The Big Bang Thursday, January 17. Doppler shift Doppler shift tells you if an object is coming...
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Transcript of The Big Bang Thursday, January 17. Doppler shift Doppler shift tells you if an object is coming...
![Page 1: The Big Bang Thursday, January 17. Doppler shift Doppler shift tells you if an object is coming toward you or moving away. Blueshift: distance decreasing.](https://reader036.fdocuments.in/reader036/viewer/2022062517/56649ec65503460f94bd201f/html5/thumbnails/1.jpg)
The Big BangThe Big Bang
Thursday, January 17
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Doppler shiftDoppler shift tells you if an object is coming toward you or moving away.
Blueshift: distance decreasing.
Redshift: distance increasing.
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All distant galaxies have redshifts.
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But wait, there’s more!....
The amountamount by which the wavelength is shifted tells us the radial velocityradial velocity of the object, in kilometers/second.
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A light source is at rest: it emits light with a wavelength λ0.
If distance to light source is changingchanging, Doppler shift will
change the wavelength to λ ≠ λ0 .
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Size of Doppler shift is proportional to radial velocity:
c
V
0
0
λ = observed wavelength
λ0 = wavelength if source isn’t at rest
V = radial velocity of moving source
c = speed of light
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Hydrogen absorbs light with λ0 = 656.3 nm.
You observe a star with a hydrogen absorption line at λ = 656.2 nm.
656.3 nm ↓
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Thinking locally: stars within 3 parsecs of the Sun.
Proxima Centauri
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Equal numbers of redshifts and
blueshifts.
Typical radial velocity V = 30 km/second
(70,000 mph).
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Thinking more globally: galaxies within 30 million parsecs of the Milky Way.
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Almost all redshifts rather than blueshifts.
Typical radial velocity V = 1000 km/second
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How do we know the distances How do we know the distances to stars and galaxies?to stars and galaxies?
No No sensesense of depth! of depth!
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Climbing the “cosmic distance ladder”.
Can’t use the same technique to find distance to everyevery astronomical object.
Use one technique within Solar System (1st “rung” of ladder); another for
nearby stars (2nd “rung”), etc...
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11stst rung rung of the distance ladder: distances within the Solar System.
Distances from Earth to nearby planets are found by radarradar.
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Radar distance measurement:
Send out a strong radio pulse, wait until the faint reflected pulse returns.
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Measured round-tripround-trip travel time = t
(typically several minutes)
One-way One-way travel time = t/2
DistanceDistance = speed × one-way travel time
Since radio waves are a form of light, distance = c t / 2
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Using fancy technical methods, round-trip travel time can be
measured with great accuracy.
Thus, we know distances within the Solar System very well indeed.
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1 astronomical unit (average distance from Sun’s center to Earth’s center) =
149,597,870,690 meters (plus or minus 30 meters).
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22ndnd rung: rung: distances to nearby stars within the Milky Way Galaxy.
Distances from Solar System to nearby stars are found by parallaxparallax.
← Proxima Centauri
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1 parsec = distance at which a star has a parallax of 1 arcsecond.
1 parsec = 206,000 astronomical units = 3.26 light-years
Not to scale
Flashback slide!
↓observed starobserver→
parallax angle
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Measured parallax angle is inversely inversely proportional to a star’s distance.
p
parsec 1 Distance (p = parallax angle,
in arcseconds)
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First star to have its parallax angle measured: 61 Cygni (in the year 1838).
Parallax angle = 0.287 arcseconds
Distance = 1 parsec / 0.287 =
3.48 parsecs
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With the Hipparcos satellite, astronomers measured parallax angles with an accuracy of 0.001 arcseconds.
Parallax too small to measure for stars more than 1000 parsecs away.
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33rdrd rung: rung: distances to galaxies beyond our own.
Distances from Milky Way to nearby galaxies are found with standard candlesstandard candles.
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In the jargon of astronomers, a “standard candle” is a light
source of known luminosity.
LuminosityLuminosity is the rate at which light source radiates away energy
(in other words, it’s the wattage).
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Sun’s luminosity = 4 × 1026 watts = 4 × 1033 ergs per second
When we measure the light from a star, we aren’taren’t measuring the luminosity.
To do that, we’d have to capture allall the light from the star.
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When we measure the light from a star, we are measuring the fluxflux.
The flux is the wattage received perper square metersquare meter of our telescope lens.
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At distance d from star of luminosity L,
the luminosity is spread over an area
4πd2.
Flux = luminosity / area
F = L / ( 4 π d2 )
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What’s this got to do with finding the distance?
You knowknow luminosity (L) of a standard candle. You measuremeasure the flux (F).
You computecompute the distance (d):
F4
L d
2d4
LF
π
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Climbing the distance ladder.
1) Measure flux of two standard candles: one near, one far.
2) Find distance to near standard candle from its parallax.
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3) Compute luminosity of near standard candle: L = 4 π d2 F.
4) Assume far standard candle has same luminosity as the near.
5) Compute the distance to the far standard candle:
F4
L d
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A good standard candle: Cepheid variable stars
Cepheid stars vary in brightness with a period that depends on their average
luminosity.
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Observe Cepheid.
Measure period.
Look up luminosity.
Measure flux.
Compute its distance!
F4
L d
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In 1929, Edwin HubbleEdwin Hubble looked at the relation between radial velocity and
distance for galaxies.
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Hubble’s result: Radial velocity of a galaxy is
linearly proportional to its distance.
Modern data
1 Mpc = 1 million parsecs
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Hubble’s law (that radial velocity is
proportional to distance) led to
acceptance of the Big Big BangBang model.
Big Bang model: universe started in an extremely dense state, but
became less dense as it expanded.