Science Facts

Is The Sun Solid Liquid Or Gas? – Sun Secret Reveal

Sun's State

The Sun is a medium-sized star at the center of the solar system and one of the hundreds of billions of stars in the Milky Way galaxy. It’s estimated to be about 4.6 billion years old, and its energy drives Earth’s climate and weather. The Sun also supports almost all life on Earth through photosynthesis, which plants and other organisms used to convert light energy captured from the Sun into chemical energy. It is a near-perfect sphere of scorching hot hydrogen and helium.

Communications on earth scientists believe the Sun has enough nuclear fuel for another 5 billion years. After that, the Sun will begin to burn helium and expand a hundred times its current size swallowing the earth. It’s believed the red giant Sun will burn for another billion years and then collapse into a white dwarf about the size of Planet Earth. The state of the sun is still debate. It looks like a solid from the earth, liquid from a telescope, and gaseous or plasma form scientifically.

Is the sun solid, liquid, or gas?

The sun is neither a solid nor a liquid. It’s gaseous and plasma! But there are a lot of arguments about the gaseous sun which can not be negligible. The body-centered cubic structure of the Sun’s core region comprises type 2 metallic hydrogen, a compress. And therefore, more metallic hexagonal planar structure.

Type 1 and type 2 metallic hydrogen can be viewed as a one-component plasma wherein the protons are restricted to their lattice points. The electrons are freely delocalized. In the liquid metallic hydrogen model of the Sun, there is no radiative zone that had characterized the standard model. In the standard model, the Sun seems like a fully compressible ideal gap. It has no actual surface since gases are not known for their surface-forming abilities.

  • The sun is made of 91.0% hydrogen and 8.9% helium. By mass, it is about 70.6% hydrogen and 27.4% helium.
Sun structure

The sun has 5 main zones: core, radiative zone, convection zone, photosphere, and chromosphere.

Core

In this model, the central core of the Sun is believed to have a density approaching 150 grams per centimeter cube and reaches temperatures of 50 million Kelvin degrees. The density of the outer core is said to be about 20 grams per centimeter cubed. It is important to note that astronomers know that the Sun’s core undergoes solid-body rotations from helioseismic studies. Gases cannot rotate in that way.

In the standard model, the core is the region where nuclear reactions take place. The Sun is limited to obtaining its vast majority of energy by directly converting hydrogen to helium. But a small amount of helium arises through intermediates, including beryllium, boron, and lithium. In all these cases, though, the end product is helium.

The Sun is unable to synthesize elements beyond the lightest, focusing only on the synthesis of helium. In this way, modern solar Theory has crippled Sun because it can’t make any heavy elements. These are the first-generation stars. Since the core is proposed to be nuclear reactions, it emits light as gamma and X-rays, which are very high frequency. After gamma and x-rays are emitted by the solar core, they are believed to enter the radiative zone, where they are repeatedly scattered, absorbed, and re-emitted.

Radiative zone

The radiative zone extends from just above the core to the next zone and is said to have a density of about 20 grams per centimeter cubed to 0.2 grams per centimeter cube. And a temperature ranging from 7 million degrees to 2 million degrees Kelvin. After millions of years in this zone, the trap photons finally emerged. However, their constant interaction with interstellar matter, their frequency is said to have slowly decreased, shifting from the x-ray range to the optical.

Convective zone

As photons progress towards the surface of the Sun, they pass through the convective zone. From helioseismic measurements, the convective zone begins about 200,000 kilometers below the solar surface. It is said to have a temperature of 2 million Kelvin degrees in the standard model. It is the region of the Sun where convection currents act to transport solar energy from the top of the radiative zone to the photosphere. Nests in between the radiative zone and the convective zone, we find the tackle line layer. Once again, based on helioseismology, this is known to be a region of high shear forces within the Sun.

The mere existence of a tack-aligned layer is sufficient evidence that the Sun’s body cannot be gaseous. Different star types differ from the Sun by the size and content of their core, radiative, and convective zones.

