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Astronomy 3L > Final > Flashcards

Final Flashcards

1
Q

A way to deduce data in between measured data points

A

Interpolation

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2
Q

An easy way to define the slope of a best fit line

A

Rise over run

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3
Q

A way of making a reasonable estimate of a value not contained within the measured data values

A

Extrapolation

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4
Q

A way to estimate the range of a specific data point

A

Consider the highest and lowest measurements representing that data point

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5
Q

Good estimate for the best value of multiple measurements

A

Take the average

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6
Q

Is it possible to have an absolutely precise measurement

A

No

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7
Q

It’s possible to determine the speed of an object by dividing

A

The distance traveled by the time it took to cover that distance

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8
Q

It’s possible to determine the time of an event by subtracting

A

The time it started by the time it ended

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9
Q

Credited as the first modern theoretical astronomer

A

Kepler

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10
Q

although they didn’t get along, they needed each others talents

A

Tycho and kepler

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11
Q

parallax uses the orbital diameter of the earth as a baseline of a triangle

A

true

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12
Q

Who first successfully measured a parallax

A

Frederick Bessel

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13
Q

Direct measurement of stellar distances

A

None

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14
Q

Equals 3.26 lightyears

A

Parsec

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15
Q

A parsec is a measurement used in

A

Parallax

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16
Q

The total power output of an object

A

Luminosity

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17
Q

An uncertainty is designated by which Greek letter

A

Loop with hook on top

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18
Q

Modern astronomers spend much of their time analyzing data in their offices

A

True

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19
Q

Determine the slope

A

Y-y/x-x

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20
Q

When graphing it’s ok to have a sharp corner in a best fit line

A

False

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21
Q

A best fit line is like connecting the dots

A

False

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22
Q

A graph is titled and displayed as

A

Y versus x

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23
Q

The best pre telescopic Astronomical observer

A

Tycho Brahe

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24
Q

A planet travels fastest when it is farthest from the sun

A

False

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25
Q

From hottest to coldest these are the suns spectral classes

A

OBAFGKM

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26
Q

Human error plagues all scientific experiments

A

False

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27
Q

A parsec equals about 3.26 ly

A

True

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28
Q

A parsec is a measurement used in

A

Parallax

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29
Q

Luminosity is defined as

A

The total power output of an object

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30
Q

main sequence stars burn which element in their cores

A

hydrogen

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31
Q

The early 20th century astronomer known for both his meticulous astrophotography work as well as his lack of formal education was

A

Milton Humason

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32
Q

the principle first elucidated in Kepler’s third law is still useful to astronomers today

A

true

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33
Q

the english 19th century astronomer known for both his study of small solar system objects as well as discovering that stellar magnitudes corresponded to a logarithmic progression was

A

Robert Pogson

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34
Q

Parallax uses actual stellar measurement

A

true

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35
Q

a noted woman astronomer who determined the correct order for the harvard college observatory’s stellar spectra was

A

Annie Jump Cannon

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36
Q

Cepheid variable measurements rely on having distinct spectra

A

false

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37
Q

Edwin Hubble using Humason’s galactic spectra discovered the expansion of the universe

A

true

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38
Q

A noted woman astronomer who used cepheid variable stars to determine distance was

A

Henrietta Leavitt

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39
Q

If the disk of Sirius replaced the disk of the sun

A

it would be larger and brighter

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40
Q

what technique can determine the surface temperature of a star?

A

Wein’s law

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41
Q

Spectroscopic parallax and cepheid variables are exactly the same thing

A

false

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42
Q

which type of magnitude could you use for determining stellar distance?

A

both of these together (absolute and apparent)

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43
Q

the birth of astrophysics was initiated by

A

both of these (herzprung and russell)

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44
Q

Luminosity refers to

A

the total energy or power output of an object

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45
Q

even if it’s not a straight line, a best fit line on a graph can be used to interpolate or extrapolate valuable scientific information

A

true

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46
Q

spectroscopic parallax doesn’t actually need a parallax degree measurement., but rather a distinct stellar spectrum

A

True

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47
Q

a cepheid variable can be used as a standard candle

A

true

48
Q

astronomical objects used to measure distances to galaxies

A

standard candle

49
Q

a method for measuring distances to stars. can be used to any main sequence star with a spectrum that can be recorded

A

spectroscopic parallax

50
Q

galaxies containing a flat, rotating disk of stars, gas, and dust, with a central concentration of stars

