HRDiagram What is it Stands for the Hertzsprung Russell Diagram Graphs surface temperature color vs Absolute Brightness Luminosity Horizontal Axis Surface TempColor Vertical Axis Absolute Brightness ID: 783184
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Slide1
THE HR DIAGRAM
The Life Cycles of Stars
Slide2HR-Diagram- What is it?
Stands for the
Hertzsprung
-Russell Diagram
Graphs surface temperature (color) vs. Absolute Brightness (Luminosity)
Horizontal Axis- Surface Temp/Color
Vertical Axis- Absolute Brightness
Mass can also be determined when Stars are placed on the HR Diagram- the higher the star is on the diagram the larger the mass. We use our Sun as a base number of a mass of 1 and stars above the Sun on the Diagram are larger than 1 and the stars below the graph are less than 1.
Slide3Main Sequence stars
This is the diagonal band of stars that start with the bright hot stars in the upper left and the cool, dim stars in the lower right corner
90% of the stars in the universe lie on the main sequence
The sun is located in the middle
Slide4Giants VS. Dwarfs
The HR diagram can estimate size and mass of the star
If you compare two stars of the same temperature the brighter star must be larger
If you compare two stars of the mass/size the hotter stars are brighter than the cooler stars.
http://aspire.cosmic-ray.org/labs/star_life/hr_interactive.html
Slide5Super Giants And White Dwarfs
Much Brighter than the main Sequence stars of the same temp
This means that they are very large and can range in size from 100-1000 times the size of the sun
GIANTS
- large bright stars a bit smaller and fainter than Super giants
Super giants
in the Red temp range tend to be in their last stages of life. They are out of hydrogen and are now fusing Helium into Carbon.
White Dwarfs-
are the small, dense remains of low or medium mass stars.
They are very hot, but dimmer then the main sequence stars of the same temperature.
They are no longer producing energy or light, they are lit because of the remaining energy from the collapse of the original star. They will eventually cool to a black dwarf.
Slide6BIRTH and Formation
Most stars fall on the main sequence
Close to 9% are White Dwarfs
Less than 1% are Giants or Super giants
FORMATION
- Space contains gas and dust and stars are formed in nurseries called
Nebulas
or a contracting cloud of dust and gas
Some Nebulas glow while others are dark
Stars are created from Gravity pulling the nebula together and making a dense ball of gas
PROTOSTAR
- enough gas and dust to form a star is available, but it is not an actual star until it gets hot enough to start nuclear (hydrogen) fusion
Slide7Adult star
When a star is on the main sequence it is considered an adult star. It will spend approx. 90% of its life span on as an adult star on the main sequence.
This begins the moment Hydrogen fusion begins
The more massive the star, the more nuclear fusion takes place to produce energy
The mass of the star determines the place it lies on the main sequence.
High mass stars are the bluest and brightest on the upper left of the main sequence (30 +times the mass of the sun and 300,000 times brighter)
Low Mass stars are the red and dim, on the lower right of the main sequence.
Larger stars die quicker than smaller stars because it uses its fuel quicker
Large- live a few million years
Medium- 10 billion (like our Sun)
Small- 100 billion or more
Slide8DEATH
At some point the star runs out of fuel. Now remember the star is stable because of its balance between inward and outward forces.
The outward force- Thermal Pressure
The inward force- Gravity
The star now begins to lose thermal
pressure and gravity squeezes the core
which starts hydrogen fusion in the shell of the star. This
causes the outer layers of the star to expand.
The star cools down and turns red
The core continues to shrink causing helium fusion. For a moment ( few million years) the star stabilizes in the red giant region of the HR diagram.
Slide9Death of a LOW or MEDIUM mass star
As the Helium supplies dwindle, the outward pressure is not enough to balance the inward pressure of gravity
The star collapses
The hot core remains with all of the gas around it. We call this a Planetary Nebula
Eventually the gas surrounding the core blows off and we are left with a hot core called a
White Dwarf
This will cool off after 20 billion years leaving a cold core called a
Black dwarf
Slide10High Mass Star- more than 8x the Sun
The star runs out of energy and turns into a
Red Super Giant
the same way a low mass star does.
The Star Collapses
This time there is so much energy because of the large mass of the outer star that the collapse causes a Super Nova Explosion.
NOW…if the CORE of the star has a mass of
3x or less
the size of the sun ( but has a much smaller diameter than the sun) it creates a
Neutron Star
which spins and emits a steady beam of radiation and light out of its poles.
*Neutron stars are so Dense that a teaspoon of a neutron star on EARTH would weigh a billion tons.
*
If the neutron star is spinning it will appear to pulse giving it the name PULSAR
FINALLY…if the CORE of the star is
more than 3x
the mass of the Sun ( and still a much smaller diameter than the Sun) the star collapses with so much energy and as the star get smaller, the gravity gets much larger. In Fact it is too large even for light to escape the gravity. This is a BLACK HOLE!