Astronomy Test Iii

Front 1

Asteroids

Back 1

Mars and Jupiter-belt—rocks

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Trojan

Back 2

Jupiter's family of asteroids

Front 3

Earth Crossers

Back 3

Apollo class can hit NEO—near earth objects

Front 4

Oort Cloud

Back 4

spherical cloud surrounding solar system, made opf comet dust, 50,000AU

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Kuiper's Belt

Back 5

outside Neptune –made up of leftover planetismals

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meteoroid

Back 6

small piece in space that create meteors

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meteor

Back 7

light from burning up in our atmosphere

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meteorite

Back 8

rock from space on the ground

Front 9

photosphere

Back 9

part of sun we see about 500 miles thick-5800K

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chromo sphere

Back 10

pink –10,000miles above photosphere—15000K

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corona and holes

Back 11

outer atmosphere and 1,000,000K+--areas which have no corona are called holes.

Front 12

luminosity

Back 12

how much energy (an object) or the sun gives off—we use sun as standard unit of 1 solar lum

Front 13

convection zone

Back 13

area just below the stars surface that energy moves outward and undulates sun surface

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radiation zone

Back 14

area around core of sun that moves the energy

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core

Back 15

15,000,000K, dense and all fusion takes place here

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helio seismology

Back 16

study of convection undulations below surface

Front 17

granulation

Back 17

salt and pepper texture on surface due to convection

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sunspots

Back 18

magnetic storms cooler by 2000K on suns surface

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sunspot cycle

Back 19

11 years if you look at numbers and 22 years if you look at total polarity switch

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prominences

Back 20

loops of gasses that connect paired sunspots

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flares

Back 21

hot storms that last 5 to 20 minutes 5million degrees sends out a lot of x-rays and solar radiation

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fusion

Back 22

combining hydrogen into helium which releases energy (only in core)

Front 23

p-p reaction

Back 23

reaction that takes place in suns core—4 hydrogen to 1 helium

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E=mc2

Back 24

E energy m=mass c = speed of light

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Neutrinos

Back 25

essentially mass-less particles that are created at suns core and may let us study the core

Front 26

Parsec

Back 26

distance to an object with parallax of one arc sec—3.26 light years

Front 27

Proper Motion

Back 27

amount stars moves across the sky—most are to far away to see proper motion

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apparent brightness

Back 28

brightness of star in night sky

Front 29

Magnitude scale

Back 29

each magnitude number changes by 2.5 times up or down

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Absolute magnitude

Back 30

how bright star would appear at 10 parsecs

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mass luminosity

Back 31

the more massive the star the brighter it is.

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radius luminosity

Back 32

temperature relationship—to truly to know the brightness of star you need to know size and temp

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visual binaries

Back 33

a star that can be seen as two stars and used to get masses

Front 34

spectroscopic binaries

Back 34

cannot see the companions but spectrum lines tells them they are there

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spectroscopic parallax

Back 35

uses HR diagram to measure distance to stars

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eclipsing binaries

Back 36

two stars that block each others light --easy to measure masses of stars

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luminosity classes

Back 37

I Supergiants
II Bright Giants
III Giants
IV Subgiants
V Dwarfs (=Main Sequence Stars)
VI Subdwarfs
VII White Dwarfs

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globular cluster

Back 38

spherical, found in halos of galaxies and contain old stars

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galactic cluster

Back 39

collection of galaxies held together by gravity

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main sequence turnoff point

Back 40

star leaves main sequence as it get old

Front 41

moleculoar clouds

Back 41

large cool gas cloud that have many materials and dust-star formation

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protostar

Back 42

forming star

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jets

Back 43

gasses ejected as star forms

Front 44

thermal vs degenerate pressure

Back 44

thermal –out—degenerate stops and collapses inward

Front 45

brown dwarfs

Back 45

failed stars

Front 46

hydrogen shell burning

Back 46

older star having fusion moved out from core

Front 47

helium flash

Back 47

low mass star trying helium fuel

Front 48

white dwarf star

Back 48

sun dies as core called white dwarf surrounded by planetary nebula

Front 49

planetary nebula

Back 49

glowing cloud of gas ejected from a low mass star at the end of its life.

Front 50

CNO cycle

Back 50

more massive stars than sun use this to fuse hydrogen into helium.

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Iron stage

Back 51

last fuel most massive stars can use

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supernova

Back 52

huge explosion--type 1 binary star death type II one large star explosion

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nuetron star

Back 53

1.4 to 6 solar mass---10 mile collapsed core of neutrons. Corpse of a high mass star supernova

Front 54

electron degeneracy

Back 54

that which stops white dwarf from collapsing any further

Front 55

white dwarf size

Back 55

.1 to 1.4 solar masses—sun ends up this way 10000 miles across—earth size

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white dwarf limit

Back 56

maximum size .1to 1.4

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accretion disk

Back 57

rapidly rotating disk that falls inward as it orbits a starlike object (i.e white dwarf)

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nova

Back 58

the dramatic brightening of a star that lasts for a few weeks and then subsides.

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white dwarf supernova

Back 59

supernova that occurs whan a white drawf reaches it’s the white drawf limit and explodes like a bomb—type 1a

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massive star supernova explosion

Back 60

type II one large star explosion

Front 61

nuetron stars

Back 61

1.4 to 6 solar mass---10 mile collapsed core of neutrons

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nuetron degeneracy

Back 62

stops further collapse

Front 63

pulsars

Back 63

rotating neutron star

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black hole

Back 64

bottomless pit, light cannot escape—6 solar masses and above

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schwarz child radius

Back 65

the size of a black holes event horizon

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event horizon

Back 66

once you cross you cannot return, of a black hole

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singularity

Back 67

place in a black hole where gravity crushes matter

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gamma ray bursts

Back 68

matter falling in to black holes giving large explosions of gammas

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Blue

Back 69

28,000 - 50,000

Front 70

Blue White

Back 70

10,000-28,000

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White

Back 71

7,500 - 10,000

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White Yellow

Back 72

6,000 - 7,500

Front 73

Yellow

Back 73

4,900 - 6,000

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Orange

Back 74

3,500 - 4,900

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Red

Back 75

2,000 - 3,500