A

spiral galaxy

51
Q

a spiral galaxy with a bar shaped structure of stars

A

barred spiral galaxy

52
Q

a spherical cluster of typically older stars on the outskirts of a galaxy

A

globular cluster

53
Q

the first astronomer to realize the vastness of the milky way and observed globular clusters on mount wilson

A

harlow shapley

54
Q

an astronomer who studied eclipses and believed there to be galaxies outside our own. Debated with Shapley over the size of the universe and the nature of spiral nebulae

A

Heber Curtis

55
Q

specifies each point on a plane by two coordinates

A

cartesian coordinate system

56
Q

the x coordinate

A

abscissa

57
Q

the y coordinate

A

ordinate

58
Q

a line drawn to be equal along coordinates

A

best fit line

59
Q

a measure of steepness, rise over run

A

slope of a line

60
Q

a system of gas, dust, and stars with their solar systems

A

galaxy

61
Q

all points of a moving body moving in the same direction

A

translational motion

62
Q

all points of an object circling around an axis

A

rotational motion

63
Q

the squares of the orbital periods of the planets are directly proportional to the cubes of the semi major axes of their orbits

A

kepler’s third law

64
Q

a unit of angular measuring, 1/60th of a degree. The distance travelled in one minute

A

arc minute

65
Q

a uit of angular measuring, the distance travelled in one second.

A

arc second

66
Q

the approximate distance from the center of the Earth to the center of hte sun

A

astronomical unit

67
Q

the distance light travels in one year

A

light year

68
Q

a unit used to measure and express distances to stars and galaxies. Equivalent to 3.26 light years

A

parsec

69
Q

the apparent difference of an object seen from two different places

A

parallax

70
Q

a German astronomer and the first to find reliable values for the distances to other stars from our sun using parallax

A

Friedrich Bessel

71
Q

indicate a wider frequency or wavelength in the radiation of an object due to emission or absorption

A

broadening of spectral lines

72
Q

an indicator of whether a star or galaxy is moving towards or away from us, with light stretching blue when towards and red when away

A

Doppler effect

73
Q

wavelength of the stars and galaxies are stretched to red, it means that space is expanding

A

the cosmological redshift

74
Q

splitting a spectral line into two or more different frequencies when in a magnetic field

A

zeeman effect

75
Q

an american astronomer who co discovered a relationship between the absolute magnitude of a star and its spectral lines relative intensities, using these to determine the size of stars. Director of Wilson observatory, studied spectral and attempted to correlate spectral lines to absolute magnitude.

A

Walter S Adams

76
Q

A german astronomer who worked at the Mount Wilson observatory where he studied the spectra of the sun with Walter S Adams

A

Ernst A Kohlshutter

77
Q

a band of stars that have hot, dense cores that produces energy from hydrogen and helium

A

main sequence stars

78
Q

occupying the upper part of the H R diagram, these develop when main sequence stars run out of hydrogen

A

super giant stars

79
Q

main sequence stars after using up all nuclear fuel, bottom left

A

white dwarfs

80
Q

A star in the final stages of stellar evolution, our sun will become this one day

A

red star

81
Q

a supernova from a star up to fifty times the mass of a sun, comes from the rapid collapse of such a star

A

type two supernova

82
Q

a supernova that takes matter from a neighboring star until a nuclear reaction is triggered

A

type one supernova

83
Q

a harvard computer who discovered the cycle of fluctuation in cepheid variables and how to use them to find distances

A

Henrietta Leavitt

84
Q

An Americanastronomer who discovered galaxies are moving away from us. Also discovered dark matter, the evolution of stars and galaxies, how solar systems form, and black holes

A

Edwin Hubble

85
Q

An American astronomer who provided high quality photographs of stars and discovered Comet Humason. Was a janitor and had no stellar education

A

Milton Humason

86
Q

Proposed the sun was stationary in the center of the galaxy, and the planets revolved around it.

A

Nicolas Copernicus

87
Q

Confirmed the theory that the Earth revolved around the sun, and was the first to use a telescope to observe astronomical bodies.

A

Galileo

88
Q

Split sunlight with prisms, created larger prism in 1800s that could observe 574 dark lines in continuous spectrum. Combination prism and telescope allowed spectra moon, mars, Venus, later used diffraction gratings. Came to the conclusion white light was all colors.

