motions of the planets days of the week: (“ … · 2016-08-06 · mercury, venus, mars, jupiter,...
TRANSCRIPT
Motions of the Planets (“Wanderers”)
Planets move on celestial sphere - change RA, Dec each night - five are visible to naked eye
Mercury, Venus, Mars, Jupiter, Saturn
www.universetoday.com
Days of the week:
- named after 7 “Power” (moving) objects in the sky (Sun, Moon, 5 planets)
English Spanish French Roman/Latin Origin
Germanic/ Norse Origin
SundaySundaySundaySunday
Domingo Dimanche Sun Sun
MondayMondayMondayMonday
Lunes Lundi Luna (Moon) Moon
TuesdayTuesdayTuesdayTuesday
Martes Mardi Mars Tyr
WednesdayWednesdayWednesdayWednesday
Miercoles Mercredi Mercury Wodan
ThursdayThursdayThursdayThursday Jueves Jeudi Jupiter (Jove) Thor
FridayFridayFridayFriday
Viernes Vendredi Venus Frigg
SaturdaySaturdaySaturdaySaturday
Sabado Samedi Saturn Saturn
Motion of the planets: - move near ecliptic (through zodiac)
- most of the time, move eastward
→ “Prograde Motion”
- occasionally: change direction and move westward
→ “Retrograde Motion”
http://alpha.lasalle.edu/~smithsc/Astronomy/retrograd.html
Models of the Universe: Aristotle: philosophy of “Idealism”
(∼ 2000 years ago)
- circles and spheres are ideal shapes
→ structure of universe based on circles and spheres
Geocentric Cosmology
- Earth is at center, stationary
- Sun, Moon, 5 known planets
→ revolve around Earth on concentric circles
- Earth at center of rotating Celestial Sphere
Claudius Ptolemy (137 A.D.)
- most accurate model of planetary motion at the time
→ based on Geocentric Cosmology
Ptolemaic Model
- “orbit” of planet around Earth - Deferent
- planets are fixed to smaller circles - Epicycles
� Planets revolve on epicycles while epicycles revolve on deferent
Link:
http://astro.unl.edu/classaction/animations/renaissance/marsorbit.html
http://www.polaris.iastate.edu/EveningStar/Unit2/unit2_sub1.htm
Ptolemaic System
- used for over 1300 years - over time, needed adjustments
Eventually, model had 234 epicycles to describe the motion of 5 planets!! Orbit of Mercury
Nicholas Copernicus (1473 - 1543)
- developed an accurate Sun centered (“Heliocentric”) model
Heliocentric Cosmology
- Earth is a planet, orbiting around the sun - other planets on larger or smaller orbits
explains retrograde motion in simple way:
- Earth passes by outer planets
- gives appearance that other planets change direction
http://mars.jpl.nasa.gov/allaboutmars/nightsky/nightsky04/ http://astro.unl.edu/naap/ssm/animations/configurationsSimulator.html
Copernicus
- used simple geometry to find distances to planets
- close to modern values!
- but, still used circular orbits - not entirely accurate
Tycho Brahe (1546 - 1601) “Greatest Observational Genius of the Age”
- very accurate & precise observations before telescope
- accuracy of 0.1o (or 6')
- near limit of human eye
- measured positions of planets
Johannes Kepler (1571 - 1630) “Greatest Theoretician of the Age”
- assistant to Tycho Brahe
- used data to describe planetary orbits (after Tycho’s death)
- tried to find correct geometrical shape: - found that orbits are Ellipses!!
Kepler’s First Law:
Orbits of planets: - are ellipses - with the sun at one focus
Properties of an Ellipse:
b
a
focus focus
a - semimajor axis b - semiminor axis
Eccentricity: - measure of how round/flat the ellipse is - ranges from 0 (circle) to 1.0 (flat line)
Kepler’s Second Law:
Kepler studied motion of a planet: the speed of the planet changes
- planets move faster when closer to sun (closest point: Perihelion)
- planets move slower when farther from sun (furthest point: Aphelion)
A line joining a planet and the sun: - sweeps out equal areas in equal times
Kepler’s Third Law:
When Kepler studied other planets, found: - a planet with a larger orbit
- takes longer to orbit the sun and moves slower!
The squares of the periods are proportional to the cubes of the semimajor axes
Definition: For Earth’s orbit Semimajor axis = 1 Astronomical Unit
For any planet, P2 = a3
Mercury: P = 0.241 yrs a = 0.387 A.U.
P2 = 0.058 yrs2 a3 = 0.058 A.U.3
Jupiter: P = 11.86 yrs a = 5.20 A.U.
P2 = 140.6 yrs2 a3 = 140.6 A.U.3
Example: An object that orbits 4 A.U. from Sun
a = 4 AU: a3 = 43 = 64
P = √a3 = √64 = 8 yrs Object will take 8 years8 years8 years8 years to orbit Sun
Galileo Galilei (1564 - 1642) - first person to use telescope to study sky
Astronomical Observations: Surface of the Moon - normal geological features like mountains, craters, valleys
→ similar to Earth
Surface of the Sun - saw spots on surface (“blemishes!”)
→ could measure rotation
Moons of Jupiter - four moons in orbit around Jupiter - obeyed Kepler’s Laws - Earth not only “center of revolution”
Venus - goes through same phases as Moon - becomes larger when dimmer,
smaller when brighter
Previous Observations -Mercury, Venus always close to sun
Geocentric (Earth-centered) Model:
- their orbits around the Earth must be linked to sun
Heliocentric Model: - their orbits are smaller than Earth,
cannot move far away from sun
http://astro.unl.edu/classaction/renaissance.html
If Venus has all the phases of Moon:
→→→→ Venus Venus Venus Venus mustmustmustmust orbit sun!orbit sun!orbit sun!orbit sun!
Observations cannotcannotcannotcannot be explained by Geocentric Cosmology!
Isaac Newton (1642 - 1727) - described what causes motion
→ FORCE - a “force” is a push or a pull
Newton’s Three Laws of Motion:Newton’s Three Laws of Motion:Newton’s Three Laws of Motion:Newton’s Three Laws of Motion:
First Law (Law of Inertia)First Law (Law of Inertia)First Law (Law of Inertia)First Law (Law of Inertia)
if no net force, an object: - will be at rest - or moves at a constant speed, in straight line, forever Second LawSecond LawSecond LawSecond Law (F = ma)F = ma)F = ma)F = ma)
If a net force acts on an object: - it changes its motion (accelerates)
- speeds up, slows down, or turns - depends on mass of object - more mass, harder to accelerate
Third Law (“Third Law (“Third Law (“Third Law (“actionactionactionaction----reaction”reaction”reaction”reaction”)))) If two objects apply forces on each other:
- the forces are exactly the same strength, but opposite in direction
Planets move on elliptical orbits - change direction, speed
� due to force on planets! Newton: Universal Law of Gravity
FG = G m1 m2
r2
G - gravitational constant = 6.67 x 10-11 m3/kg s2
- proportional to masses (m1, m2) - inversely proportional to square of distance (r)