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astronomy final > astronomy exam 2 > Flashcards

astronomy exam 2 Flashcards

1
Q

plato and aristotle

A

believed in a geocentric earth and that the perfect heavens were in the midst of a perfect sphere, and that planets orbited earth in a central path

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2
Q

retrograde motion

A

what they observed as moving forward then stepping back, didn’t fit with geocentric theory

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3
Q

ptolemy

A

mathematician who liked geocentric earth, but understood the dilemma and came up with platonic geocentric plan

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4
Q

platonic geocentric earth

A

move earth over slightly from center, planets moved at constant speed, there were epicycles and deferent

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5
Q

equant

A

where you’d see things moving at a constant speed

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6
Q

mercury and venus

A

were never seen far from the sun, their epicycles were along lines that connected earth to the sun

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7
Q

ecliptic

A

apparent path of the sun against a background of stars (projection of earth orbiting against sky)

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8
Q

zodiac

A

band around the sky about 9 degree above and below the ecliptic

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9
Q

pseudoscience

A

set of beliefs that doesn’t follow basic scientific ideas

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10
Q

Milankovitch Hypothesis 1920

A

small changes in earths orbit, precession, and inclination effect earths climate and caused ice ages

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11
Q

scientific argument

A

careful presentation of theory and evidence in logical discussion

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12
Q

angular diameter/2.06 x 10^5

A

linear diameter/distance

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13
Q

copernicus

A

came up with heliocentric theory and explained retrograde motion

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14
Q

1563

A

Jupiter and Saturn close to the sun in sky, both models fail

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15
Q

three laws of motion

A
  1. a body continues at rest or in uniform motion in a straight line unless acted upon by some force
  2. The change of motion (a) of a body of mass m is proportional to the force (f) actin on it and is in the direction of the force
    f =ma
  3. When are body exerts a force on a secons body the second body exerts equal and opposite force back
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16
Q

Kepler’s three laws of planetary motion

A

planets move on elliptical orbits around sun, constant area and velocity, p^2/a^3 = constant

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17
Q

p

A

orbital speed

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18
Q

a

A

semi major axis

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19
Q

galileo (late 1500’s)

A

used telscopes and wrote about his observations, found out the moon is imperfect, saw stars too faint for the naked eye, also thought there were planets orbiting Jupiter.

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20
Q

galilean satellites

A

Galileo thought there were planets orbiting Jupiter, but they are moons that orbit at different speeds and this confirms geocentric view of the earth

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21
Q

galileos discovery about the sun

A

that the sun had spots and they moved which meant it was spinning

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22
Q

Galileo’s discovery about Venus

A

venus had phases like the moon which meant a heliocentric system

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23
Q

Isaac Newton

A

discovered gravity, calculus, theory of light, laws of motion

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24
Q

forces are expressed in

A

Newtons

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25
Q

force of attraction equation

A

F = GMaMb/r^2

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26
Q

Newtons laws of gravity states that

A

force always pulls mass to the center

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27
Q

2nd law of motion

A

F=ma (a= kinematic quality of acceleration)

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28
Q

velocity

A

is always tangent to direction, changes during motion

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29
Q

circular velocity (speed of object in motion)

A

V= (sqrt) GME/r

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30
Q

affects tides

A

gravitational force on near side of earth gets pulled more than the far side

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31
Q

kepler’s third law

A

p^2/a^3= constant

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32
Q

newton’s equation to help us find mass of an object

A

p^2/r^3= 4pi^2/Gme

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33
Q

angstrom

A

distance measurement of 10^-10 m

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34
Q

copernicus

A

heliocentric universe, couldn’t precisely say planetary positions, said earth moves faster than other planets further from the sun,

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35
Q

paradigm

A

commonly accepted set of ideas and scientific assumptions

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36
Q

kepler

A

abandoned uniform circular motion, faster when closer to the sun

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37
Q

ellipse

A

closed curve around 2 points, total distance from 1 focus to any point on curve back to other focus in constant

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38
Q

semimajor axis

A

half of longest axis of ellipse

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39
Q

eccentricity e

A

measure of flattening of ellipse an ellipse of e=0 is circular, closer to 1 it gets the flatter

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40
Q

first law of motion

A

orbits of planets are ellipses (nearly circular)

