models of the solar system positions of planets change, whereas stars appear relatively ‘fixed’...

Models of the Solar System• Positions of planets change, whereas stars

appear relatively ‘fixed’

• Greeks held on to the Geocentric model because they could not observe stars to change their positions, and therefore thought that the earth must be stationary

• Ptolemy, Aristotle and others refined the geocentric model

• But there were problems…….such as the path reversal by Mars Retrograde motion

Retrograde motion of Mars(path reversal seen in the Sky)

Epicycles – Ptolemic Geocentric Model

How do we know the Earth is spherical ?

• The ancient Greeks had deduced not only that the Earth is spherical but also measured its circumference !

• What kind of an object always has a round shadow ?

Earth Shadow during Lunar Eclipse

Multiple ExposurePhotograph

Alexandria

Cyrene

Tropic of CancerSyene

Syene

Alexandria

Earth

7º

Sunlight7 = Distance (Alexandria - Syene)-- ---------------------------------------360 Circumference of the Earth

Eratosthenes’s method to measure the circumference of the earth

Answer: 40,000 stadia= 25,000 mi !

At noon on summer solstice day theSun is directly overhead at Syene,but at an angle of 7o at Alexandria

Earth-Moon-Sun GeometryAristarchus’s determination of distances

(Closer the S-E-M angle to 90, the farther the Sun)

If we replace the moon with a planet, then can determine relative distances,as done by Copernicus

Copernicus

Copernican Model:Inferior and Superior Planets

(orbits inside or outside the Earth’s orbit)

InferiorConjunction

SuperiorConjunction

Earth

Configurations of Inferior Planets, Earth, and the Sun

ConjunctionOppositionEarth

Synodic (apparent) period – one conjunction to next (or one opposition to next)

Configurations of Superior Planets, Earth, and the Sun

Synodic and Sidereal Orbital Periods• Inferior planets are never at opposition;

superior planets can not be at inferior conjunction

• Copernican model of orbital periods• Synodic period is the apparent orbital

period of a planet, viewed from the earth, when the earth-planet-sun are in successive conjunction or opposition

• Sidereal (with respect to stars) period is the real orbital period around the Sun

• Synodic periods of outer planets (except Mars) are just over one year

Apparent (Synodic) and true (Sidereal – with respect to stars) orbital periods of

planets differ due to Earth’s relative motion

Synodic periods of all outer planets (except mars) are just over 1 year becausetheir Sidereal periods are very long and they are in opposition again soon afteran earth-year

Earth-Venus-Sun

Inferior planets appear farthest away from the Sun at ‘greatest elongation

Maximum Eastern Elongation

Maximum WesternElongation

Earth

Measurements of Distances to Planets

90 deg

P

S

E

Angle of maxelongation = P-E-S

Sin (P-E-S) = PS / ES ES = 1 AU

P-E-S

Copernicus first determined the relative distances of planets

Copernican Heliocentric Model:(Retrograde motion of Mars seen when

Earth overtakes Mars periodically)

Earth is closer to the Sun, therefore moves faster than Mars

Tycho: The most accurate pre-telescopic observer

Tycho charted very accurately the movement of Mars in the Sky, but still believed In the Geocentric Universe

Kepler – Tycho’s assistant(used Tycho’s data to derive Kepler’s Laws)

Planetary Orbits• The Copernican heliocentric model is essentially

correct• But it consisted of circular orbits which did not

exactly fit observations of planetary positions • Kepler realized, based on Tycho’s data of the

orbit of Mars, that orbits are elliptical Kepler’s First Law

• However, the difference for Mars is tiny, to within the accuracy of drawing a circle with a thick pen !

Kepler’s First Law:All planetary orbits are elliptical,

with the Sun at one focus

Eccentricity ‘e’:e = distance between foci/major axis

= AB / ab

A

B

a

b

A circle has e = 0, and a straight line has e = 1.0

Kepler’s Second Law:Planetary radius sweeps equal area

triangles in equal time

It follows that the velocity of the planet must vary according to distance from the Sun -- fastest at Perihelion and slowest at Aphelion

Kepler’s Third Law: P2 = a3

P – Orbital Period, a – semi-major axis

What is the size ‘a’ of the orbit of a comet with the period ‘P’ of 8 years?

Kepler’s Laws

• Empirically derived from observational data largely from Tycho (e.g. observations of the positions of Mars in its orbit around the Sun)

• Theoretical explanation had to await Newton’s discovery of the Law of Gravitation

• Universally valid for all gravitationally orbiting objects (e.g. stars around black holes before falling in)

Galileo

Galileo’s Discoveries With Telescope• Phases of Venus - Venus displays phases like the Moon as it revolves around the Sun

• Mountains and “seas” on the Moon - Other objects in the sky are like the Earth (not therefore special)

• Milky Way is made of stars like the Sun• Sunspots - “Imperfections” or “blemishes” in otherwise perfect “heavenly” objects

• 4 Galilean satellites of Jupiter - Objects in the sky revolve around other objects, not the Earth (i.e. other moons)

All of these supported the Copernican System

Galileo also conducted experiments on gravity :

Regardless of mass or weight objects fall at the same rate

Phases of Venus

Venus is never too far from the Sun, therefore can not be in opposition like the Moon. Changing phases of Venus demonstrate that it orbits the Sun like the Earth.

Orbits and Motions

• Orbits can not be circular since objects do NOT revolve around each other, but around their common center-of-mass

• The Earth and the Moon both revolve around each other

• This motion is in addition to Earth’s Rotation, Revolution, Precession

The Earth-Moon Barycenter• The earth and the moon both revolve

around a common center of mass called the Barycenter

• The barycenter of Sun-planet systems lies inside the Sun

• As the earth is much more massive, the barycenter lies 1700 Km inside the earth

• Calculate its position ‘O’ from

M(E) x EO = M (M) x MOE M

O

Gravity• Galileo’s observations on gravity led to

Newton’s Law of Gravitation and the three Laws of Motion

• Objects fall at the same rate regardless of mass because more massive objects have more inertia or resistance to motion

• Fgrav = G (m1 x m2) / r2

• Force of gravity between two masses is proportional to the product of masses divided by distance squared ‘inverse square law’