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Astronomy 130 > Chapter 5-The Nature of Light > Flashcards

Chapter 5-The Nature of Light Flashcards

1
Q

how are most observations of space collected

A

through electromagnetic waves “light”

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2
Q

what was light for many centuries

A

a mystery

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3
Q

2 things light is similar to

A

waves and particles

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4
Q

young’s double slit experiment

A

a screen with two slits was put in front of a light source and projected on to a wall to see what the light would be. it was a center point of light with other patches of light fanned out on its sides

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5
Q

photo electric effect

A
  • light shining on a piece of metal can cause electrons to be ejected from the surface
  • but it only happens if the light has a wavelength shorter than some value
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6
Q

as intensity of light increases what happens to the electrons

A

they increase but their energy does not

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7
Q

what is the equation for frequency

A

frequency equals speed of light (c) over wavelength of light (lambda)

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8
Q

frequency (f)

A

number of cycles per unit time

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9
Q

speed (c)

A

how fast something moves from one place to another

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10
Q

wavelength (lambda)

A

distance from peak to peak (or trough to trough)

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11
Q

low frequency =

A

long wavelength

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12
Q

high frequency=

A

short wavelength

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13
Q

energy

A

ability to do things

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14
Q

how do waves and energy connect

A

waves transport energy from one location to another

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15
Q

light

A

electromagnetic waves/ radiation

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16
Q

what is the quantization of light equation

A

energy = plank’s constant(h) x speed of light(c) over wavelength(lambda)

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17
Q

what equation did Einstein use to explain photoelectric effect

A

quantization of light

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18
Q

in the case of light, waves are carried by what

A

electromagnetic field

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19
Q

all light does what

A

travel in the speed of light in vaccume

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20
Q

what are kirthoffs 3 types of spectrum

A
  • continuous
  • emission
  • absorption
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21
Q

continuous line spectrum

A
  • a hot opaque body, such as a perfect blackbody or a hot dense gas produces this
  • the complete rainbow of colors without any spectral lines
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22
Q

emission line spectrum

A
  • a hot, transparent gas, produces this
  • a series of bright line against a dark background
  • ex: neon sign
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23
Q

absorption line spectrum

A
  • a cool, transparent, gas in front of a source of continuous spectrum produces this
  • a series of dark lines among the colors of a continuous spectrum
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24
Q

what type of spectra does a star produce

A

a continuous spectrum

25
Q

blackbody

A
  • EMITS radiation only according to its temperature
  • a perfect body does not exist
  • it absorbs all of the radiation that falls of it
  • does not reflect any light
26
Q

all electromagnetic wavelengths can be what

A
  • emitted from a blackbody
  • but same intensity at all wavelengths
  • peak wavelength depends on temperature
27
Q

a blackbody is pretty much what

A

a star

28
Q

wiens law

A
  1. 0029mK/T
    - lower temps have a higher wavelength
    - higher temps mean lower wavelength
29
Q

Stefan-Boltzmann law

A

-hotter objects emits more radiation at all wavelengths

Flux=(Constant)Temperature^4

30
Q

which types of stars are blue

A

hotter stars

31
Q

flux

A

energy per area per time

32
Q

what is the type of element determined by

A

the number of protons

33
Q

atomic number

A

number of protons in nucleus

34
Q

atomic mass number

A

number of protons and neutrons

35
Q

molecules

A

consist of two or more atoms

36
Q

what type of line spectra is the solar spectrum

A
  • absorption line spectrum

- this tells us that the sun has an atmosphere

37
Q

Bohr model of the atom

A

electrons can only occupy certain orbits

38
Q

what are spectral line caused by

A

when electrons transition between orbits

39
Q

what is an orbital

A

energy levels of an atom

40
Q

each orbital has what

A

an associated energy

41
Q

electron always wants to be where

A

in the ground state at n=1

42
Q

to get an electron form n=1 to n=2 you have to do what

A

add 10.2 Veto add more energy

43
Q

electron can “move up” by

A

absorbing a photon

44
Q

electron can “move down” by

A

emitting an electron

45
Q

we can use the Stefan boltzmanns law to determine what

A

the flux of energy at the suns surface

46
Q

blue-shifting

A

anytime a form of light moves towards the radio side of the spectrum (bottom)

47
Q

red-shifting

A

when light shifts up towards the gamma ray side of the spectrum (top)

48
Q

the light we see now has….

A

left its source sometime in the past

49
Q

the further out in space we look…

A

the further back into time we see

50
Q

knowing the flux and size of the star we can determine what

A

luminosity

51
Q

luminosity

A

blackbody spectrum+ stefan boltzmann+ size of the star

52
Q

if you know the radius and flux you can get the…

A

luminosity

53
Q

if you know the flux and luminosity you can get the…

A

radius

54
Q

power

A

energy per time

55
Q

doppler effect

A

parent shift in wavelength due to the relative motion of the source and/or the observer

56
Q

Doppler effect example

A

sirens of an ambulance are higher pitched as it goes towards you and lower pitched as it goes away

57
Q

when the siren goes away its

A

redshifted

58
Q

when the siren goes away its

A

blue shifted

59
Q

the further away the object is in space the more (what color shift is it)

A
  • redshift

- this proves that the universe is expanding

Astronomy 130 (10 decks)

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