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41
Q

second law

A

planet moves from A to B in 1 month, same time from A^1 to B^1

42
Q

Ptolemy attempted to explain motion of planets using

A

epicycles and defferents

43
Q

third law

A

orbital periods are related to their distance from the sun

44
Q

theory

A

is not a tentative idea

45
Q

mass

A

matter of an object

46
Q

inverse square relation

A

both force of gravity and light intensity decrease with square of distance form source

47
Q

spring tides

A

high amplitude at new moon

48
Q

neap tides

A

low amplitude at first 3 quarter moons

49
Q

light in classical theory

A

is a transverse wave

50
Q

speed

A

distance/time

51
Q

modern view of light

A

it is a photon

52
Q

photon

A

bundle of energy with wavelength and volume, particle of electromagnetic wave

53
Q

photon

A

bundle of energy with wavelength and volume, particle of electromagnetic wave

54
Q

E=hv

A

e= energy of photon, h= planks constant, v= frequency

55
Q

problems with refracting telescopes

A

hard to make perfect glass without impurities, machining lens is difficult, can only support around edge which limits size,

56
Q

refraction

A

bending of light

57
Q

chromatic aberation

A

refraction depends on wavelength, but waves don’t meet at the same place and this prevents clearly focused images

58
Q

reflecting telescopes

A

have better support and no chromatic abberation

59
Q

what does telescope do

A

gathers light, resolution, magnification

60
Q

light

A

electromagnetic radiation

61
Q

electromagnetic spectrum

A

goes through space at 3.000 x 10^8m/s

62
Q

wavelength

A

distance between peaks of a wave

63
Q

frequency

A

number of waves passing in one second (v)

64
Q

higher frequency =

A

shorter wave

65
Q

inversely

A

amount of energy a photon carries is —- proportional to its wavelength

66
Q

spectrum

A

array of electromagnetic radiation in order wavelength

67
Q

infrared

A

beyond red end of visible spectrum

68
Q

optical telescopes

A

collect visible light

69
Q

resolving power

A

ability of telescope to reveal fine detail

70
Q

diffraction fringe

A

unavoidable blurring around every point of light in image

71
Q

proportional

A

diffraction fringe is to wavelength

72
Q

seeing

A

refers to amount of image blurring due to atmospheric

73
Q

radio astronomer

A

have poor resolution and low signal instensity

74
Q

light gathering powers

A

to compare calculate the ratio of the areas of the primaries which is the ratio of the D squared

75
Q

resolving power calculate

A

to calculate = angular distance between 2 stars

76
Q

magnifying power

A

to calculate ratio of focal length of primary lens over eyepiece

77
Q

hubble space telescope

A

most successful observatory in history, lacks seeing distortion

78
Q

photographic plate

A

records images of celestial objects

79
Q

photometers

A

sensitive light meters that measure brightness of individual objects

80
Q

charge-coupled devices

A

more sensitive, digitized images, image-recording devices and photometers

81
Q

array detectors

A

infrared detectors

82
Q

represational-color-images

A

colors represent intensity

83
Q

spectograph

A

spreads out light according to color and uses grating

84
Q

spectral lines

A

dark or bright lines that cross spectrum at specific wavelengths

85
Q

adaptive optics

A

monitors and corrects atmospheric distortion

86
Q

laser guide star

A

artificial star from atmosphere glow

87
Q

inerferometry

A

synthesizing large telescopes using small ones

88
Q

spectrograph

A

breaks light up into spectrum

89
Q

cosmic rays

A

subatomic particles through space at tremendous velocities, created somehow that go through space and collide in earths upper atmosphere make a shower of secondary particles

90
Q

isotopes

A

same protons, different neutrons

91
Q

ion

A

a charged atom, any atom that isn’t neutral

92
Q

Balmer series

A

light from hydrogen gas thats visible to humans

93
Q

400-700 nm

A

visible light

94
Q

ways atoms get excited

A

collisions among atoms, photon of correct energy gives energy to atom

95
Q

2 types of spectra

A

absorption and emission spectra

96
Q

absorption

A

when rays bounce off in different directions, path is diverted when its spit out

97
Q

emission

A

takes longer, see photons who are readmitted

98
Q

lyman

A

studied transition from higher to lower N, we can’t see those

99
Q

Balmer

A

is N=2, which we can see

100
Q

Pascheh

A

is N=3, we can’t see

101
Q

higher temperature gas

A

transfers things down to N=2 division

102
Q

why is it necessary to have rockets and satellites in order to do UV and X ray astronomy?

A

Because Earth’s atmosphere absorbs most of these types of radiation

astronomy final (4 decks)

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