Astro exam 2

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65 Terms

1
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What are the main properties of light?

  1. Ray/Beam

    1. Reflection

    2. Refraction

  2. Wave Behavior

    1. Diffraction

    2. Dispersion

    3. Polarization

    4. Interference

  3. Particle Behavior

    1. Photoelectric Effect

2
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What is reflection in terms of light?

light bouncing off of a surface.

<p><span style="line-height: 115%;"><span>light bouncing off of a surface.</span></span></p>
3
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What is refraction in terms of light?

the bending of light as it passes through from one medium to another.

  • Small to large index of refraction (n) = light will bend toward normal

  • Large to small index of refraction (n) = light will bend away from normal

<p>the bending of light as it passes through from one medium to another.</p><ul><li><p><span style="background-color: transparent;"><strong><span>Small to large index of refraction (</span><em><span>n</span></em><span>) = light will bend toward normal</span></strong></span></p></li><li><p><span style="background-color: transparent;"><strong><span>Large to small index of refraction (</span><em><span>n</span></em><span>) = light will bend away from normal</span></strong></span></p></li></ul><p></p>
4
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What is particle behavior in terms of light?

light behaves as photons, discrete packets of energy.

5
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What is Constructive interference?

light waves overlap and amplify each other before continuing on their path.

<p>light waves overlap and amplify each other before continuing on their path.</p>
6
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What is Destructive interference?

Opposite light waves cancel each other before continuing on their path.

7
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What is the relationship between Wavelengths and photon energy?

shorter wavelength (higher frequency) → more energy & refraction/bluer light; longer wavelength (lower frequency) → less energy/redder light.

8
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Subproperties of light as a ray?

reflection and refraction

9
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Subproperties of light as a wave?

Diffraction

Dispersion

Polarization

Interference

  • Constructive

  • Destructive

10
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What are the different kinds of interference (light as a wave)?

Constructive and destructive

11
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Subproperties of the Particle properties of light?

Photoelectric effect

12
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photon energy formula?

E = hc/λ

  • hc = light constant

  • λ = wavelength

13
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What are the electromagnetic properties of light (waves)?

• Light consists of oscillating electric and magnetic fields perpendicular to each other.

        - Electric and magnetic fields are always at 90° to each other.

• does NOT require a medium to propagate (generate).

WAVELENGTH = λ

<p>• Light consists of oscillating electric and magnetic fields perpendicular to each other.</p><p>&nbsp; &nbsp; &nbsp; &nbsp; - Electric and magnetic fields are always at 90° to each other.</p><p>• does NOT require a medium to propagate (generate).</p><p>WAVELENGTH = <span>λ</span></p><p></p>
14
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How does light interact with human vision?

• Rods detect light intensity (brightness).

• Cones detect color; sensitive to red-green, blue-green, and violet-blue regions.

15
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What is a light ray?

A straight-line path that light travels.

16
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What is Snell’s law?

n1sin(θ)1 = n2sin(θ)2 - describes the angle of refraction between 2 media

<p>n1sin(θ)1 = n2sin(<span><span>θ)2 - describes the angle of refraction between 2 media</span></span></p>
17
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What is diffraction?

The spreading of light as it passes through an obstruction.

<p>The spreading of light as it passes through an obstruction.</p>
18
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What is dispersion?

The splitting of white light into constituent colors under refraction through a prism.

<p>The splitting of white light into constituent colors under refraction through a prism.</p>
19
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What is polarization?

Restriction of the electric field components of light to a single plane.

20
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What is interference?

Overlapping of light waves that can amplify (constructive) or cancel (destructive) each other.

21
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What is the photoelectric effect?

When light with enough energy hits a surface, it can eject electrons; energy is carried by photons.

(Ephoton = hc/λphoton)

<p>When light with enough energy hits a surface, it can eject electrons; energy is carried by photons.</p><p><span style="line-height: 115%;"><span>(</span><strong><span>Ephoton = hc/λphoton)</span></strong></span></p>
22
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How does wavelength relate to photon energy?

Shorter wavelength → more energy; longer wavelength → less energy.

23
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Order the visible colors from smallest to largest wavelength.

Violet (HIGH energy), Indigo, Blue, Green, Yellow, Orange, Red (LOW energy)

24
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Order types of light waves from least to most energy.

Radio (LARGE wavelength), Microwave, Infrared, Visible, Ultraviolet, X-ray, Gamma (SMALL wavelength)

25
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What are the human-visible light wavelengths?

4000–7000 angstroms (400–700 nm).

26
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What are rods responsible for?

Detecting light intensity.

27
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What are cones responsible for?

Detecting color.

28
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What is Kirchhoff’s FIRST law?

Any sound, liquid, or opaque gas that is heated above absolute zero will produce a continuous thermal radiation spectrum (LIGHT)

  • heated electrons produce light

29
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How does tempurature affect molecular states?

increasing tempurature = solid → liquid → gas.

30
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How does pressure affect molecular states?

Decreasing pressure = solid → liquid → gas.

31
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Why is ice less dense than water?

Solid water molecules are less densely packed than liquid water molecules - cool tempuratures don’t agitate the molecules.

32
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What is temperature?

Measure of atomic/molecular motion; quantifies kinetic energy.

