Name: planet orbits as ellipses
Uploaded: 2025-05-22T09:05:41.000Z
Duration: 1 min 10 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

Earth and Environmental Science

Earth's Place in the Universe

ESS.EES.1.1

Kepler's First Law of Planetary Motion

Johannes Kepler, birinci yasasında her gezegenin eliptik bir yörünge izlediğini ve odaklarından birinde Güneş'in olduğunu belirtti.
Eliptik yörüngede, bir gezegen günberi noktası A'da Güneş'e en yakın ve günöte noktası B'de olduğunda Güneş'e en uzaktır. Gezegenin Güneş'ten ortalama uzaklığı, elipsin yarı ana eksenine eşittir.
Günberide, gezegenin potansiyel enerjisi günötedekinden daha düşüktür, çünkü rA mesafesi rB mesafesinden daha küçüktür.
Enerji korunumu ilkesine göre, gezegenin kapalı bir yörüngedeki toplam enerjisi korunur. Bu nedenle, gezegenin günberideki kinetik enerjisi günötedekinden daha yüksektir.
Kinetik enerji, gezegenin kütlesinin çarpımı ile yörünge hızının karesinin yarısına eşit olduğundan, gezegen günberi vaktinde Güneş'e daha yakın olduğunda yörüngesinde daha hızlı hareket eder ve Güneş'ten uzakta olduğunda yavaşlar.

kepler'in gezegen hareketi birinci yasası

17. yüzyılın başlarında, Alman gökbilimci ve matematikçi Johannes Kepler, güneş sistemindeki gezegenlerin hareketi için üç yasa ileri sürdü. Kepler, bu ilk iki yasayı, öncülerinin Nikolaus Copernicus ve Tycho Brahe'nin gözlemlerine dayanarak formüle etti.

Polonyalı gökbilimci Nikolaus Copernicus, güneş sistemi için güneşmerkezli bir modeli önerdi. Bu güneşmerkezli teoride, Dünya da dahil olmak üzere bütün gezegenler, Güneş etrafında dairevi yörüngelerde dönerler.

Öte yandan Johannes Kepler'ın işvereni olan Danimarkalı gökbilimci Tycho Brahe, her gezegenin pozisyonunu ayrıntılı olarak kaydetmişti. Çoğu görülebilir gezegen için, bu gözlemler, Kopernik güneşmerkezli teorisiyle uyumluydu, ancak Mars gezegeni için durum farklıydı.

Tycho Brahe'nin Mars verilerini analiz ederken, Johannes Kepler gezegenlerin dairesel değil de eliptik yörüngelerde Güneş etrafında döndüğünü fark etti. Bu da onu gezegen hareketlerinin birinci yasasına götürdü, bu yasa her gezegenin bir elips boyunca yol aldığını ve Güneş'in bu elipsin bir fokusunda bulunduğunu belirtmektedir.

Bir elips, uzunlamasına uzatılmış bir çemberdir. Bir elipsin ne kadar uzunlamasına uzandığı, eksantriklik adı verilen bir parametre kullanılarak ifade edilir.

<img alt="Equation1" src="/files/ftp_upload/12754/12754_Figure_1.png" style="text-align: center; height: 500px;" />

Bir elipsin uzantısı boyunca olan ekseni büyük eksen a, buna perpendicular olan ise küçük eksen b olarak adlandırılır. Dolayısıyla, bir elipsin eksantrikliği şu şekilde ifade edilir:

<img alt="Equation1" src="/files/ftp_upload/12754/12754_Equations_1.png" style="text-align: center; height: 50px;" />

b < a olduğu için, bir elipsin eksantrikliği her zaman birimden küçüktür. Bir çember için a = b olduğundan, çemberin eksantrikliği sıfırdır.

Mars'ın yörüngesinin eksantrikliği 0.0935'tir. Bu, en yüksek eksantrikliği olan gezegenin Merkür olduğu düşünülür, çünkü onun eksantrikliği 0.21'dir. Dünya'nın yörüngesinin eksantrikliği ise 0.0167'dir.

Gezegenler, Güneş'in bir fokusunda bulunan eliptik yörüngelerde bulunduklarından dolayı, yıllar boyunca radyal uzaklıkları değişir. Onların Güneş'e en yakın olan mesafesi periheliyken, daha uzak olan mesafe ise apoheli olarak adlandırılır.

Bu metin <a href="https://openstax.org/books/university-physics-volume-1/pages/13-5-keplers-laws-of-planetary-motion">Openstax, University Physics Volume 1, Section 13.5 Kepler's Laws of Motion</a> adlı kaynaktan uyarlanmıştır.

Kepler'in Gezegen Hareketi Birinci Yasası

17. yüzyılın başlarında, Alman gökbilimci ve matematikçi Johannes Kepler, güneş sistemindeki gezegenlerin hareketi için üç yasa öne sürdü. O...

Education

JoVE Core

Physics

Fizik

Unit 1

Ünite 1

Gravitation

Kütleçekimi

KEY TERMS AND CONCEPTS

TEMEL TERİMLER VE KAVRAMLAR

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 positions of the planets in great detail, and most of the visible planets matched the Copernican picture. Mars was the major exception.

An ellipse is an elongated circle. Its longest axis is the major axis, marked a, and the shorter axis across it is the minor axis, marked b. The amount of stretch is called eccentricity. Because b is less than a, the eccentricity of an ellipse is always less than 1, and a circle has an eccentricity of zero because its sides are equal.

Kepler’s orbit model also explains why a planet’s distance from the Sun changes during the year. The closest point is called perigee, and the farthest point is called apogee. Mars has an eccentricity of 0.0935, which is the most eccentric orbit after Mercury at 0.21. Earth’s orbit is much closer to a circle, with an eccentricity of 0.0167.

Planet Orbits as Ellipses

gravitation

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acceleration due to gravity on other planets

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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...

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kepler's third law of planetary motion

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key terms and concepts

Learn how Kepler used Mars data to show that planets move in ellipses, not perfect circles, and why eccentricity changes a planet’s distance from the Sun.

Planet Orbits as Ellipses | JoVE K12

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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.

ESS.EES.1.2

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Motion and Stability- Forces and Interactions

PS.Phy.2.4

Pennsylvania State Academic Standards

Earth and Space Science

Space Systems

3.3.9-12.A

3.3.9-12.D

Weather and Climate

3.3.9-12.E

Louisiana Student Standards for Science

High School

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Earth’s Place In The Universe

HS-ESS1-1

HS-ESS1-2

HS-ESS1-3

HS-ESS1-4

Virginia  Standards of Learning

HIgh School

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ES.2.c

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New Jersey Student Learning Standards for Science

Alabama Course of Study Science

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112.48.c.9.

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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

PHYS.5

PHYS.5.H

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South Carolina College and Career Ready Science Standards

Earth and Space Science (ESS)

E-ESS1-4.

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New York State Science Learning Standards

Earth and Space Sciences

HS-ESS1-4.

Georgia Standards of Excellence

SAST1

SAST1.1

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ESS.EES.1.3

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Planet Orbits as Ellipses

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