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Physics Module 5 > Classification of stars > Flashcards

Classification of stars Flashcards

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1
Q

Definition parsec

A

the distance to an object subtending 1 second of arc to the radius of the Earth’s orbit.
(1 second of arc (arcsecond) = 1/3600 of a degree).

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2
Q

Units parsec

A

pc

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3
Q

Definition light year

A

Distance light travels in a vacuum in 1 year.

(number of seconds in 1 year = 365 x 24 x 60 x 60 = 3.15x107s

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4
Q

Units light year

A

lyr

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5
Q

Definition astronomical unit

A

The mean distance between the Earth and the Sun

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6
Q

Units astronomical unit

A

AU

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7
Q

Definition of absolute magnitude

A

The brightness an object would appear if it was 10 parsecs from the Earth.

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8
Q

Definition of apparent magnitude

A

The brightness of an object as seen from Earth

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9
Q

What is black body radiation?

A

The electromagnetic radiation emitted by an object because of its temperature

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10
Q

General shape of black body curves

A

Temperature is DECREASING going from P to R.

Area under curve is total power output per m2 (as given by Stefan’s Law)

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11
Q

Definition of (lander)max

A

The wavelength at which maximum emission occurs.

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12
Q

Assumption about a star to use Wein’s displacement law ((lander)max)

A

Star is acting as a black body.

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13
Q

Effect of atmosphere on estimate of a star’s temperature

A
  • Ozone in atmosphere preferentially absorbs UV part of spectrum
  • This increases observed max (longer wavelength)
  • Resulting in an underestimate of the star’s temperature
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14
Q

Definition of intensity

A

energy arriving every second on a 1 m2 surface orientated perpendicular to the direction of radiation

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15
Q

Units of intensity

A

Wm-2

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16
Q

Relation between intensity and apparent magnitude

A

Each change in magnitude of 1 (on the magnitude scale) corresponds to a change in intensity of 2.5 (actually 2.51).
So a star which has a magnitude that is 5 times brighter than another star, has an intensity which is 100 times greater (2.55 = 100).

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17
Q

Inverse square law and assumptions in its application

A

the intensity I at a distance r from a star with a total power output P, is given by
Intensity
Inverse square law assumes that:
• no light is scattered or absorbed between source and observer
• the source can be treated as a point

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18
Q

Spectral Class O

A

colour = Blue, Temp. = 50,000 - 25,000, He+ He H absorption lines

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19
Q

Spectral Class B

A

colour = Blue, Temp. = 25,000 - 11,000, He H absorption lines

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20
Q

Spectral Class A

A

colour = Blue - White, Temp. = 11,000 - 7,500, H(strongest) Ionised metals absorption lines

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21
Q

Spectral Class F

A

colour = White, Temp. = 7,500 - 6,000, Ionised metals absorption lines

22
Q

Spectral Class G

A

colour = Yellow - White, Temp. = 6,000 - 5,000, Ionised & neutral metals absorption lines

23
Q

Spectral Class K

A

colour = Orange, Temp. = 5,000 - 3,500, neutral metals absorption lines

24
Q

Spectral Class M

A

colour = Red, Temp. = 3,500 - 2,500, neutral metals & TiO absorption lines

25
Q

How are Hydrogen Banter lines produced?

A
  • The atmosphere of the star has hydrogen atoms with electrons in the n=2 state
  • Light from the star passes through the atmosphere of the star
  • Electrons (at the n=2 level) are excited into higher energy states
  • They can only absorb certain amounts of energy
  • These certain energies are related to specific frequencies (E=hf)
  • The electrons then de-excite
  • The electrons may de-excite through different energy level changes
  • When the electrons de-excite the light is radiated in all directions
  • This means that the intensity of the light at particular frequencies is reduced, resulting in absorption lines
26
Q

For a Hertzsprung Russell (HR) diagram…

A

…You need to:
• Know names of different star categories
• Sketch the position of different star categories
• Add appropriate scales to axes (absolute magnitude, temperature and/or spectral class).
• show life cycle of our sun as a line on HR diagram (from main sequence [G5], to giants, to white dwarf)

27
Q

Spectral class and magnitude of our sun

A

G5 (it’s like a, like a, like a G6 – but not a G6)

28
Q

Stellar evolution of our sun

A
  • Our sun is currently a main sequence star (G5)
  • As it uses up Hydrogen fuel and starts fusing Helium its core gets hotter and expands - it becomes a giant star.
  • As it expands, the outer surface of Sun will cool
  • Outer parts of sun are pushed away (by continued Helium fusion) to form planetary nebula.
  • Leaving extremely hot but small core - it becomes a white dwarf.
  • Fusion has finished and the white dwarf cools eventually to a brown dwarf.
29
Q

Neutron star composition and properties

A

Neutron stars consist of neutrons and have the density of nuclear matter

30
Q

Properties of a neutron star

A
  • very dense
  • powerful radio source
  • spinning (usually very quickly)
  • strong magnetic field
  • faint
31
Q

Definition of a supernova

A

Where the absolute magnitude of a star increases rapidly and enormously due to it exploding

32
Q

Definition of a black hole

A

an object whose escape velocity is greater than the speed of light

33
Q

Properties of a black hole

A
  • Large gravitational field strength

* Nothing, including light, can escape

34
Q

Definition event horizon

A 
The boundary (or surface) where the escape velocity equals the speed of light
Schwarzschild radius, Rs, on formula sheet is the radius of the event horizon
35
Q

What is at the centre of galaxies?