Photosphere

In the standard model, the photosphere has a temperature of about 5700 degrees Kelvin with an extremely low density of only two times 1e-7 grams per centimeter cubed. This density is lower than those made in a laboratory vacuum. Once photons cross the photosphere, they make their way into outer space.

Chromosphere

The chromosphere is around the photosphere, with the calculated density in the standard model of about 1e-12 grams per centimeter cubed. And a temperature slightly below the order of the photosphere. That density is one 100,000 of the density of the photosphere. Then comes the hypothesized transition zone. Here, the outer solar atmosphere temperature rapidly increases from about 10,000 Kelvin degrees to nearly 1 million Kelvin degrees. The density of the outer atmosphere can drop to less than one million of the value of the level at the chromosphere.

Corona

In the corona, the temperature is thought to reach millions of degrees, according to modern theory. Corona is known to be associated with the production of emission lines. Given rising to the corona in the standard model. It is interpreted as the result of the strange heating of the corona to millions of degrees. This increases temperature with elevation above the solar surface because gases can only produce emission lines via heating in this model. Still, that conjecture is not reasonable and violates thermodynamic laws.

The liquid metallic hydrogen model explains these emissions by invoking the high electron affinity of metallic hydrogen in the corona. When free atoms interact with this material, they are stripped of many electrons, resulting in a highly ionized species. This mechanism allows the corona to harvest electrons and maintain the electrical neutrality of the solar body.

Sun’s state explanation

In the standard model, the Sun is viewed as a fully compressible object. And it is treated mathematically using the ideal gas law. This expression was first obtained by observing gases in containers.

Ideal gas law, PV = nRT

In this equation, P represents pressure, V is the volume, the number of particles expressing moles (n) is the gas constant, and T is the temperature. Fixing the number of moles and the temperature makes the right-side constant. In that case, increasing pressure will result in a decrease in volume. While increasing volume decreases pressure. Now the problem with utilizing the ideal gas law to treat the interior of a gaseous Sun is relatively easy to explain. How do we define pressure? It’s the amount of force applied to a given area. For instance, its units are often expressed as pounds per square inch or Newton’s per square meter.

Unfortunately, in the gaseous model of the Sun, there are no actual surfaces by which pressure can even be defined. There is no area in the force over area definition of pressure, making the ideal gas law unusable. Astronomers use imaginary surfaces in their models to skirt around this problem. But as will be seen below, this is not a solution.

Homer Lane ignored this problem and applied the ideal gas law to the Sun in 1870. If the Sun truly has an entirely gaseous interior, there are two problems.

  • First, how do astronomers prevent the Sun from collapsing on itself.
  • Secondly, how does a gaseous Sun maintain a stable radius.

Remember that the rule in the laboratory is that a gas expands to fill the void, yet the Sun is stable. So how is that achieved if the Sun is truly a gas?

Astronomers solved the stability problem by invoking a principle called hydrostatic equilibrium. It constitutes a balance between gravity gas pressure and radiation pressure. The birth of the standard model begins by considering gravity. Most of us recognize that there is more gravity on the earth than on the moon. We have all seen movies of Apollo astronauts bouncing around while they gaze at the earth.

The Sun has a great mass of two times 10 to 30 kilograms. That’s more than 300,000 times the mass of the earth. The Sun is also unbelievably big. Inside its volume defined by the photosphere, one could fit over 1 million earth. Despite its huge mass and volume, it is interesting to highlight that our star has a very ordinary density of only 1.4 grams per centimeter cube. It is close to the density of water at 1 gram/centimeter cubed and about 1/4 of the density of the earth.

Given the Sun’s mass, it is not too much to believe that the service gravity of our star is nearly 30 times what we experience here on earth. Astronomers argue that the inward-directed force of gravity within each star is counterbalanced by externally directed gas pressure and radiation pressures. When all these forces balance, we have hydrostatic equilibrium.

  • For a start, the size of Sun theory suggests a gas pressure produced by electrons primarily acts to oppose the force of gravity. Within giant stars, however, radiation pressure becomes dominant.

