A state equation for dense nuclear thing like neutron stars

Neutron stars are some of the largest things in the universe. They are the core of a crumpled megastar who went sernova, there was a typical radius of 10 km only more than the length of Mt. Everest-and their density can take several times in atomic nuclei.

Feel like physicists love extreme things like this because they ask them to stretch their theories in new places and see if they have confirmed, requiring new thinking and new science.

For the first time, researchers use lattice quantum chromodynamics to study the interior of neutron stars, how the pressure, temperature and other properties are related to each other.

Their work contamination on Physical Review Letters.

Neutron stars present other challenges other than an humorous density. Their little size makes them impossible to study visual telescopes, because it does not exceed a point. .

World Laboratories cannot be many materials equal to their ego, about an hour in water quadrillion – or near their dimensions. Even study theory is difficult, because relevant equations cannot be solved with math or computional techniques.

This new method, using the same particle theory and simulations, determines the new, strong control over the nopeutron stars. In particular, a highest speed sound was established – higher but specific – and such stars can grow greater than before.

Like any substance, neutron stars have a state equation, or more than a round diagram, like water.

The properties of a neutron star specified in Quantum chromodynamics .

But QCD makes calculating particle interactions very difficult, because the usual word in force, the gluon, brings the main figure of strong particles. It seems that the photon, the boss that sends strong electromagnetic (em) electrical fees. (Instead, photon neutral in photson.)

Thus, QCD is called a “nonlinear” theory. QCD also has a separate property of asymptotic freedom – the energy is small and important to be lost in small distances, such as the rise of distance, but the opposite of other distance forces.

If there is a lot of coup, the amount of welcomes theorists cannot use their standard, called good mathematical procedure called Theory of perturbationinvolving the violation of the calculation of an endless series (such as a Taylor series Familiar with basic calculus) and calculate one or some of the first terms.

EM perorturbation is good at EM because consecutive power to coupling over and over, Alpha ~ 1/137, get a bit speed. But that doesn’t happen for the full energy spectrum of QCD.

So, the authors of the lead Ryan Abbott in the center for theoretical physics of the Massachusetts Institute of Technology (MIT) and his fellow men turned to a stable alternative, lattice qcd.

There, the space and time in which interactions with the fragments divided by a discrete grid, and the dynamics of interactions are calculated only with grid points. Even this technique has Neutron Star Learners’ problems.

But another adaptation is possible: using isospin, another number of amounts with the opposite amounts, + the idea that proton and neutrons can be treated with the same isospins).

Quantum Mechanical Mathematics on Isospin is very similar to the usual fragment of fragment of quantum mechanics and quantum electembynamics. It is known that the nuclear thing in any density has a pressure less than nuclear thing in nonzero isospin density.

Using this pressure limit, the group can “drill” in high-density regions of Neutron Star and earn strict results. To do this, the team decreases the full mathematical description of a neutron star, then run several times in the lattice qcd taking “several thousand times in the GPU,” dividing several gpu times.

Many parts of the calculation previously done other researchers; Abbott estimates that with all the problem required “Many GPU times” in a supercomputer. To correct the isospin nuclear thing adapted to a discrete space-time grid, they obtained “continuous space” where no one has done for isospin nuclear thing.

They obtained a state of the State of Isospin-Dense item for any chemical potential to be isospin (energy change if added or reduced the particle number) to a result presented for the first time.

From the genuine field theory, previously suggested that the speed of a neutron star, traveling as a maximum interview with the Q / √3 in the power of light. But Abbott finds and in his group a speed sound that exceeds it – even if it’s uncertain, it’s higher, with a peaking range of ¾ c.

Abbott results and colleagues open a window to further computation studies in Neutron Stars. The more refined calculations can be made, such as multiplying viscyities, and maybe to interpret astronomy observations, and may have predicted it.

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