star light, star bright. 3 factors that determine the brightness of a star temperature hotter the...
TRANSCRIPT
Star Light, Star Bright
3 Factors that determine the brightness of a star
Temperature
Hotter the star the brighter the star
Blue…..white……..yellow…….orange…….….red
HOTTEST----------------------------------------------COOLEST
Size
• Larger the star Brighter the Star
• Smaller the star Dimmer the Star
Distance
• Closer the star Brighter the star
• Further the star Dimmer the star
Brightness Key Terms
• Luminosity– How much light energy is coming from the surface
• Apparent Magnitude– How bright it appears to be due to distance
• Absolute Magnitude– How bright it is if its distance was a parsec or 33 light years
• Parallax– The shift of closer stars against a background of farther stars as
the Earth goes around the Sun
Luminosity
• Definition- actual or true brightness of a star
• Total amount of energy given off
• Dependent on 2 things:Temperature
6000K 10,000K
More luminous since more surface area
Size
6000K6000K
More luminous since more energy
Apparent Magnitude• Definition- how bright a star appears when seen from
earth
• System developed where a number is assigned to a star based on brightness– Scale is basically based on powers of 10 difference– A +2 is 10 times as bright as a 3, +100 times as bright as a +4
• Smaller # Brighter the star Bigger # Dimmer the star
• Sun -28 , Full Moon -11, Polaris 7• Hubble can see +28
Absolute Magnitude• Definition- brightness of a star as if all
stars were seen from the same distance
Earth Earth
Sun- average star, Abs. Mag of +4.8 (less luminous, looks brighter because closer)
Rigel- orion, Abs, Mag. of -6.4 (more luminous, further away)
To Determine: apparent magnitude and distance to earth
Moving Stars?
• Parallax- the apparent change in position of a star due to the movement of observer
Finger: left/right
Life Cycle of a Star
Nebula ProtostarMain
Sequence
Star
Red giant
Red supergiant
Planetary
Nebula
White
Dwarf
Supernova Black Hole
Neutron Star
Life Cycle of Stars
1
2
Life Cycle Introduction
• http://www.youtube.com/watch?v=f_KLOFe2rDY
• http://www.youtube.com/watch?v=YU6X3SPZAJo
Step 1: Initiation
• Stars are born in nebulae (huge clouds of gas and dust)
• Nebula begin to condense when an outside force, such as shock wave, acts upon it
Step 2: Pre-star
• A protostar forms when a part of the nebula contracts, shrinks, and pressure and internal temperature increases
• Protostar begins to glow where nebula is contracting
Step 2 contd: A star is born
• As contraction, temperature, density, and pressure increase protostar gets larger and brighter
• Center becomes so hot fusion begins
• Once fusion begins, a star is born
• TRUE STAR
Step 3: Teenager star• Internal temperature hot
enough to start fusion at center said to be a main sequence star
• Sun is an example• Each protostar will turn
into one main sequence star
• 90% of stars are main sequence stars
• Vary in surface temperature and absolute magnitude
Fate determined by Size
• If a normal size star (Sun) follows path 1
• If star is a GIANT follows path 2
Path 1
Step 4: Middle-aged star
• Red giant- very bright, once an average star, but is now close to end of life
- Has expanded to many times its original size (heat causes it to expand)
- Hydrogen core has turned to helium and eventually to carbon
- Our sun will become a red giant star in about 5 billion years
Star like our sun begins to die
• Star begins to die when its core temperature rises to a point where fuel is used up
• A carbon-oxygen core forms • Eventually the gases at a
star’s surface begin to blow away in abrupt bursts
• Resulting glowing halo is called a planetary nebula
Death of a star like our sun
• atoms no longer fuse, fuel is used up
- Outer gases escape leaving the core which collapses and shrinks
- Heat still present but will continue to escape for about a billion of years
- White Dwarf- small, very dense, hot star at the end of its life, mostly carbon with nuclear cores depleted (about the size of earth but heavier)
Path 2
Step 4: Middle-aged massive star• Supergiant- largest
known type of star- can be as large as our
solar system- rare but exists- In a massive star,
hydrogen is fused more quickly and fusion continues until a iron nuclei is formed
Death of a Supergiant
• Elements are used up very quickly and eventually runs out of fuel
• Collapse of the core produces a shock wave that blasts the star’s outer layers into space producing a supernova
• Supernova- exploding star
Option A after a supernova
• After a massive star “goes supernova” it leaves behind its core (called a neutron star)
-Neutron Star- small, dense star made of neutrons
• When neutron star is first formed, it spins very rapidly and gives off radio waves
Option B after a supernova
• Black Hole- a star that collapses
• How do we know they exist? Pulls gases off nearby stars, as gas is pulled into this “nothing space” x-rays are emitted from the gas as molecules are pulled in
Cycle continues
• Star is born from great clouds of gas and dust
• Stars mature, grow old, and die
• As a star dies, it makes new clouds of dust gas and dust where new stars can begin to form
• More massive a star, the shorter its life
• http://www.youtube.com/watch?v=HfqcZdNnQ6s
• http://www.youtube.com/watch?v=hoLvOvGW3Tk&feature=related
Hertzsprung-Russell Diagram
• Graph that compares temperature and absolute magnitude (brightness)
The Hertzsprung-Russell Diagram (H-R diagram)
Cool and bright
Cool and dim
Hot and dim
Hot and bright
Sun
CoolHot
Dim
Bright
Cool and dim
Cool and bright
Hot and dim
Hot and bright
Main sequence
Giants
Supergiants
White Dwarfs