur.

Deniz seviyeleri, Ay'ın yerçekimi kuvvetinden dolayı yerçekimi kuvvetlerinin etkisiyle günde iki kez yükselir. Güneş, Ay'dan 27 milyon kat daha kütlelidir, ancak Güneş'in Dünya'dan uzaklığı, Dünya ve Ay arasındaki mesafeden yaklaşık 390 kat daha fazladır. Çünkü gelgit kuvvetleri, mesafenin küpüne ters orantılıdır, Güneş'in gelgit kuvveti Ay'ın yaklaşık yarısıdır.

Ay, Dünya üzerinde gelgitlere sebep olan baskın kuvvettir, ancak Güneşin hala bir etkisi vardır. Gelgitler, üç cismin yönelimine bağlı olarak değişir. Güneş, Dünya ve Ay hizalanmış olduğunda, yani Dolunay veya Yeniay gününde, gelgit kuvvetleri toplanır ve gelgitlerin amplitüdü maksimum olur. Bunlara "İlkbahar gelgitleri" denir. Yarı Ay gününde, Ay, Güneş-Dünya çizgisine dik olarak yer alır. Burada, gelgitler en küçüktür ve "Düşük gelgitler" olarak adlandırılır.

ünya'nın dönmesi ve Ay'ın yörüngesi, gelgit sürelerinin hesaplamasını daha da karmaşık hale getirir. Bununla birlikte, yaklaşık olarak ardışık yüksek (veya alçak) gelgitler arasındaki süre 12.5 saat olarak kabul edilebilir.

Bu metin, <a href="https://openstax.org/books/university-physics-volume-1/pages/13-6-tidal-forces">Openstax, University Physics Volume 1, Section 13.6: Tidal Forces'tan uyarlanmıştır.</a>

Gelgit Kuvvetleri

Dünya'nın okyanus gelgitlerinin kökeni, 2000 yılı aşkın bir süredir sürekli bir araştırma konusu olmuştur. Bununla birlikte, Newton'un çalışmasının ...

Education

JoVE Core

Physics

Fizik

Unit 1

Ünite 1

Gravitation

Kütleçekimi

KEY TERMS AND CONCEPTS

TEMEL TERİMLER VE KAVRAMLAR

how the moon shapes earth’s tides

Earth’s ocean tides are driven by gravitational tidal forces. Scientists have studied the origin of tides for more than 2000 years, and Newton’s work marked the start of a proper understanding. These same tidal forces also act on other astronomical bodies. They can produce internal heat that leads to volcanic activity on Io, one of Jupiter’s moons, and they can tear apart stars that pass too close to black holes.

Newton’s law of gravitation says that gravitational force is inversely proportional to the square of the distance between two point masses. Earth, however, is not a point mass. The side facing the Sun feels a stronger pull than the side farther away. That difference in gravity across an extended object creates tidal forces. For tidal forces, the strength falls off with the cube of the distance between the two masses.

On Earth, sea level rises twice a day mainly because of the Moon’s tidal force. The Sun is much more massive than the Moon, but it is also much farther from Earth. Even though the Sun is about 27 million times more massive, its tidal force is only about half as strong as the Moon’s because tidal forces depend strongly on distance. The Moon is the main cause of Earth’s tides, but the Sun still changes them.

The size of the tides depends on how the Sun, Earth, and Moon are lined up. When they are aligned during a Full Moon or New Moon, the tidal forces add together and the tide height is greatest. These larger tides are called spring tides. During a Half Moon, the Moon is at right angles to the Sun-Earth line. Then the tides are smallest, and they are called neap tides.

Earth’s rotation and the Moon’s revolution make the timing of tides more complicated. Even so, the time between one high tide and the next, or one low tide and the next, is about 12.5 hours. That pattern helps explain why coastal water levels rise and fall in a regular cycle.

How the Moon Shapes Earth’s Tides

gravitation

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...

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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

Gravitational Potential Inside a Shell

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

Gravity near Earth gives objects a downward acceleration called acceleration due to gravity. It comes from Earth’s gravitational pull and points toward the center of the Earth. Newton’s law of gravitation shows that the gravitational force depends on mass, while Newton’s second law shows that the acceleration produced by a force depends on how that force acts on the object. Because of this relationship, the acceleration due to gravity is independent of an object’s mass. An object and the Earth...

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

Earth's Spin and Apparent Weight

Earth’s spin changes how weight is measured on the surface. Because the Earth turns once every 24 hours, objects on the surface move in a circle. That motion requires a net centripetal force, which points toward the center of the circle. The north and south poles are the only exception. At the equator, the force that provides this inward pull comes from Earth’s gravity. It is the difference between an object’s true weight and the normal force from the ground. The normal force is the support...

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

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potential energy due to gravitation

Gravitational Binding and Potential Energy

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the principle of superposition and the gravitational field

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Adding Gravitational Forces with Superposition

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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

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energy of a satellite in a circular orbit

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Satellite Orbits and Energy in Space

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kepler's second law of planetary motion

Kepler's Equal-Area Planet Motion

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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

Earth’s ocean tides are driven by gravitational tidal forces. Scientists have studied the origin of tides for more than 2000 years, and Newton’s work marked the start of a proper understanding. These same tidal forces also act on other astronomical bodies. They can produce internal heat that leads to volcanic activity on Io, one of Jupiter’s moons, and they can tear apart stars that pass too close to black holes. Newton’s law of gravitation says that gravitational force is inversely...

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detection of black holes

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key terms and concepts

Learn how the Moon and Sun create Earth’s tides, why spring and neap tides happen, and why high tides repeat about every 12.5 hours.

How the Moon Shapes Earth’s Tides | JoVE K12

physics

JoVE Temel Fizik, kinematik, dinamik, akışkanlar mekaniği, statik, dalgalar ve akustik dahil olmak üzere temel fizik konularının teorisini ve uygulamasını kısa ve anlaşılması kolay animasyonlu videolarla tanıtıyor. Ek olarak, sektör içindeki bilim insanı videoları, dünya çapındaki günümüz laboratuvarlarında gerçekleştirilen klasik ve orijinal araştırma deneylerinde ilgili kavramların uygulanmasını göstermektedir.

Pennsylvania State Academic Standards

Earth and Space Science

History of Earth

3.3.9-12.F

3.3.9-12.J

Space Systems

3.3.9-12.D

Weather and Climate

3.3.9-12.E

Louisiana Student Standards for Science

High School

Earth Science

Earth’s Systems

HS-ESS2-4

ohios-learning-standards-and-model-curriculum

Ohio’s Learning Standards and Model Curriculum

Physical Geology

igneous-metamorphic-and-sedimentary-rocks

Igneous, Metamorphic And Sedimentary Rocks

Ocean

Virginia  Standards of Learning

HIgh School

ES.3

ES.3.a

ES.3.b

PH.3

PH.3.b

Arizona Science Standards

HS.E2

HS.E2U1.16

Alabama Course of Study Science

9-12.ESS.1.2.d

Florida Department of Education

SC.912.E.5

SC.912.E.5.6

SC.912.E.5.10

Georgia Standards of Excellence

Astronomy

SAST2

SAST1.2

Oceanography

SO5.

SO5.3

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Energy Dynamics

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Use models to illustrate how the sun produces energy.

ESS.EES.1.3

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ESS.EES.1.4

Explain how Earth's position relative to the sun influences conditions on Earth.

How the Moon Shapes Earth’s Tides

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