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Slipher’s Spectra of Nebulae

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Iron. Iron. Iron. Iron. Scandium. Scandium. Sodium. Sodium. Slipher’s Spectra of Nebulae. Lowell Telescope – near Flagstaff Arizona –provided spectra of ~50 nebulae – showing 95% of them were moving away from Earth at speeds up to 1500km/s. General Relativity. Different Model Universes. - PowerPoint PPT Presentation
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Slipher’s Spectra of Nebulae Lowell Telescope – near Flagstaff Arizona –provided spectra of ~50 nebulae – showing 95% of them were moving away from Earth at speeds up to 1500km/s Iron IronScandium Sodium Iron Iron Scandium Sodium
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Page 1: Slipher’s Spectra of Nebulae

Slipher’s Spectra of Nebulae

Lowell Telescope – near Flagstaff Arizona –provided spectra of ~50 nebulae – showing 95% of them were moving away from Earth at speeds up to 1500km/s

Iron Iron Scandium Sodium

Iron Iron Scandium Sodium

Page 2: Slipher’s Spectra of Nebulae

General Relativity

Page 3: Slipher’s Spectra of Nebulae

Different Model Universes• 1917 Einstein’s Cosmological Constant

Universe• 1916, 1920 de Sitter’s Empty Universe

Solutions predicted spectra shift• 1922 Friedmann showed family of

solutions based on homogenous isotropic Universe.

• 1930 Einstein de-Sitter Flat Universe• 1936 Robertson-Walker Solutions

Page 4: Slipher’s Spectra of Nebulae

Hubble’s Discovery of the Expanding Universe

•1926 Hubble measuring average space density of Galaxies to look at effects of Curvature using static Universe solutions

•1927 Lemaitre showed Hubble Law (velocity proportional to Distance) expected of Friedmann Universes, and demonstrated, using Hubble’s/Slipher Data the Law in nature. Noted age of Universe roughly 1/Hubble Constant

•1928 Robertson predicts linear relationship and claims to see it in plot of Galaxy brightness versus Slipher’s redshift

•1929 Humason announces velocity of NGC 7619 of 3779 km/s

•1929 at National Academy of Science Hubble presents paper announcing Universe is Expanding

•1929-1931 Hubble/Humason extend relation to 20000 km/s

Page 5: Slipher’s Spectra of Nebulae

1000 km/s

Assuming brightest stars are standard Candles

2 Mpc

H0=500 km/s/Mpc = 2 Gyr-1

Page 6: Slipher’s Spectra of Nebulae

Lemaitre – The unsung hero

• Fought for Belgium starting at 14 in WWI• Seminary in 1923, ordained as a priest• 1923 Visited Eddington in Cambridge England • 1924 Visited Harlow Shapley in Cambridge, Mass• 1925 enrolled in PhD at MIT, but returned to Brussels to work

on it.• 1927 published “homogeneous Universe of constant mass

and growing radius accounting for the radial velocity of extragalactic nebulae”– Independently derived Friedman Equations– Suggested Universe was expanding– Showed it was confirmed by Hubble’s data.

Mathematics accepted by Einstein, but basic idea rejected by Einstein

• 1931 Discussed primeaval atom which everything grew out of – the Big Bang

Page 7: Slipher’s Spectra of Nebulae

Newtonian Cosmology

Page 8: Slipher’s Spectra of Nebulae

Apply Gauss’ Law:

Since this holds for any sphere, there is a solution for all spheres, M=0

So need to fake it: Lets assume that all forces cancel out, outside the sphere, and we only have to worry about those forces inside the sphere.

GM

r2ˆ r ⋅∫ dA =< g > A = 4πGM

Page 9: Slipher’s Spectra of Nebulae

r

v=H0r

Page 10: Slipher’s Spectra of Nebulae

• Within shell of radius r,

– Note as time moves forward, galaxy moves out, (r increases), but Mass “affecting” object is constant.

