Saturday, April 12, 2014

beginning with a Universe?

-  1672  -  Beginning with a Universe.  Really, how did it all start?  Where did we come from?  How long will it last?  Astronomy looks back in time to get the answers.
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---------------------  -  1672  -  Beginning with a Universe.
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- Everyone knows now about the Cosmic Microwave Background radiation that has a temperature of  2.75 degrees Kelvin everywhere and in all directions.  It is a release of photon radiation from the charged plasma of the Big Bang.  After 370,000 years of expansion and cooling  the radiation could finally escape the charged plasma.  A picture of the CMB is literally a picture of the birth of the Universe.  The hot and cold patches across the CMB are the galaxy clusters and the voids in space we see today, 3,725,000,000 years later.
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-.  Prior to the CMB release the charged plasma of positive protons and negative electrons scattered the photons to such a great extent they bounced around without escaping.  When the plasma cool down to 3,000 degrees Kelvin the protons captured electrons forming neutral hydrogen.  Now the photons could escape the opaque expanding cloud leaving the pattern, the CMB, that existed at that time
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-.  Going back even further in time, earlier than one microsecond, protons and neutrons could not exist because the temperature was so hot that only the fundamental particles Quarks, leptons, photons, V and Z  bosons, and gluons made up the plasma of charged particles..
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-.  Today, thanks to the Planck Telescope, launched in May, 2009, the resolution of this picture has increased to 50 million pixels.  This radiation is 13,725,000 000years old.
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-.  The CMB picture appears as uniform radiation.  But, the high-resolution uncovers tiny, millionths of degrees changes from cooler to hotter spots.  The angular separation of these spots are the result of sound waves that existed in the plasma.  The cold spots eventually collected under gravity’s attractive force and became galaxies.  The spot’s cycle today have a wavelength of 450 million light-years.
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-.  By decoding this soundwave into its fundamental and harmonic components astronomers are able to conclude that the expansion force is 68.3 % of the Cosmos in total mass-energy.  And , that matter, the attractive gravity force, makes up the other 26.8 %.  Most of this is Dark Matter because Ordinary Matter that makes up our world is only 4.9 % of this total mass- energy.  The density of Deuterium implies that Ordinary Matter amounts to only 4.9 percent of the total mass-energy density in the Universe.
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-.  100,000,000 years after the Big Bang the universe was 5 parts Dark Matter and 1 part Ordinary Matter, almost entirely hydrogen and helium.   When the first stars formed they were giant stars, > 100 Solar Mass.  At a Redshift of 1,100 we see the Universe when it was 380,000 years old and had a temperature of 3,000 Kelvin.
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-.  Today the Dark Energy is pulling the Universe apart at an ever accelerating rate.  Eventually all matter and energy will be so diluted the Cosmos will end up cold and dark.  But, that will be several billion years from now.
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-.  The radiation has been traveling over billions of light-years.  Gravity bends light.  By analyzing  gravitational lensing effects astronomers can map the distribution of matter in the Universe over this time span.
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-.  The radiation does not oscillate in random directions.  The light is polarized.  When the polarized radiation strikes electrons it scatters in the” E-mode” of the polarized light.  The “B-mode” polarized orientation is more difficult to detect.  New telescopes are attempting to use these polarization parameters to learn more about the Cosmic Background and Cosmic Inflation.
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-   Light is electromagnetic radiation.  E-mode is the electric half of the wave and at right angles to it is the B-mode, magnetic wave.  Together they make one electromagnetic wavelength.  The shorter this wavelength the more energy it carries.  The longer this wavelength the less energy it carries.  The spectrum runs from Gamma-Rays, to X-rays, to Ultraviolet rays, to Blue light, to Red light, to Microwaves, to Radio waves.
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-.  Gravity is a property of space and time and not only a force described by Newton’s equation and not only a force described by Newton's equation:
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------------------  F  =  M * m * G  /  r^2
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-  The force of gravity is directly proportional to the masses and inversely proportional to the distance between them.
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-.  Gravity according to Einstein is created by space being curved by the presence of mass.  Falling objects are simply following the path of least resistance in curved space-time.
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-.  The above law for gravity works for a very good first approximation.  It uses a gravitational constant of “G” which should be the same everywhere the Universe.
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---------------------- .  G = 6.674215  * 10^-11 meters^3 per kilogram second^2
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-.  On Earth’s surface, where the distance to the center is everywhere the same, the acceleration of gravity is always and everywhere 32 feet per second per second.  Newton's equation almost always works.  You have to get down to the details to find the exception.
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-.  The planet Mercury seemed to be such an exception.  The planet’s orbit around the Sun was in the form of daisy petals instead of a simple circles.  The irregular movements were very small, 43 arc seconds per hundred years.  In 4,000 years the change would only amount to the width of a full moon.  But all the equations astronomers had to use at the time could not explain this small change.
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-.  Einstein had a new equation, the General Theory of Relativity, it worked to explain the perihelion of revolving bodies.  The perihelion is the point of orbit of a planet when it is nearest to the Sun.  His equations calculated the shift of this point to perfect accuracy.
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-.  In 1925 Einstein’s  equations were able to explain the gravitational Redshift of light leaving a massive body like a White Dwarf star.  And again his equations worked when the light from a star passed an eclipse Sun bending by 1.75 seconds of arc.
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-.  Today, astronomers measure this effect all the time as gravitational lensing.  When one star is directly behind another star, the light from the farther star is bent around the near star magnifying the image as if the light were traveling through a lens.
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-.  The equations have been proven to work over and over again in dozens of experiments.  Some more examples:
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-.  Measuring gamma rays that are Redshifted and Blue shifted with gravity.  Called the Mossbauer Effect and the Doppler-Fizeau Effect.
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-.  Measuring radar beams passing a planet.
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-.  Measuring binary pulsars revolving a mutual center of gravity.
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-.  The Special Theory of Relativity has been proven hundreds of times.  This General Theory of Relativity concerning gravity is still being contested.  We still don't understand gravity.  But , so far, Einstein’s equations remain, because they work, even though we are not sure why.
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-  (1)  Other Reviews on Relativity:  1662, 1663,  1582,  874,  768,  766,  648,  550.
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-.  (2)  Calculus is math to measure anything that changes.  That is most everything.  Derivatives are calculus math to calculate how fast things change.  Integration  calculus  are mathematical ways to accumulate a sum of these changes.
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-. (3)  Any plane is an infinite number of parallel lines.  Any solid is an infinite number planes.  Mathematics must systematically evolve from deductive reasoning using simple postulates to derive complex theories.  Calculus is like a cloth of woven thread and a book of completed pages.
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