mini review of where we’ve come from: cmb, sne ia, and clusters tell us the universe is mostly...

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Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM Escape Equation and adiabatic expansion show how why we want to measure H, m , , plus how k, R, t, etc are all related. Didn’t derive how t depends on m , , etc, did argue by units

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Page 1: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Mini review of where we’ve come from:

CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Escape Equation and adiabatic expansion show how why we want to measure H, m, , plus how k, R, t, etc are all related.

Didn’t derive how t depends on m, , etc, did argue by units that 1/H gives approximate age

Page 2: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Defined de-acceleration parameter = as /2 for = 0, matter dominated era, but a different physical concept.

Showed static universe naturally requires dark energy. This gives a negative pressure for positive matter and k = +1. We can see from dU= -pdV this causes expansion

From de-acceleration definition and that q = m/2- for measured values of and m we can see the universe is accelerating today

Page 3: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• Big Bang pretty good

• BB was invented to explain several things

• We know we need more (CDM and ) but

• There’s more:

• Inflation is needed ( maybe, you be the judge)

Page 4: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Classical BB was based on laboratory (confirmed) physics.

Do next. We can use R(t) and t versus 1+z and T = T0(1+z), I never proved in detail: comes from radiation density (r) proportional to T4 and r goes as r0(R(t0)/R(t))4

Also use = o(R(t0)/R(t))3, for matter

Page 5: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• First a review of what BB does explain• And how• We will put in detail!• Logical progression from the escape equation math

Page 6: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

The Big Bang “Explains”

• Why the sky is dark at night (Olber’s paradox).

• Why the Universe is old.

• Why the Universe is mainly hydrogen and helium.

• The existence of the CMB.

• That the Universe is expanding.

Page 7: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Olber’s Pardox

• If the Universe were infinite

• AND UNEVOLVING

• uniform in density of stars (or galaxies)

• then we would be “burned to crisp.”

• From simple geometry:

• The apparent brightness of objects falls off as one over the distance squared.

Page 8: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Olber’s Pardox, cont.• Number of objects per unit volume in a shell at a

distance goes as the distance squared.

• Exactly cancels the one over distance squared dimming of an individual star or galaxy.

• The sum of all the brightness adds to infinity if

the Universe is static, un-evolving, uniform in density, and infinite.

Page 9: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Olber’s Pardox, cont.

• The BB defeats Olbers Paradox by

• Expanding universe

• Star formation had a beginning.

• Stars to evolve.

• Expansion is not necessary, however, only that stars live for a finite time is.

Page 10: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• The BB says the Universe expands

• And we observe expansion

• Our models with the escape equation give expansion

• The observation of distant objects plus (time it takes light to travel implies a large age)

• The CMB (universe has been cooling) fits with expansion model and observations

• Model says the Universe is about 15 billion years old.

Page 11: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

BB “Explains” Hydrogen & Heliumso called BB Nucleo-synthesis • The Big Bang starts the Universe off with

a “hot” big bang!

• The initial universe was then hot and dense in the first 3 minutes (or so) to “burn” (fuse) hydrogen into helium.

• Expansion prevented heavier elements from being formed in any significant quantities.

Page 12: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• Universe in first 3 minutes not too hot to break up He and not too cold or under dense to fuse H into He.

• Works if we start at 1 second with a “reasonably” high T (about 1 million K).

• We can estimate this T and density () by extrapolating back from the “brick wall”

• know T, , 1+z of brick wall when becomes transparent from “simple” atomic physics

Page 13: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• 1+z = R(t0)/R(t)

• t = AR(t)2; A = constant

• applies in radiation dominated era

• about 100,000 years before brick wall becomes transparent.

• know t, know T at brick wall transparent

• Extrapolate back to t = 1 second

• using T =T0(1+z) => at 1 second

• T ~ 1 million K , OK!

Page 14: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• We also know the physics of radiation , matter etc. well enough to do this back to 1 second, at least. See the book, page 376, figure 13.7

• Key “players” are protons, neutrons, electrons and neutrinos.

• Neutrons decay into protons, electrons, and neutrinos.

• the reverse can happen as long as the temperature and density are high enough.

Page 15: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• => density and temperature fall and a “significant” number of free neutrons have decayed, the fusion process halts.

• Half of all of free neutrons will decay in about 10.6 minutes

• Net effect is that after about 3 minutes process stops

• The higher the density, the higher the probability the neutrons and protons will join up and eventually make He.

Page 16: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• An intermediate step join of proton to neutron = “deuterium” = D.

• The “simple” process is then p + n => D

• D + p => “light” He (with only 1 neutron) written 3He.

• 3He + 3He => 4He (ordinary, super stable helium) + stuff

• The denser the material, the more D is burned into He at faster rate than D is made.

Page 17: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

Baryonic matter

Page 18: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

=> Higher He/H tracks with lower D/H

Page 19: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

The Net Result cont.:• => A measure of the ratio of He/H and or D/H

is the most direct method we have of determining b.

• Therefore a major goal of some people is to go out and measure these quantities while others make sure the theory is correct.

=> A measure of the ratio of He/H and or D/H is the most direct method we have of determining b.

Page 20: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

How to win a Nobel prize in Physics:

• Find relic neutrinos from left over n decay

• n -> p + e + e

• Good luck, terribly difficult (why hasn’t been done!)

Page 21: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• Neutrinos are so penetrating that

• IF we could detect them

• we could see back to about the 1st second

• Very exciting

Page 22: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

• The BB model then starts out hot and dense to explain He/H and D/H.

• The Universe expands and cools until the “brick wall” becomes transparent.

• => What is the brick wall made of and how to we predict transparency?

• The brick wall is mainly hydrogen gas but before it becomes transparent, the hydrogen is nearly totally ionized.

• Electrons and protons are free of each other in a ‘weird” state we call a “plasma.”

Page 23: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

The CMB more details now:• As the Universe expands,

• Both the hydrogen gas and the photon gas cool.

• If hot enough, the photons can separate electrons from protons that might have joined together to make ordinary hydrogen gas.

• And at the same time electrons are very efficient at absorbing or scattering photons.

• So the photons can’t travel far and we have “brick wall.”

Page 24: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

The CMB more details now:• Eventually, however, the gases (photons,

electrons, and protons) cool so much

• that the photons don’t have enough energy to free “bound” (to protons)

• not enough to even to “excite” the atom by being absorbed. (Nature has “conspired” so that electrons can only circle the proton in certain specific orbits and if there isn’t enough energy for an “orbital transfer”, the photon can’t be absorbed be the atom.)

Page 25: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

The CMB more details now:• So gases cool down to point where hydrogen

becomes “atomic” hydrogen and the gas “suddenly” becomes transparent. The photon gas then streams away on its own to reach us today as the CMB.

Page 26: Mini review of where we’ve come from: CMB, SNe Ia, And Clusters tell us the universe is mostly dark energy and will expand forever. Plus that we need CDM

The BB doesn’t really say why started out hot or expanding but:

• The model is consistent with this much of the data.

• Using only laboratory physics

• We already know some problems: smoothness of CMB, CMB fine structure, SNe Ia, and clusters. But some say we need more => enter Inflation: