Embed Size (px)
Citation preview
Formation of the Solar System
Modelling the Solar SystemGEOCENTRIC MODEL (EARTH-CENTERED MODEL)
Explains the daily motion of the planets constellations and stars (East West appearance and disappearance)
Lasted 14000 years Describe by Ptolemy in
ancient Greece
Could NOT explain retrograde motion
HELIOCENTRIC MODEL
Described by Nicolaus Copernicus and supported by Galileo
Based on observation of the Galilean moons revolving around Jupiter and observations of Venusrsquo phases (like the Moon)
Could explain retrograde motion
Retrograde Motion
Steps in forming a star system1 Interstellar dust clouds (nebula)
Where does interstellar dust come from
2 Made primarily of H and He3 Low density -gt High density4 Spinning and accelerated rotation (centripetal
force)5 Once conditions (temperature and pressure)cause
H to fuse into He a star is born6 Spinning causes heavierhigh melting point
materials to stay close to the center and lighterlow melting point materials to be further from the center (OR DO THEY)
Keplerrsquos First Law Planets orbit in an elliptical shape
Keplerrsquos First Law Earthrsquos semi major axis is ~150 000 000 km (Astronomical Unit AU)
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Modelling the Solar SystemGEOCENTRIC MODEL (EARTH-CENTERED MODEL)
Explains the daily motion of the planets constellations and stars (East West appearance and disappearance)
Lasted 14000 years Describe by Ptolemy in
ancient Greece
Could NOT explain retrograde motion
HELIOCENTRIC MODEL
Described by Nicolaus Copernicus and supported by Galileo
Based on observation of the Galilean moons revolving around Jupiter and observations of Venusrsquo phases (like the Moon)
Could explain retrograde motion
Retrograde Motion
Steps in forming a star system1 Interstellar dust clouds (nebula)
Where does interstellar dust come from
2 Made primarily of H and He3 Low density -gt High density4 Spinning and accelerated rotation (centripetal
force)5 Once conditions (temperature and pressure)cause
H to fuse into He a star is born6 Spinning causes heavierhigh melting point
materials to stay close to the center and lighterlow melting point materials to be further from the center (OR DO THEY)
Keplerrsquos First Law Planets orbit in an elliptical shape
Keplerrsquos First Law Earthrsquos semi major axis is ~150 000 000 km (Astronomical Unit AU)
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Retrograde Motion
Steps in forming a star system1 Interstellar dust clouds (nebula)
Where does interstellar dust come from
2 Made primarily of H and He3 Low density -gt High density4 Spinning and accelerated rotation (centripetal
force)5 Once conditions (temperature and pressure)cause
H to fuse into He a star is born6 Spinning causes heavierhigh melting point
materials to stay close to the center and lighterlow melting point materials to be further from the center (OR DO THEY)
Keplerrsquos First Law Planets orbit in an elliptical shape
Keplerrsquos First Law Earthrsquos semi major axis is ~150 000 000 km (Astronomical Unit AU)
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Steps in forming a star system1 Interstellar dust clouds (nebula)
Where does interstellar dust come from
2 Made primarily of H and He3 Low density -gt High density4 Spinning and accelerated rotation (centripetal
force)5 Once conditions (temperature and pressure)cause
H to fuse into He a star is born6 Spinning causes heavierhigh melting point
materials to stay close to the center and lighterlow melting point materials to be further from the center (OR DO THEY)
Keplerrsquos First Law Planets orbit in an elliptical shape
Keplerrsquos First Law Earthrsquos semi major axis is ~150 000 000 km (Astronomical Unit AU)
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Keplerrsquos First Law Planets orbit in an elliptical shape
Keplerrsquos First Law Earthrsquos semi major axis is ~150 000 000 km (Astronomical Unit AU)
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Keplerrsquos First Law Earthrsquos semi major axis is ~150 000 000 km (Astronomical Unit AU)
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Keplerrsquos Second Law Planets move faster when they are closer to the Sun
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Keplerrsquos Third Law
P2 = a3 Where P = Earth years and a =
length of semi-major axis in AU Describes the relationship between
the size of a planetrsquos ellipse and its orbital period (year length)
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Gravity
Newton mathematically described gravity as an attractive force between 2 objects that depends on mass and separation
F = Gm1m2
r2
Where F is force (newtons) G is the universal gravitational constant
(66726 x 10-11 m3 kgs2) m1 and m2 are measured in kg r is the distance between the bodies in
meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
Circular Motion
v2 = Gm r
where v is velocity (ms) G is the gravitational constant m is the mass in kg r is the distance between the two bodies
in meters
