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----------------------------- 2681 - PULSARS - rotating neutron stars?
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- This Neutron Star is part of a binary system. Its companion is a Red Giant star that is 1/7 the mass of our Sun. The two stars orbit each other every 26 hours.
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- The Neutron Star is spinning so fast it would fly apart except for the fact that its surface is solid and harder than a diamond. The density of the star is 50 trillion times heavier than the density of solid lead. Its magnetic field is a trillion times more intense than that of our Sun.
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- A Neutron Star is a collapsed star that no longer has any more fusion fuel to burn. It remains a hot cinder. In this case a hot spinning cinder that can not offer any radiation or resistance to the gravity that is compressing it.
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- For a normal collapsing star the size- of- our- Sun , gravity would compress it to the size of our Earth before a resistance could stop it. At this point compression would stop because the electron’s pressure to refuse to collapse any further would hold up the gravity. The star this size would remain a White Dwarf Star.
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- However, if the size of the star was 40% larger than our Sun ( >1.4 Solar Mass), then the electron’s pressure would break down. The electrons would collapse into the protons in the nucleus and become neutrons. When this happens the star collapses from Earth-size to a ball 20 miles in diameter. A Neutron Star is 20 miles in diameter and still weighing more than the Sun.
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- When this collapse is happening the spinning star is speeding up its rate of rotation. Just like an ice skater pulling in her outstretched arms speeds up her rate of spin. When a star’s diameter shrinks it spin rate goes up to maintain the equivalent Angular Momentum. This is the law of the Conversation of Energy, or , in this case the Conservation of Angular Momentum energy. This particular Neutron Star is spinning at 716 revolutions per second.
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- How does a law of conservation make a Neutron Star spin so fast? Emmy Noether proved mathematically in 1916, when she was 34 years old, that spatial symmetry ( a rotating sphere looks the same from any direction) required a law of conservation.
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- That law was the Conservation of Angular Momentum. She also proved that time symmetry, time translation, ( the law that physics is the same no matter when you apply it) required the Conservation of Energy.
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- A kitchen blender on its highest speed is rotating a hundred revolutions per second. This 20 mile diameter ball is rotating 716 revolutions per second. The equator on the ball is traveling at 43,000 miles per second. If the Earth were doing this instead of a day taking 24 hours we would have 2 days per second. How time flies.
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- Not only would you be spinning this fast standing on the equator, the gravity is so intense that your whole body would be crushed to the size of a protoplasm. You would spread across the surface of the star like a film of oil only one atom thick.
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- If life were not difficult enough under these conditions the star would be releasing quick bursts of energy with every rotation. Each flash of radiation occurs across a wide range of wavelengths. The flashes are so fast that we can not see them. The star looks like a continuous source of light. Our eyes can not separate flashes that are faster than 30 times per second, let alone 716 flashes per second.
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- The spin rate was not detected until 2004 when radio signals were analyzed. This radio signal became a flash along our line of sight because the beam axis of the jets is slightly off center from the rotation axis of the star. This causes the beam to rotate like a lighthouse beacon. Radio signals could be analyzed to pull up the repetition rate of 716 times per second.
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- For astronomy to date, this is the fastest spinning star in the Cosmos. It could not be crushed any denser without becoming a “Quark Star”. This phenomena is in theory only. Yet to be discovered. Theoretically, just as electrons give out and get crushed down to neutrons, the neutrons could get crushed down to their fundamental particles the Quarks. An announcement will be made shortly, stay tuned.
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- Angular Momentum is the product of mass and velocity and radius of a rotating body. Mass stays the same so if the radius is reduced in order for the product to remain unchanged the velocity of rotation must increase.
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--------------------------- L = m * v * r
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- If the Neutron Star has a radius of 10 kilometers and it is spinning at 716 rotations per second how big was it to start with?
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---------------- Circumference = 2 * pi * r = 2 * pi * 10 km = 62.8 kilometers
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---------------- Completing 716 rotations per second is a velocity of 44,988 kilometers per second. ( 32 million miles per hour or 5% the speed of light.)
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---------------- The mass of the Neutron Star is 2 Solar Mass = 2 * 6 * 10^24 kilograms
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--------------- The Big Stars rotation was 57 days.
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--------------- Angular Momentum = 12 * 10^24 kg * 4.5 *10^24 km/sec * 10 km
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-------------- 57 days is 4,924,800 seconds
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-------------- The velocity = 2 * pi * r km / 4.9* 10^6 seconds
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-------------- The mass stays the same, and cancel out of the equation.
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-------------- 4.5 *10^24 km/sec * 10 km = ( 2 * pi * r km / 4.9* 10^6 sec ) * r
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------------------ r^2 = 35 * 10^10 km
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----------------- r = 5.9 * 10^5 km
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----------------- r = 367,950 mile radius
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------------------ Our Sun’s radius is 432,292 miles.
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- Neutron Stars are leftovers after supernova explosions. These stars are the remnant cores of bigger stars. Stars burn their nuclear fusion fuels for millions to billions of years. Big stars burn hotter and have shorter lifetimes, maybe 10 million years.. Smaller stars like our Sun will have a lifetime of some 10 billion years.
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- When the Big Stars go supernovae they leave behind a Neutron Star that can range in mass from 0.7 to 2.7 Solar Mass. However, that mass is concentrated into a rotating sphere that is only 12 miles in diameter.
