Chapter 5-The Nature of Light Flashcards

(59 cards)

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
blackbody
- 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
all electromagnetic wavelengths can be what
- emitted from a blackbody - but same intensity at all wavelengths - peak wavelength depends on temperature
27
a blackbody is pretty much what
a star
28
wiens law
0. 0029mK/T - lower temps have a higher wavelength - higher temps mean lower wavelength
29
Stefan-Boltzmann law
-hotter objects emits more radiation at all wavelengths | Flux=(Constant)Temperature^4
30
which types of stars are blue
hotter stars
31
flux
energy per area per time
32
what is the type of element determined by
the number of protons
33
atomic number
number of protons in nucleus
34
atomic mass number
number of protons and neutrons
35
molecules
consist of two or more atoms
36
what type of line spectra is the solar spectrum
- absorption line spectrum | - this tells us that the sun has an atmosphere
37
Bohr model of the atom
electrons can only occupy certain orbits
38
what are spectral line caused by
when electrons transition between orbits
39
what is an orbital
energy levels of an atom
40
each orbital has what
an associated energy
41
electron always wants to be where
in the ground state at n=1
42
to get an electron form n=1 to n=2 you have to do what
add 10.2 Veto add more energy
43
electron can "move up" by
absorbing a photon
44
electron can "move down" by
emitting an electron
45
we can use the Stefan boltzmanns law to determine what
the flux of energy at the suns surface
46
blue-shifting
anytime a form of light moves towards the radio side of the spectrum (bottom)
47
red-shifting
when light shifts up towards the gamma ray side of the spectrum (top)
48
the light we see now has....
left its source sometime in the past
49
the further out in space we look...
the further back into time we see
50
knowing the flux and size of the star we can determine what
luminosity
51
luminosity
blackbody spectrum+ stefan boltzmann+ size of the star
52
if you know the radius and flux you can get the...
luminosity
53
if you know the flux and luminosity you can get the...
radius
54
power
energy per time
55
doppler effect
parent shift in wavelength due to the relative motion of the source and/or the observer
56
Doppler effect example
sirens of an ambulance are higher pitched as it goes towards you and lower pitched as it goes away
57
when the siren goes away its
redshifted
58
when the siren goes away its
blue shifted
59
the further away the object is in space the more (what color shift is it)
- redshift | - this proves that the universe is expanding