A

Newton

89
Q

Collects first star catalogue, considered the greatest astronomical observer using Babylonian star records and accurate models of the motion of the sun and moon. Developed trigonometry and assigned magnitude 1-2 to brightest stars and marked their places on metal plate to divide them by six magnitude classes

A

Hipparchus

90
Q

He discovered several minor planets and made observations on comets. He introduced a mathematical scale of stellar magnitudes with the ratio of two successive magnitudes being the fifth root of one hundred (~2.512) and referred to as Pogson’s ratio.

A

Robert Pogson

91
Q

Comparing the known absolute magnitude of this celestial object with well known intrinsic luminosities with its measured apparent magnitude allows a highly accurate estimation of distances. Globular clusters

A

standard candle

92
Q

Compares stars by plotting luminosity versus color (or energy versus temperature). Plots revealed if there were common properties governing behavior of stars, and correlations were obvious

A

HR diagram

93
Q

Indirect method to measure distances. it does not rely on the geometric parallax effect. can be applied to any main sequence star for which a spectrum can be recorded. The method depends on the star being sufficiently bright to provide a measurable spectrum, one must measure the apparent magnitude of the star and know the spectral type of the star.

A

spectroscopic parallax

94
Q

When an atom receives a precise level of incoming energy, electrons orbiting the nucleus of the atom absorb and transit it to a higher state. A dark line will be visible in the spectrum

A

absorption spectra

95
Q

is an event that occurs when one object is hidden from the observer by another object that passes between them

A

occultation

96
Q

all planets orbit the sun in an ellipse, with the sun as one of the focii

A

keplers first law

97
Q

It states that a line between the Sun and the planet sweeps equal areas in equal times. Thus, the speed of the planet increases as it nears the Sun and decreases as it recedes from the Sun.

A

keplers second law

98
Q

P² = a³, so the period of a planet’s orbit (P) squared is equal to the size semi-major axis of the orbit (a) cubed when it is expressed in astronomical units

A

keplers third law

99
Q

a more general form of Kepler’s Third Law that could apply to any two objects orbiting a common center of mass. M1 + M2 = A3/P211. Kepler’s Law is T2R3 = K constant and T is period of traslation in orbit and R again, distance between Sun and Planet2.

A

Newton’s derivation of Keplers third law

100
Q

The modern stellar classification scheme is based on spectral absorption or emission lines, which are sensitive mostly to the star’s surface temperatures, rather than differences in gravity, chemical composition, or luminosity.

A

Harvard observatory classification of stellar spectra

101
Q

Electron must shed absorbed energy by emitting a photon of light at that exact energy level (color). When these pass through a prism, the spectrum is revealed

A

emission spectra

102
Q

measure of an object from earth

A

apparent magnitude

103
Q

10pc from the earth observed

A

absolute magnitude

104
Q

a displacement or difference in the apparent position of an object viewed along two different lines of sight and is measured by the angle or half-angle of inclination between those two lines.

A

parallax

105
Q

the field of study that measures and interprets the electromagnetic spectra that result from the interaction between electromagnetic radiation and matter as a function of the wavelength or frequency of the radiation

A

spectroscopy

106
Q

The amount can be calculated by gravitational lensing. At the cosmic scale, when there is a source large source of light L such as light from a galaxy which is located behind a body of large mass (visible + invisible matter) M, the mass of M acts as a lens and bends the light from L.

A

dark matter

107
Q

A celestial object consisting of a nucleus of ice and dust and a tail of gas by the sun

A

Comet

108
Q

A comet that only lasts less than 200 years and is found near the ecliptic

A

Short period comet

109
Q

A comet with 200+ year orbital periods and possibly from the Oort cloud

A

Long period comet

110
Q

A comet that passes close to the Sun at perihelion

A

Sun grazing comet

111
Q

Circumstellar disc in the outer solar system larger than the asteroid belt

A

Kuiper belt

112
Q

Predicted collection of icy objects found farther away than anything else in our solar system

A

Oort Cloud

113
Q

Levy 9 broke apart and collided with Jupiter, providing the first direct observation of an extraterrestrial collision of solar system objects

A

Comet shoemaker

114
Q

An American stronger who discovered the dirty snowball hypothesis

A

Whipple

115
Q

key theoretical development for 20th-century astronomy and cosmology was the development of the theory of relativity, from 1905 to 1915, which eventually led to an explanation of the origin of the universe.

A

Einstein

Astronomy 3L (4 decks)

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