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- When the Big Star starts out it can be 8 to 25 Solar Mass, maybe even as big as 150 Solar Mass. When it runs out of fuel and implodes into a spinning Neutron Star the collapsing outer layers of the star rebound into a titanic explosion hurtling material into outer space.
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- The Neutron Star at the core spins faster in order to maintain the Conservation of Angular Momentum as it collapses to a smaller diameter. This rapid rotation generates a giant magnetic field, like an spinning electric dynamo. The magnetic field generates a current of charged particles that escape out the magnetic poles.
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- Often the beam of particles are offset from the rotational axis causing the beam to rotate like a lighthouse beacon. When the beam flashes across our field of view we call it a “Pulsar”.
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- Only 8 supernovae explosions have been recorded witnessed by the naked eye. One was recorded in August 7, 1181 that lasted for 156 days before becoming too faint for the naked eye. This supernova was designated 3C58. Compared to the Crab Nebula supernova that was witnessed beginning July 4, 1054, 3C58 is 2,000 times weaker in the X-ray spectrum even though the X-ray nebula is several time larger than the Crab.
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- It was difficult to find the point source Neutron Star at the center of the nebula. On March 28, 2001 astronomers finally measured the period of this Pulsar at 65.7 milliseconds. This is roughly twice the period of the Crab Pulsar witch is 30 milliseconds. The luminosity was measured at 100,000 Solar Luminosity. The magnetic field was 10 trillion Earth’s magnetic field ,but , about the same as the Crab’s.
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- The spin rates of Pulsars slow down as the drag of the strong magnetic fields causes a loss of spin energy. The initial spin rate of the Crab was 19 milliseconds. For 3C58 it was 60 seconds.
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- Our Sun’s nuclear fusion creates a surface temperature of 5,800 Kelvin. Temperature is the vibration of atoms and this temperature has a vibration emission wavelength of 500 nanometers, the wavelength of yellow light.
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- Neutron Stars have a different source of energy since they no longer have nuclear fuel. Their spinning magnets generate electric fields that are up to 1,000 trillion volts at the poles. The charged electrons and anti-electrons spiral around these electric field lines.
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- The constant acceleration of charged particles creates a continuous radiation, called “synchrotron radiation“. In the beginning this energy crates a surface temperature on the Neutron Star of 1,000,000,000 Kelvin. The Neutron Star cools down as it radiates its energy away.
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- After 100 years the surface temperature is still 3,000,000 Kelvin. Escaping neutrinos carry way energy as well as the synchrotron radiation. 3C58 is 820 years old and its surface temperature has cooled to 1,400,000 Kelvin.
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- Neutron Stars are so dense because they are collapsed atoms. A hydrogen atom can be compared to a nuclear pea orbited by an electron 200 feet away. Most of the atom is empty space.
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- When the Neutron Star is formed this empty space is collapsed as the electron collides with the proton at the nucleus forming a neutron. When the electrons and protons combine neutrinos are emitted carrying away energy. 80% of the star’s mass is these neutrons with maybe 20% remaining electrons and protons in the outer layers.
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- The calculations for 3C58 observed temperatures do not match up with the scenario described above. Something else is going on. Possibly neutrons are breaking down into individual quarks.
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- Possibly other particles are being created and need to be part of the calculations. Possible particles are up-down-strange quarks creating “ lambdas”. Up-quarks and anti-quarks are creating “pions”. Up-quarks and anti-strange quarks are creating “kaons”. All of these exotic particle creations could increase the stream of neutrinos carrying off more energy and cooling the Neutron Star faster.
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- More discoveries are needed to tell us what is going on inside the Neutron Stars. 3C58 has given us more data, but, we need more. An announcement will be made shortly, stay tuned.
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- Emmy Noether born 1882 to a math teacher in Nazi Germany. She was not allowed go to school or later to teach in Germany because she was a woman and a Jew. She learned on her own auditing her father’s classes. She wrote the laws of conservation in 1916.
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- Albert Einstein helped to get her through immigration into the United States, out of Nazi persecution. She taught math at a girls school in Pennsylvania. Died in 1935 of ovarian cancer. She was one of the very first women scientists. She discovered one of the most powerful laws in all of physics.
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- Other Reviews available:
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- 2659 - PULSARS - rotating Neutron Stars? - Pulsars are rapidly rotating, highly magnetic compact stars. The rotating magnetic field of a pulsar acts as a generator, accelerating energetic charged particles that then stream along the field lines.---------- This Review lists 13 more reviews available all about pulsars.
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- 2602 - PULSAR - spinning Neutron Star? - Pulsars were discovered more than 50 years ago as beacons of stars that have collapsed into dense cores, behaving unlike anything we see on Earth. For decades, scientists have been studying pulsars in the hopes of getting a better understanding of their inner workings.
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- 1897 - The mysterious Neutron Stars, Pulsars, and Quasars create radio bursts of energy that astronomers are still trying to explain.
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- 1327 - Neutron Stars - The surface is solid and harder that a diamond, 50 trillion times denser than solid lead. Its magnetic field is a trillion times more intense than that of our Sun.
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- 1273 - Neutron Star mergers.
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- 1192 - The new zoo of Pulsars.
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- 642 - Neutron Stars, Pulsars, and Magnetars.
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- 861 - Cannon Ball Stars
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- 625 - Neutron Stars.
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- 21 - Stars grow old.
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- March 27, 2020 1327 1331 2681
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--------------------- Friday, March 27, 2020 -------------------------
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