Astronomy Test 2

Front 1

Light as a wave

Back 1

Electric and magnetic fields that travel=Electromagnetic wave

Front 2

What EM waves can human eyes detect?

Back 2

400nm-700nm

Front 3

Light as a particle (photon)

Back 3

Photon energy is proportional to 1/wavelenth

Front 4

Longer wavelength equals...

Back 4

less energy

Front 5

The electromagnetic spectrum

Back 5

Gamma ray, xray, ultraviolet, visible, infared, microwave, radio

Front 6

Two atmospheric windows

Back 6

visible, radio

Front 7

Telescopic Functions

Back 7

Light gathering Power
Resolving Power
Magnifying power

Front 8

Issac Newton

Back 8

Cut a slit in a curtain and passed the light through a prism for the colors

Front 9

Fraunhofer

Back 9

Passed light through curtain onto a diffraction grating and found dark lines. Labeled them.

Front 10

Bunsen and Kirchoff

Back 10

Passed light through heated chemicals and found bright lines. Discovered sodium on the sun

Front 11

Kirchoff's 1st Law

Back 11

If light passes through a hot, hig density solid, liquid, or gas, you get a continuous spectrum

Front 12

Kirchoff's 2nd Law

Back 12

Hot, low density gas gives off a bright line spectrum

Front 13

Kirchoff's 3rd Law

Back 13

Source of continous spectrum light passes through a cooler, low density gas creating a dark line spectrum

Front 14

Bohr

Back 14

Spectral lines are due to atomic electrons changing energy levels

Front 15

Photons are Absorbed

Back 15

dark line spectrum

Front 16

Photons are Emitted

Back 16

Bright Line Spectrum

Front 17

Balmer Series

Back 17

Electrons jumping up or down from energy level 2

Front 18

Parallax

Back 18

apparent change in an objects position due to a change in the observers location

Front 19

Parallax Method

Back 19

distance in parsecs=1/parallax angle in arc seconds

Front 20

Parallex Measurements Largest to smallest

Back 20

0.77 arc sec-0.002 arc sec

Front 21

Apparent Magnitude

Back 21

how bright a star appears to be (negative is brighter)

Front 22

Absolute Magnitude

Back 22

measure of the light output of a star

Front 23

When does (m) = (M)?

Back 23

When the distance is 10pc

Front 24

Range of M for stars

Back 24

-10 to +20

Front 25

Luminosity

Back 25

measure of the light output of a star

Front 26

Rangle of L for stars

Back 26

10 to the power of 6-10 to the power of -6

Front 27

Proper Motion

Back 27

motion perpendicular to the line of sight-moving side to side

Front 28

Radial motion

Back 28

motion along the line of sight-moving toward or away

Front 29

Doppler Effect-Moving towards

Back 29

Blue

Front 30

Moving away

Back 30

Red

Front 31

Black Body

Back 31

hot solid, liquid, or a hot, high density gas

Front 32

Black Body Radiation

Back 32

light emitted by a hot object

Front 33

Wien's Law

Back 33

temperature is proportional to 1/wavelength max

Front 34

What is Wien's law saying?

Back 34

cool stars are red, hot stars are blue

Front 35

Stefan Boltzmann Law

Back 35

L is proportional to radius squared * temperature to the fourth power

Front 36

Are stars black bodies?

Back 36

Almost, they have valleys in the dark line

Front 37

What type of spectra does a star give off?

Back 37

A dark line

Front 38

What can we find from a stars spectrum?

Back 38

Chemical Composition
Radial Motion
Surface Temperature

Front 39

Chemical composition

Back 39

by line patterns

Front 40

Radial Motion

Back 40

Shift in line patterns

Front 41

Surface Temperature

Back 41

strength of spectral lines

Front 42

Stellar Spectral Types

Back 42

OBAFGKM

Front 43

Hertzsprung-Russell Diagram

Back 43

M vs. Spectral Type

Front 44

Stellar Size

Back 44

Stefan Boltzmann law-range from 0.01R Sun-1000R Sun

Front 45

Stellar Mass

Back 45

mass a/mass b=distance b/distance a

Front 46

Newton's form of Kepler's 3rd Law

Back 46

mass a + mass b= a AU cubed/P years squared

Front 47

Range of masses

Back 47

0.08 solar masses-100 solar masses

Front 48

Stellar density range

Back 48

10 to the -6g/cm cubed-10 to the 7 g/cm cubed

Front 49

Innerstellar Medium Composition

Back 49

3/4 hydrogen, 1/4 helium, 2% heavier elements

Front 50

ISM Density

Back 50

1 atom/cm cubed

Front 51

Giant Molecular Clouds density, size, and temperature

Back 51

100 atoms/cm cubed
big
cold

Front 52

Hydrostatic Equilibrium

Back 52

balance between inward gravity and outward energy released from fusion

Front 53

How do stars form

Back 53

Shockwave goes through giant moecular cloud creating dense cores. Gravity starts to collapse these dense cores. A protostar (nucleus) forms in the dense core. Protostar gives off heat and creates energy. Hydrostatic Equilibrium occurs.