What is gas pressure? First, think about the 5 layers of atmosphere above the earth. Gas pressure supports the atmosphere. As you remember from earlier, pressure is equal to force over area. Gas pressure is generated when an atom in our atmosphere strikes the surface of the planet. At that point, much like a billiard ball, it bounces off the surface and is redirected upward. The net result is that any movement of an atom downward immediately transforms upward. To generate atmospheric gas pressure, we needed an actual surface. However, in a standard model of the Sun, there is no surface!

LV Faye was the first to deprive the Sun of an actual surface when he argued in 1865 that it was only apparent. He could not do otherwise, given that he was promoting a gaseous solar body. Today astronomers tell us that the surface of the Sun is nothing but an optical illusion. Given the theory that the Sun is just a ball of gas, they had no choice.

The real fact about Sun

Gases can never have an actual surface. But if the Sun has no surface and its interior is entirely gaseous, how could it generate gas pressure. After all, the only surfaces inside a gaseous Sun are imaginary. Clayton uses an imaginary surface to argue that the Sun’s interior can support electron gas pressure. The problem, of course, is that imaginary surfaces are actual. Some insight into this question can be gained by returning to the billiard table.

For example, Suppose you have some ball, and each ball represents a gas particle. The bank of the table is an actual surface. The angle at which the cue ball strikes the bank will be equal to the angle it leaves. There can be a complete reversal of direction. But if the cue ball hits another ball, it will transfer momentum to the second ball and remain stationary after impact. This example makes it easy to say why particles within a gaseous Sun could never act as an actual surface.

Clayton’s imaginary surface cannot be used to justify gas pressure in the Sun. When a particle moves downward towards an imaginary plane, it will not change direction upon reaching it. Imagine a particle on the Sun moving downward and hitting another particle. It can simply push the second particle deeper into the solar body. This collision does results in a downward force, not an upward one. There can be a complete transfer of momentum with no change in direction. Conversely, the opposite can be argued if the particle was initially moving upward. It is impossible to generate net gas pressure inside an object like a gaseous Sun. No surface, no pressure.

In fact, if one adds the force of gravity, gas-particle movements inside a gaseous Sun are more likely to generate solar collapse rather than a stable structure. Consequently, astronomers cannot justify electron gas pressure as a component of hydrostatic equilibrium within the Sun.

Then we come to radiation pressure. The escape of a photon from the Sun’s center involves millions of years of bouncing around within the interior. In a vacuum, light moves at 3 times 10 to the 8th meters per second. That’s a lot of speed. To place everything in perspective, the width of the entire Milky Way galaxy is 100,000 light-years. It is assuming a light speed in a vacuum. It means that the standard model requires some of the light to travel ten times the diameter of the galaxy of which the Sun is only a speck before escaping. But one of the biggest problems is invoking internal radiation in the first place.

Last words

On earth, objects strive for internal thermal equilibrium using conduction and convection, not radiation. Radiative processes are reserved for reaching equilibrium with the outside world. Consequently, the standard model of the Sun suffers from two flaws.

  • Gas pressure cannot exist in the absence of an actual surface, and there are none within a gaseous Sun.
  • Objects on earth do not use radiative processes in trying to achieve internal thermal equilibrium.

Conduction and convection are reserved for this situation.


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Sources:

Tobias, S.M. (2005). “The solar tachocline: Formation, stability and its role in the solar dynamo.” In A.M. Soward; et al. (eds.). Fluid Dynamics and Dynamos in Astrophysics and Geophysics.
Mullan, D.J (2000). “Solar Physics: From the Deep Interior to the Hot Corona.”
Abhyankar, K.D. (1977). “A Survey of the Solar Atmospheric Models.” Bulletin of the Astronomical Society of India.”Solar.” Oxford English Dictionary (Online ed.). Oxford University Press.
Pitjeva, E. V.; Standish, E. M. (2009). “Proposals for the masses of the three largest asteroids, the Moon–Earth mass ratio and the Astronomical Unit.” Celestial Mechanics and Dynamical Astronomy.

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