33
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What are the temperature points in degrees Fahrenheit?

0°F = coldest in Fahrenheit’s hometown, 32°F = water freezes, 100°F = cow’s internal temp, 212°F = water boils.

34
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What are the Temperature points in degrees Celsius?

0°C = water freezes, 100°C = water boils.

35
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What is the absolute scale (Kelvin scale)?

scales the same as degrees C;

absolute 0 = where ALL molecular motion stops.

36
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General Relativity Theory

Mass itself warps spacetime, creating gravitational wells.

<p>Mass itself warps spacetime, creating gravitational wells.</p>
37
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What is an event horizon?

Boundary around a black hole beyond which nothing can escape.

38
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What is spaghettification?

Stretching vertically and compressing horizontally due to strong tidal forces near black holes.

39
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Name proofs of general relativity.

1) Solar eclipse starlight bending—the Sun’s gravity causes apparent positions of stars to shift during eclipse

2) frame dragging (gravity probe B)

<p>1) Solar eclipse starlight bending—the Sun’s gravity causes apparent positions of stars to shift during eclipse</p><p>2) frame dragging (gravity probe B)</p>
40
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Special Relativity Theory

Light speed is constant (300,000 km/s) for all inertial observers.

41
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What is length contraction? formula?

objects moving close to light speed appear shorter in the direction of motion; L = L0 ()

L0: observed length

<p>objects moving close to light speed appear shorter in the direction of motion; L = L0 (<span>➰</span>)</p><p>L0: observed length</p>
42
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What is time dilation? formula?

time passes more slower for an object moving close to light speed (t = t0/)

t0 = observed time

<p>time passes more slower for an object moving close to light speed (t = t0/<span>➰</span>)</p><p>t0 = observed time</p>
43
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Name proofs of special relativity.

Muon decay experiment (length contraction), twin paradox (time dilation).

44
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What is the muon decay experiment?

Because muons travel near the speed of light, their lengths contract (length contraction), allowing them to cover the distance to Earth before decaying - they normally don’t travel fast enough to make it to earth.

45
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What is the twin paradox?

When one twin travels on a high-speed spaceship and returns, they are younger than the stay-at-home twin due to time dilation;

at near-light speed, time slows and distances contract, effectively shifting through many inertial frames.

46
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IGNORE

Objects moving near light speed appear more massive.

47
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What is momentum (p)?

quantification of how much movement a mass has; p = mv

<p>quantification of how much movement a mass has; p = mv </p>
48
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What is kinetic energy?

energy of motion; (KE = 1/2mv^2)

49
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What is potential energy?

Energy stored due to position or state; (PE = mgh).

<p>Energy stored due to position or state; (PE = mgh).</p>
50
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What is a conserved quantity?

A property that remains constant if not added or removed from a system.

  • mass

  • can’t be spontaneously made/taken away

51
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What are some rules in energy problems?

Ei = Ef

  • PE = 0 at the end of a motion

  • KE = 0 at the start of a motion

Ei = KEi + PEi = 1/2mvi² + mgh

Ef = KEf + PEf = 1/2mvf² + mgh

**MASS (m) CAN BE CROSS-CANCELLED WHEN IT’S NOT GIVEN

<p>Ei = Ef</p><ul><li><p>PE = 0 at the end of a motion</p></li><li><p>KE = 0 at the start of a motion</p></li></ul><p>Ei = KEi + PEi = 1/2mvi² + mgh</p><p>Ef = KEf + PEf = 1/2mvf² + mgh</p><p>**MASS (m) CAN BE CROSS-CANCELLED WHEN IT’S NOT GIVEN</p><p></p>
52
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General theory of relativity

mass itself warps spacetime

53
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Special Theory of Relativity

speed of light is constant for everyone, regardless of their motion

  • cannot see it on ourselves, only see it on object moving relative to us

54
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frame dragging

is the effect where a spinning massive object causes spacetime to move along with it

  • mass twisting/warping spactime

55
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How many degrees C/degrees F in 0 K?

0 K = -273.15°C; -456°F

56
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Halflife

how long it takes for HALF of a sample to go through radioactive decay

57
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Kitchhoff’s SECOND Law

Any transparent gas that is “excited” will produce an emissions spectrum

58
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particles and quarks

Protons (+): 2 up quark, 1 down

Neutron: 2 down quark, 1 up

Electron (-)

59
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Changes in intensity of light: brightness & colorr

Dimmer light = cooler, redder; LOW FREQUENCY

Bright = hotter, bluer; HIGH FREQUENCY

60
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Sp notation

A (atomic mass = ΣpΣn)

Sp (species)

Z (atomic charge = Σp)

61
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Peak wavelength formula

(λmax (R) = 30,000,000/Temp(K)

62
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What is the sun’s peak wavelength?

λmax (Sun) = 5000 angstrom

63
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Angstrom (Å)

unit that describes wavelength intensity

64
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Wein’s law

peak wavelength has an inverse relationship with temperature

65
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Total energy in thermal emissions (Total E(photon)) formula

Total E(photon) = σT^4

  • Higher temp = power of 4

  • σ: stefan-boltzmann constant

doubling T makes value 16x larger (σ(2T)^4 = σ⋅2^4⋅T^4=16σT^4)