– Equation of Motion for any Galaxy

30 3

4rM πρ=

constant2

1 2 =−=r

GMmmvE

Page 11: Slipher’s Spectra of Nebulae

Critical Universe

• E=0

( )

critG

H

r

rGrH

r

GMmmv

ρπ

ρ

πρ

≡=

=

=

8

3

34

2

1

2

1

20

3

20

2

Critical Density defines line between bound and unbound Universe. Density higher than this, Universe has negative Energy – Bound, lower than this, Universe has positive Energy - Unbound

The density changes in time, so v=H(t)r

Page 12: Slipher’s Spectra of Nebulae

Motion of Critical UniverseDefined boundary

condition t=0, r=0

Age of Universe:

Page 13: Slipher’s Spectra of Nebulae

General Equation of Motion (non-critical case)

( )

200

20

03

02

200

20

0

03

02

000

2

3

4

234

2

1

3

4

2

34

2

1 at

2

1

rGH

r

rG

dt

dr

rGH

mK

r

mrGrHmKt

Kr

GMmmv

⎟⎟⎠

⎞⎜⎜⎝

⎛−=

⎟⎠⎞

⎜⎝⎛

−⎟⎠

⎞⎜⎝

⎟⎟⎠

⎞⎜⎜⎝

⎛−=

−=

=−

ρπρπ

ρπ

ρπ

M is constant as seen by our galaxy, so I have usedthe current epoch expression for M for all times r.

Page 14: Slipher’s Spectra of Nebulae

non-critical case, cont

( )0*

0

2

*

*

20

002

0

0

2

*

*

200

2002

00

2

*

*00

200

20

03

02

*

*00

00*

*

*

*

0*

*

0

*

20

0000*

0*

1D

3

81

3

8

3

4

23

4

2

1

3

4

234

2

1

1

1

1

1

3

8

Ω−=Ω

−⎟⎟⎠

⎞⎜⎜⎝

⎟⎟⎠

⎞⎜⎜⎝

⎛−=−⎟⎟

⎞⎜⎜⎝

⎟⎟⎠

⎞⎜⎜⎝

⎛−=⎟

⎞⎜⎝

⎛−⎟⎟

⎞⎜⎜⎝

⎟⎟⎠

⎞⎜⎜⎝

⎛−=

⎟⎠⎞

⎜⎝⎛

−⎟⎠

⎞⎜⎝

=

==

==

==Ω==

τ

ρπρπ

τ

ρππρτ

ρπρπ

τ

ττ

τ

ρπ

ρ

ρτ

d

dD

H

G

r

r

H

G

d

dD

rGH

r

rrG

d

dDHr

rGH

r

rG

dt

dr

d

dDHr

dt

dr

Hdt

dr

rd

dt

dt

dr

dr

dD

d

dD

Hd

dt

rdr

dD

H

GtH

r

rD

crit

Substitution to simplifyThis ODE

Page 15: Slipher’s Spectra of Nebulae

dD*

dτ *

⎝ ⎜

⎠ ⎟

2

− Ω0

D*

= 1− Ω0( )

Again define variables to solve this ODE

ξ =1− Ω0

Ω0

D* τ =1− Ω0( )

3 / 2

Ω0

τ *

dτ=

dD*

dD*

dτ *

dτ *

dD*

=1− Ω0

Ω0

, dτ *

dτ=

Ω0

1− Ω0( )3 / 2

dτ=

1− Ω0

Ω0

dD*

dτ *

Ω0

1− Ω0( )3 / 2

dD*

dτ *

=dξ

dτ1− Ω0( )

1/ 2

⎝ ⎜

⎠ ⎟2

1− Ω0 − Ω0

1− Ω0

ξΩ0

= 1− Ω0( )

⎝ ⎜

⎠ ⎟2

−1

ξ=

1− Ω0( )1− Ω0

= ±1

Page 16: Slipher’s Spectra of Nebulae

⎝ ⎜

⎠ ⎟2

=1

ξ±1

dτ = dξξ

1± ξ

τ = dξξ

1± ξ0

ξ

final substitution! for Bound (-) case

ξ = sin2(η /2) =1

21− cosη( )

dξ = sin(η /2)cos(η /2)dη

τ = sin(η /2)cos(η /2)dηsin2(η /2)

1− sin2(η /2)0

η

τ = sin(η /2)cos(η /2)dηsin2(η /2)

cos2(η /2)=

0

η

∫ sin2(η /2)dη

τ =0

η

∫ 1

2−

1

2cosη

⎝ ⎜

⎠ ⎟dη =

1

2η −

1

2sinη

⎝ ⎜

⎠ ⎟

Page 17: Slipher’s Spectra of Nebulae

Final Parametric Solution

( )

tH

r

r

00

2/3

0

00

0

1sin

2

1

2

1

1cos1

2

1

Ω

Ω−=⎟

⎞⎜⎝

⎛−=

Ω

Ω−=−=

ηητ

ηξ


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