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Astronomy > Historical Models > Flashcards

Historical Models Flashcards

1
Q

Geocentric Model

A

Uniform motion, earth is center of solar system

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2
Q

Problems with the geocentric model

A

mercury and venus would show up in the wrong spots, retrograde, varying brightnesses

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3
Q

Ptolemv

A

Added epicycles that moved at a uniform rate to the geocentric model, fixed retrograde and varying brightness problem and mercury and venus problems

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4
Q

Copernican Heliocentric Model

A

Put the sun at the center of the universe, planets orbit sun, earth rotates on axis, planets have their own speeds (explained retrograde motion and varying brightness), no problems with mercury and venus

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5
Q

Retrograde motion

A

Planets catching up to each other and passing one another, due to varying orbital speeds

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6
Q

Tycho Brahe

A

Wanted to record more accurate data, favored geocentric model, collected 20 years of precise measurements

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7
Q

Johannes Kepler

A

neither model is satisfactory when circles are used

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8
Q

Kepler’s 1st Law

A

Each planet’s path around the sun is an ellipse, with the sun at one focus

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9
Q

Kepler’s 2nd Law

A

A planet moves along its elliptical path with a speed that changes in such a way that a line from the planet to the sun sweeps out equal areas in equal intervals of time (Equal areas in equal time)

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10
Q

Kepler’s 3rd Law

A

The ratio of the cube of a planet’s average distance from the sun to the square of its orbital period is the same for each planet (a^3/p^2 = 1) (a is average distance in AU) (p is the orbital period in years)

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11
Q

Galileo Galali

A

Saw mountains on the moon, saw sunspots, saw 4 moons of jupiter, observed the phases of venus

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12
Q

What broke the geocentric model?

A

The observation of the phases of venus

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13
Q

Parallax Effect

A

If you close one eye and then switch eyes a close object will jump

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14
Q

What broke the sphere of stars?

A

The parallax effect, stars are not the same distance away

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15
Q

Isaac Newton

A

Formulated laws of motion

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16
Q

Newton’s 1st Law

A

Law of inertia, unless an object is acted on by a net, outside force, the object will maintain a constant speed in a straight line (natural state of motion is constant velocity)

17
Q

Newton’s 2nd Law

A

The acceleration of an object is directly proportional to the net force applied and inversely proportional to its mass (larger the mass the less the acceleration)
F=acceleration x mass

18
Q

How does an acceleration occur?

A

An applied force causes a change in speed of direction of the velocity vector

19
Q

Newton’s 3rd Law

A

When object x exerts a force on object y, object y exerts an equal magnitude and opposite directional force on x (Ice skating example)

20
Q

Newton’s Law of Universal Gravitation

A

F = (Gm1m2)/ (R^2)
R is the distance between objects
Force between two objects is always attractive

21
Q

Mass

A

A property of matter, how much stuff an object has, stays the same no matter the planet

22
Q

Weight

A

Due to the gravitational pull of the earth’s mass on our mass, W = mass x gravity, earth’s gravity = 9.8 m/s^2

23
Q

How does moon orbit earth?

A

Circular motion, the gravitational force between the moon and the earth accelerates the moon towards earth, the moon is constantly falling towards earth but never hits due to its inertia.

24
Q

Center of Mass

A

The point to balance out two objects, said objects orbit the center of mass.

25
Q

Bary Center

A

Sun and 9 planets move about this point, sits just outside the sun

26
Q

Equivalence Principle

A

Effects of gravity are indistinguishable from the effects of acceleration, mass can bend 4 dimensional space-time, gravity is caused by gravitational potential wells in 4D

27
Q

Einstein’s 1st Prediction

A

The bending of light around a large mass was predicted a verified by general relativity

28
Q

Correspondence Principle

A

To replace a theory the new theory must do everything the old one did and more.

29
Q

Where did Newton and Einstein match in ideas?

A

The paralleling of mercury

Astronomy (10 decks)

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