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I would also think that this heliosphere loops back into itself at the solar poles similar to what the Earth's magnetosphere does. Energy that is thrown out from the Sun, hits the interstellar medium at the bow shock and then flows back around towards the Sun's poles.
Originally posted by XPLodER
Area of circle 1 = 1 dia = volume 0.5235987756
Area of circle 2 = 2dia =volume 4.188790205
Area of circle 3 = 3 dia =volume 14.13716694
Let's look at the area of interest in this diagram, the red area between the bodies:
Originally posted by XPLodER
And your latest reply describes an expansion of plasma moving through space, NOT an expansion of 3 dimensional space that the bodies reside in, right?
Originally posted by XPLodER
But the process in space is not expansion of gas but an expansion of 3 dimensional space that the bodies reside in.
Let's look at the area of interest in this diagram, the red area between the bodies:
OK based on this example, when dealing with a planet like the Earth, the leading edge (closest to the sun) is at 93,000,000 miles, and the trailing edge of the Earth is 8000 miles further, say 93,008,000 miles. So the expansion of the solar wind sphere can be calculated using those two radii. That's not much expansion, and that's all the expansion there is in the red area in your diagram, right?
radial definition
ra•dial (rā′dē əl)
adjective
1.
a. of or like a ray or rays; branching out in all directions from a common center
b. having or characterized by parts that branch out in this way
2. of or situated like a radius
3. ANAT. of or near the radius or forearm
Eddy diffusion
From Wikipedia, the free encyclopedia
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Eddy diffusion, eddy dispersion, or turbulent diffusion is any diffusion process by which substances are mixed in the atmosphere or in any fluid system due to eddy motion.[1][2] In another definition[3] it is mixing that is caused by eddies that can vary in size from the small Kolmogorov microscales to subtropical gyres.
Because the microscopic processes responsible for atmospheric mixing are too complex to model in detail, atmospheric modelers generally treat atmospheric mixing as a macroscopic "eddy" diffusion process. In this approach, the diffusion rate at each pressure level is parameterized by a quantity known as the eddy diffusion coefficient, K[4] (also sometimes called eddy diffusivity).
References
Originally posted by XPLodER
The expansion of area from 1Au to 2Au is an 7 fold “expansion” of area in all directions simultaneously “3 dimentional” expansion refers to the area “expansion” not just “radially”
I read the wiki and it lists the termination shock, is that what you're talking about?
Originally posted by XPLodER
edit to add the amount of expansion is not local to the "diameter of the earth"
the expansion happens from 0Au to 10Au
so at the 10Au point (approx)
the eddy currents have become so diffuse themselves they can no longer "support" the expansion of area and the three dimentional expansion comes to an ubrupt halt difusing at a boundry we know as the helio shock boundry
So 75 to 90 AU is a lot further than 10AU if that's what you mean.
The termination shock is the point in the heliosphere where the solar wind slows down to subsonic speed (with respect to the star) due to interactions with the local interstellar medium. This causes compression, heating, and a change in the magnetic field. In our solar system the termination shock is believed to be 75 to 90 astronomical units[7] from the Sun.
Originally posted by Arbitrageur
I read the wiki and it lists the termination shock, is that what you're talking about?
Originally posted by XPLodER
edit to add the amount of expansion is not local to the "diameter of the earth"
the expansion happens from 0Au to 10Au
so at the 10Au point (approx)
the eddy currents have become so diffuse themselves they can no longer "support" the expansion of area and the three dimentional expansion comes to an ubrupt halt difusing at a boundry we know as the helio shock boundry
en.wikipedia.org...
So 75 to 90 AU is a lot further than 10AU if that's what you mean.
The termination shock is the point in the heliosphere where the solar wind slows down to subsonic speed (with respect to the star) due to interactions with the local interstellar medium. This causes compression, heating, and a change in the magnetic field. In our solar system the termination shock is believed to be 75 to 90 astronomical units[7] from the Sun.
But getting back to the topic of this thread, your diagram shows a red area where the flow would "speed up" between the bodies, that is the area of interest I've been focusing on for the venturi effect claim. So in that area of interest the expansion from 0.99996AU to 1.00004AU isn't a huge effect, I don't see how additional expansion of the solar wind out to 10AU is relevant to that.
And you still haven't answered my question:
In addition to speeding up in between the bodies, as your diagram shows, won't the solar wind also speed up on the corresponsing outside edges? In this illustration that would be the top and bottom flow.
Don't the flows above and below the top sphere cancel out, and the flows above and below the bottom sphere cancel out?
If you bring the spheres closer together you might get some interaction different from this, but they would have to be pretty close, much closer than the moon is to the Earth.
If you bring the spheres closer together you might get some interaction different from this, but they would have to be pretty close, much closer than the moon is to the Earth.
According to the laws governing fluid dynamics, a fluid's velocity must increase as it passes through a constriction to satisfy the conservation of mass, while its pressure must decrease to satisfy the conservation of energy. Thus any gain in kinetic energy a fluid may accrue due to its increased velocity through a constriction is negated by a drop in pressure. An equation for the drop in pressure due to the Venturi effect may be derived from a combination of Bernoulli's principle and the continuity equation.
Originally posted by XPLodER
According to the laws governing fluid dynamics, a fluid's velocity must increase as it passes through a constriction
Originally posted by Arbitrageur
Originally posted by XPLodER
According to the laws governing fluid dynamics, a fluid's velocity must increase as it passes through a constriction
Yes but the gap between the Earth and the moon is too large to be called a constriction
General volumetric thermal expansion coefficient
In the general case of a gas, liquid, or solid, the volumetric coefficient of thermal expansion is given by
The subscript p indicates that the pressure is held constant during the expansion, and the subscript "V" stresses that it is the volumetric (not linear) expansion that enters this general definition. In the case of a gas, the fact that the pressure is held constant is important, because the volume of a gas will vary appreciably with pressure as well as temperature. For a gas of low density this can be seen from the ideal gas law.