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astronomy final > astronomy exam 3 > Flashcards

astronomy exam 3 Flashcards

1
Q

What are two ways atoms get excited

A

Collision among atoms, photon of correct energy gives energy to an atom

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2
Q

two types of spectra

A

Absorption and emission

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3
Q

emission

A

See photons who are readmitted

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4
Q

higher radiation

A

higher temperature

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5
Q

lambda max

A

Wavelength where radiation curve has highest energy

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6
Q

intensity

A

Energy per unit time per unit area

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7
Q

doppler effect

A

Sound waves move differently when they are coming towards or away from you, sound is artificially compressed

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8
Q

longer wavelength =

A

red / shorter wavelength = blue

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9
Q

granules and sunspots

A

are features of the photosphere

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10
Q

spicules

A

chromosphere features

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11
Q

solar wind

A

Charged particles emitted from sun

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12
Q

zamon effect

A

helps remotely sense magnetic fields, sun spots have strong magnetic fields

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13
Q

plasma

A

highly ionized fluid

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14
Q

sun rotations

A

moves faster in its equator differential rotation

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15
Q

Kepplers law of planetary motion

A

p^2/a^3

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16
Q

coulomb force

A

repulsive force between particles with electrostatic charge, nuclear resistance to collisions reactions only at suns center

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17
Q

binding energy

A

energy needed to pull electron away

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18
Q

permitted orbits

A

One of the energy levls in atom that elecctrons may occupy

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19
Q

ground state

A

Lowest permitted electron orbit of atom

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20
Q

excited atom

A

moves from low to high energy levels

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21
Q

thermal energy

A

energy from agitation

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22
Q

blackbody radiation

A

radiation emitted by heated object made up of photons with distribution of wavelengths

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23
Q

stefan boltzwan law

A

mathematical relation between temp of black body and energy emitted

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24
Q

weins law

A

lambda max = 2.90 x 10^6/T(k)

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25
Q

balmer series

A

only 3 hydrgen lines in what series are visible

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26
Q

doppler effect

A

change in wavelength of radiation caused by motion of source

27
Q

nuclear fusion

A

combine light nuclei, net energy

28
Q

how much mass converts into energy

A

e=mc^2

29
Q

for fusion to occur

A

there needs to be high temperature and high density

30
Q

v-neutrino

A

subatomic particles that don’t like to interact

31
Q

parallax

A

position relative to other stars can change depending on our orbit

32
Q

intrinsic brightness

A

actual brightness distance effect accounted for

33
Q

luminosity

A

total ammount of energy a star emits every second

34
Q

spectral classification

A

use specture of star to determine the temperature of the star absorption line strength of carious elements allows temperature to be found

35
Q

spectropic parallax

A

finding distance to star using spectrum

36
Q

binary star system

A

center both orbits is center of mass at the center

37
Q

types of binary star systems

A

center both orbits is center of mass at the center

38
Q

visual system

A

observable through telescope as two stars.

39
Q

spetroscopic

A

look at spectrumm evidence that there are two stars

40
Q

eclipsing binary

A

orbital plane close to parallel to our line of sight dips in intensity when one blocks the other, total brightness is dimmed

41
Q

supernova explosion

A

shockwave hits gas and dust regions w cloud becomes more dense.

42
Q

protostar

A

lump in gas and dust cloud that becomes star because it is compressed and hot enough to be opaque to radiation and not go through nuclear

43
Q

cocoon

A

is the dust and gas around the protostar

44
Q

young stellar objects,

A

cocoon is gone so the protostar is more visible

45
Q

parrralc

A

is a shift in star position

46
Q

stellar parallax

A

shift of a star observed form 1 au baseline

47
Q

parsec

A

distance to imaginary star wit a parallaz of one arc second

48
Q

visual binary

A

is when two separate stars are visible on a telescope

49
Q

spectroscopic binary

A

are two stars that are too close together to be seen as separate visually

50
Q

spectroscopic parallax

A

finding distance by comparing apparent magnitude with absolute magnitude

51
Q

degenerate matter means

A

electrons groups together and dont let size of the core to change

52
Q

planetary nebula

A

in medium stars when outer layer of core begins to drift away

53
Q

core remnant

A

what remains all fusion stops

54
Q

compact object

A

not actually a star anymore after star cools

55
Q

white dwarf

A

what’s left of medium mass star after it dies, it has low luminosity because it has low surface area

56
Q

Chandreshhar limit

A

mac amount of mass white dwarf can have while remaining white dwarf

57
Q

why do sunspots appear dark?

A

they appear dark because of convection occurring near them leaving cool spots, on the surface. Because they are cool, they emmit less light and appear dark

58
Q

what conditions must be met for fusion to occur and be sustained?

A

temperature must be high enough, pressure must be high enough

59
Q

which object would have the most narrow absorption lines main sequence star, giant star, supergiant star

A

super giant

60
Q

where are granules found?

A

granules are areas new the surface caused by convection. They’re found in the photosphere

61
Q

what is happening in the core of the sun that generates energy

A

fusion

62
Q

is the average number of sunspots visible on the sun the same year after or not?

A

No, the average number of sunspots visible on the sun is not the same year after year. The number of sunspots visible from Earth changes daily and in cycles that can last for decades, centuries, or millennia. The most well-known cycle is the 11-year sunspot cycle, where the average number of sunspots increases and then decreases over the course of 11 years.

63
Q

explain how astronomers can estimate the luminosity of a star from its spectrum

A

Astronomers can estimate a star’s luminosity by analyzing its spectrum to determine its spectral type and luminosity class. A star’s spectrum of light appears as a color to the human eye, and the color is a good indicator of its brightness

64
Q

method used in spectroscopic parallax

A
  1. Fin the temperature of the star
  2. Use luminosity classification to estimate luminosity
  3. use H-R diagram to find Mv
  4. observe to find m
  5. fo the math to find d

astronomy final (4 decks)

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