students will be able to determine how distances between stars are measured. students will be able...

Students will be able to determine how distances between stars are measured.

Students will be able to distinguish between brightness and luminosity.

Students will be able to identify properties used to classify stars.

Star: A self-luminous celestial body consisting of a mass of gas held together by its own gravity.

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Main Idea: Stellar classification is based on measurement of light spectra, temperature, and composition.

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Constellations: Groups of stars.• There are 88 of them.• Circumpolar Constellations:

Visible in Northern Hemisphere all year.

• Summer, Fall, Winter, Spring: Only visible during certain seasons.

• Constellations are used by people to know when to prepare for planting, harvest, and ritual celebrations.

Circumpolar StarTrails

Hercules: Visible in NH only during summer

Orion: Visible in NH only during winter

Seasonal Constellations

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Star Clusters: Groups of stars that are gravitationally bound to each other.

2 kinds:1. Open Cluster: Not densely packed.2. Globular Cluster: Densely packed into

spherical shape.

Open Star Cluster Globular Star Cluster

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Binary Stars: Two stars that are gravitationally bound together and that orbit a common center mass.

• Hard to tell two stars apart.• One star often is much brighter than

the other.

Constellation in a cup

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Stellar Position and Distances: 2 Units used to measure long

distances:1. Light Year (ly): The distance that

light travels in 1 year = 9.461 x 10 km.

2. Parsec (pc): 3.26 ly.

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Distances in Light Years

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Parallax: Apparent shift in position of an object caused by the motion of the observer. • Used to calculate distance.• Earth’s orbit around the Sun means that

an observer’s position in space is always changing.

• Distance to a star can be estimated using the star’s parallax (angle of change.)

• Closer the star, the larger the shift.• Estimates are accurate up to 500 pc

away.

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4 Basic Properties of Stars: 1. Mass2. Diameter3. Luminosity4. Temperature – Estimated by

finding spectral type of star. Controls nuclear reaction rate and governs luminosity and magnitude.

H-R Diagram

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Magnitude: • Apparent Magnitude: How bright a

star appears. Brightest stars = +1 Next brightest = +2 A difference of 5 magnitudes = 100 x

more bright. Ex) +1 is 100 x more bright than +6.

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Magnitude: • Absolute Magnitude: Accounts for

distance (apparent does not.) How bright a star would appear if it were

10 pc away.

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Luminosity: Energy output from surface of star per second – a star’s power.• Requires that one know a star’s

apparent magnitude and distance away.

• Measure in watts – energy emitted per second. Sun’s luminosity = 3.85 x 10 w.

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Classification of Stars: Word of the Day:

• Spectral Line: An isolated bright or dark line in a spectrum produced by emission or absorption of light of a single wave length.

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Spectral Lines: Provide information about a star’s temperature and composition.

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Temperature: Corresponds to a star’s spectral lines.

Types: O Hot 50,000 K B A F G K M Cool 2,000 K Each type is subdivided into more

specific divisions by numbers 0 – 9.

Spectral Lines of Stars

Hotter Stars

Cooler Stars

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Composition: All stars have similar compositions.• Hot Stars: Less lines in spectra

(fewer kinds of gasses.)• Cool Stars: More lines in spectra

(more kinds of gasses.)

Typical Composition of Stars:• 73% hydrogen (H)• 25% helium (He)• 2% other elements.

Composition of Stars“Heavier Elements” = Anything heavier than Helium

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Hertzprung – Russell Diagram (H-R Diagram): • Shows the lifetimes of stars.• A graph on which absolute

magnitude is plotted on vertical axis and temperature or spectral type is plotted on horizontal axis.

Each class of star has a specific mass, luminosity, magnitude, temperature and diameter.

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H-R Diagram: Plots evolution of stars from one class to another.

Main Sequence: Area of the H-R Diagram in which most stars are located.• Runs diagonally from upper left

corner (Hot Bright Stars) to lower right corner (Cool Dim Stars.)

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Main Sequence: Contains 90% of stars including Sun (which is at the center because it has an average temperature and luminosity.)• Stars here fuse hydrogen.• As hydrogen runs out stars fuse

helium and begin to evolve off of the main sequence.

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Mass determines a star’s lifetime.• More Mass = More Pressure =

Shorter Lifetime• Higher mass stars burn hydrogen

faster.• Lower Mass = Less Pressure =

Longer Lifetime• Lower mass stars burn hydrogen

slowly.

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Red Giants and White Dwarfs: Red Giants: Top right of H-R

diagram = Cool, Bright Stars.• Because these stars are cool, but

still bright, they must have large surface areas.

• Mass is more than 100 x greater than the Sun.

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Red Giants and White Dwarfs: White Dwarfs: Lower left of H-R

diagram = Hot, Dim Stars.• Appear dim, though they are very

hot, must have small surface areas.• Size of Earth, but has a mass same

as the Sun.