A

Super massive black holes

36
Q

How are type 1a supernovae used as standard candles to determine distances

A
  • All type 1a supernovae have the same peak absolute magnitude (M).
  • Apparent magnitude, m, (of supernovae) can be measured
  • Distance to galaxy, d, (supernova) can be calculated using m-M=5log(d/10).
37
Q

Controversy surrounding accelerating universe

A
  • The absolute magnitude of type 1a supernova is known, so they can be used as standard candles
  • Using m-M=5log(d/10) the distance to the galaxy can be calculated
  • Supernovae are very bright so they can be seen in very distant galaxies
  • It has taken billions of years for the light from the most distant galaxies to reach Earth; these supernovae were therefore produced when the Universe was young
  • Measurement of red shift (to measure velocity) and use of Hubble’s Law shows that these supernovae are fainter than expected
  • This indicates that the Universe is expanding faster now than when the supernovae exploded as the light has had to travel further to reach us than expected by a constant rate of expansion.
38
Q

What is causing accelerating expansion of universe?

A

Dark energy

39
Q

Binary star system

A

Two stars orbiting a common centre of mass

40
Q

Eclipsing binary star system

A

Binary star system whose orbit lies in same plane as the line of sight from the Earth
(so one star passes in front of the other as observed from Earth)

41
Q

Explain light curve from binary star system

A
  • Brightest magnitude occurs when both stars can be seen.
  • First (smaller) dip occurs when brighter star is in front of dimmer star.
  • Second (large) dip occurs when dimmer star is in front of brighter star.
42
Q

Definition of Doppler effect

A

Change in wavelength (of em radiation) due to relative velocity between observer and source

43
Q

How can Doppler effect be used to calculate relative velocity?

A
  • From spectrum obtain change in wavelength, for a spectral line
  • Using known wavelength measured on Earth,
  • Calculate v from Change in wavelength over wavelength = v/c
44
Q

Assumption for Doppler equation

A

v

45
Q

Definition of red shift

A

Increase in wavelength (of em radiation) due to relative recessive velocity between observer and source

46
Q

Interpretation of red shift in terms of expanding universe

A

Hubble observed that:
• (virtually) all galaxies are red shifted – means they are moving away from us (and each other)
• the more distant galaxies have greater red shifts – meaning more distant galaxies are travelling faster
• Hubble discovered that the (recessional) velocity of a galaxy was directly proportional to its distance.

47
Q

Estimation of age of universe

A

from v=d/t and hubbles law, v= Hd…

Time (age of uni.) = d/v = d/Hd = 1/H

48
Q

Assumption for estimating age of Universe from Hubble’s Law

A

Hubble’s constant, H, has been constant since the Big Bang.

49
Q

Features of Big Bang

A
  • Expanding universe
  • from an extremely hot and dense single point
  • Suggest about 15 billion years ago (from Hubble’s constant)
  • “explosion” – creation of space/matter and time
50
Q

Evidence for Big Bang

A

Redshift of distant galaxies
• In keeping with Hubble’s law (see Hubble observations above).
• Hubble’s law can be used to age universe.

Cosmological microwave background radiation
• If Universe is about 15 billion years old and has been expanding and cooling since Big Bang.
• would estimate temperature of “empty space” to be a few Kelvin after this time.
• black body curve of “empty space” corresponds to temperature of about 2.7 Kelvin (appropriate max)
• consistent with temperature universe would have cooled to after 15 billion years

Relative abundance of Helium and Hydrogen
• short time after Big Bang universe hot enough to fuse matter
• Hydrogen fused to form Helium
• Universe continued to expand, and cool
• making fusion of helium into heavier elements impossible
• creating predicted ratio of 3:1 (Hydrogen to Helium)
• consistent with observation of matter in Universe.

51
Q

Properties of quasars

A
  • Originally identified as strong radio sources (though now known to emit at all parts of em spectrum)
  • They have very large red shifts (and hence large distance from Hubble’s law)
  • They are very faint (dim apparent magnitudes)
  • They are very small (about size of a solar system)
  • Application of m-M=5log(d/10), using d calculated from Hubble’s law, suggests they are the brightest objects in the universe (same absolute magnitude as several galaxies put together)
  • Now believed to be super massive black holes at centre of active galaxies
  • Most distant measurable objects.

Physics Module 5 (5 decks)

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