h.a.l. astronomy school
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H.A.L. Astronomy School. Star Stuff:. Or, Interesting Stuff to Know and Tell about Stars. 1930 hours EDT. 2030 hours EDT. 2130 hours EDT. - PowerPoint PPT PresentationTRANSCRIPT
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H.A.L. Astronomy School
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Star Stuff:Or, Interesting Stuff to Know
and Tell about Stars
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1930 hours EDT
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2030 hours EDT
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2130 hours EDT
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Kochab
Proper Names Kochab KocabBayer Designation Beta Ursae MinorisFlamsteed Number 7 Ursae MinorisBSC 5563HD 131873Constellation Ursa MinorRight Ascension 14h 50m 42sDeclination +74° 9' 20“Distance 127 light years 39 parsecsMagnitude Apparent: +2.2 Absolute: -0.8 to -0.7Spectral Class K4 Orange GiantOptimum Visibility April/May Usually visible from northern latitudes
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How’s the “seeing”? Using Certain Stars to Determine Limiting Magnitude
The 2,3,4, and 5 System:
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An Illusion of Permanence: At a Casual Glance
Heavens seem eternal and unchanging
Sky we see at night is virtually indistinguishable from the sky seen by our ancestors
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Empirical Reality, 1 of 3 Stars are born even NOW from
interstellar gas and dust, in cold clouds that are scattered abundantly throughout our galaxy
Perhaps an interstellar cloud encounters one of the galaxy’s spiral arms…
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Empirical Reality, 2 of 3 …or perhaps a supernova detonates
nearby From the shock of events like these,
the cloud begins to contract under the pull of gravity, forming protostars – the fragments that will one day become stars
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Empirical Reality, 3 of 3 As protostar develops, its internal
pressure builds and its temperature rises
In time, hydrogen burning can ignite, and a star is born
Clusters of these young stars illuminate the interstellar gas and dust that surround them, producing beautiful glowing nebulae
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Starbirth, starlife, stardeath Stars are born, they mature and they
grow old Major stages in their lives can last for
millions or even billions of years Some even blow themselves apart in
death throes that enrich interstellar space with the material for future generations of stars
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Stars Seem Unchanging to Our Eyes
But only because of the colossal time scale over which
they change
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150 ly (45 parsecs)
Distance: 23,000 ly (7,000 parsecs)
The average density of stars in M13 is about 100 times greater than in the neighborhood of the Sun.
Stellar census of a few hundred thousand stars
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Stellar Astrophysics:The Very Short Course
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Mass Matters, 1 of 4 The most massive stars are the most
luminous, while the least massive stars are the least luminous
Observation and theory show that there is a lower and an upper mass limit for stars
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Mass Matters, 2 of 4 A protostar less massive than 0.08
solar masses can never develop the necessary pressure and temperature to start hydrogen “burning” at its core
Theory indicates this failed star contracts to become a hydrogen-rich object called a brown dwarf
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Brown Dwarfs Brown dwarfs are intermediate in
their properties between stars and Jovian planets (such as Jupiter with a mass of 0.001 solar masses)
Jupiter is NOT a failed star Observational confirmation of brown
dwarfs did not come until 1994 (Gliese 229)
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Mass Matters, 3 of 4 Protostars with masses greater than
about 100 solar masses also do not become main-sequence stars
They rapidly become very luminous with pressure so great that it overwhelms the effects of gravity, expelling the outer layers into space and disrupting the star
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Mass Matters, 4 of 4 The range for main-sequence stars is
between 0.08 and 100 solar masses High-mass stars are extremely rare Therefore, stars can range from
8/100 the mass of our Sun to 100 times the mass of our Sun
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Star Color = Star TemperatureO
B
A
F
G
K
M
Sun
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"We are made of star stuff. We are a way that the cosmos can know itself." -----Carl Sagan in the opening sequence of Cosmos