Exploring Superfluidity in Neutron Stars: A Crayon Explanation

In summary, the conversation discusses the concept of superfluidity in neutron stars and its relationship to cooling. It is mentioned that superfluidity plays an important role in the structure of neutron stars, with neutrons pairing in different states depending on the density. The issue at hand is understanding the effect of superfluidity on the cooling rate and how it may cause extra cooling through the emission of neutrino-antineutrino pairs. The conversation also briefly mentions a humorous explanation using crayons to describe superfluidity.
  • #1
bcrowell
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I thought others might be interested in this: http://arxiv.org/abs/1011.6142

As a nuclear physicist, I don't find it surprising to hear that neutron stars are superfluid. Nuclei are superfluid. I'm not clear on the relationship between superfluidity and cooling. Can anyone explain this using crayons?
 
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  • #2


You are in good company - http://news.discovery.com/space/the-neutron-star-cooling-mystery.html [Broken]. We are basically clueless.
 
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  • #3


Crayons? Well, crayons are the carriers of the color force, and... no wait, let's start over.
The known structure of neutron stars is getting pretty complex, and superfluidity plays an important part. In a region near the surface, the density is below what's found in nuclei. Here, superfluidity results from nucleons (both n and p) pairing in the 1S0 state, much like they do in nuclei. Nearer the center, however, the density is so great that the repulsive core in the 1S0 state becomes important. The neutrons now prefer the 3P2 state, and this is the superfluidity that they're talking about. (There's still a few protons around.)
This has all been known for some time, and the issue is what observable effect it has on the cooling rate. The neutrons form a degenerate Fermi gas, making the available transitions few. Most of the cooling normally comes from the Urca process (beta decays, n to p and vice versa). Any neutrinos that are formed easily escape, carrying away their energy.
Once superfluidity occurs, the bound pair state becomes available, and transitions to and from this state can happen with emission of a neutrino-antineutrino pair. This is what causes the extra cooling. They're hoping that the observations continue to confirm this theoretical picture.
 
  • #4


Bill_K said:
Crayons? Well, crayons are the carriers of the color force, and... no wait, let's start over.

all i have to say is... lol
 
  • #5


First of all, it's great to see interest in neutron stars and their fascinating properties! Superfluidity is a phenomenon where a liquid flows without any resistance, similar to how a superconductor allows electricity to flow without resistance. In the case of neutron stars, the liquid in question is actually the dense matter that makes up the star's core, which is primarily composed of neutrons.

Now, imagine you have a box of crayons, each representing a neutron. In a normal liquid, the crayons would move around and bump into each other, creating friction and resistance. But in a superfluid, the crayons are able to move freely and smoothly without any resistance, just like the neutrons in a neutron star. This is due to the unique properties of the superfluid, which allow the neutrons to flow without any hindrance.

As for the relationship between superfluidity and cooling, it has to do with the fact that superfluids have very low viscosity, meaning they have a hard time transferring heat. This allows the neutron star's core to cool down very slowly, as the heat is unable to escape easily. This slow cooling process is what allows neutron stars to maintain their superfluid state for a long time.

In summary, superfluidity in neutron stars can be explained using crayons as a liquid-like state where particles can flow without any resistance, leading to slow cooling and the maintenance of this unique state. I hope this helps to better understand the concept of superfluidity in neutron stars.
 

1. What is superfluidity in neutron stars?

Superfluidity is a state of matter where a substance has zero viscosity, meaning it can flow without any resistance. In neutron stars, the matter is so dense that it becomes a superfluid, allowing it to flow freely without any friction.

2. How is superfluidity studied in neutron stars?

Scientists study superfluidity in neutron stars through observations and theoretical models. They use telescopes to observe the behavior of neutron stars and analyze the data to understand the properties of superfluid matter. They also use mathematical equations and simulations to create models of how superfluid matter behaves in neutron stars.

3. What is the role of superfluidity in neutron stars?

Superfluidity plays a crucial role in the cooling process of neutron stars. As the star ages, it cools down and forms a crust, which is made up of superfluid matter. This superfluidity allows the star to cool down more quickly, making it easier for scientists to study and understand the properties of neutron stars.

4. Can superfluidity be found in other celestial bodies?

Yes, superfluidity can also be found in other celestial bodies such as white dwarf stars and certain types of gas giants. However, it is most commonly observed in neutron stars due to their extreme density and high temperature.

5. How does superfluidity in neutron stars impact our understanding of the universe?

The study of superfluidity in neutron stars helps scientists better understand the behavior of matter under extreme conditions, which can provide insights into the origins and evolution of the universe. It also has practical applications, such as in the development of superconductors, which have various technological uses.

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