How Does the Stiffness of Supernova EOS Change with Various Parameters?

In summary, the stiffness or softness of the supernova (SN) equation of state (EOS) depends on temperature, progenitor mass, and other parameters such as compressibility and symmetry energy. Softening in the neutron star (NS) EOS can potentially lead to softening in the SN EOS. This topic is being studied in a PhD thesis, specifically looking at the effects of extending a standard relativistic mean field model to include density-dependent couplings for the NS EOS. The possibility of predicting changes in the CCSN EOS from the softening of the NS EOS is being explored.
  • #1
silly_sheep
On what does the stiffnes/softness of the SN EOS depends? How does it change with temperature, progenitor mass, or other parameters like compresibility, symmetry energy etc? Would softening in NS EOS lead to softening in SN EOS?

Tnx, Cheers
 
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  • #2
silly_sheep said:
On what does the stiffnes/softness of the SN EOS depends? How does it change with temperature, progenitor mass, or other parameters like compresibility, symmetry energy etc? Would softening in NS EOS lead to softening in SN EOS?

Tnx, Cheers

hi there
welcome to PF :smile:

you have marked you thread at level A = post graduate level
what study / research have you done yourself so far with this topic so we can get an idea of where you are at ?

cheers
Dave
 
  • #3
davenn said:
hi there
welcome to PF :smile:

you have marked you thread at level A = post graduate level
what study / research have you done yourself so far with this topic so we can get an idea of where you are at ?

cheers
Dave

Hi Dave,

well, I am doing a PhD on the Equation of state topic... however, my EOS in for infinite nuclear matter and neutron stars, that is high densities, T=0 and taking into account only neutrons, protons and electrons as degrees of freedom. I made an extension on one of the standard used models (relativistic mean field model with density dependent couplings) and with it i am getting the softening of the EOS for NS. I am curious if it is possible to predict any changes for CCSN EOS that can be deduced from the NS EOS softening, that is, if it will also soften... since the densities are quite different and for CCSN the T is included...

So am trying to learn a bit more about CCSN EOS :)
 
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Likes davenn

1. What is a supernova equation of state?

The supernova equation of state is a mathematical relationship that describes the behavior of matter at extremely high densities and temperatures, such as those found in a supernova explosion. It takes into account factors such as pressure, temperature, and energy to determine the physical properties of the matter.

2. Why is the supernova equation of state important?

The supernova equation of state is important because it helps us understand the physics behind supernova explosions, which are some of the most powerful and catastrophic events in the universe. It also has implications for understanding the behavior of matter in other extreme environments, such as neutron stars and black holes.

3. How is the supernova equation of state calculated?

The supernova equation of state is typically calculated using theoretical models and computer simulations. These models take into account various physical factors, such as the effects of gravity, nuclear interactions, and radiation, to determine the properties of matter at high densities and temperatures.

4. How does the supernova equation of state affect the evolution of a supernova explosion?

The supernova equation of state is a key factor in determining the energy and dynamics of a supernova explosion. It affects how the matter in the exploding star behaves, and ultimately determines the type and strength of the explosion. Understanding the equation of state is crucial for accurately predicting and modeling the evolution of supernovae.

5. Can the supernova equation of state change over time?

Yes, the supernova equation of state can change over time as the physical conditions of the supernova explosion evolve. In the early stages of the explosion, the equation of state may be different from the later stages as the matter expands and cools. This dynamic behavior adds complexity to the study of supernova explosions and requires sophisticated models to accurately capture the changes in the equation of state.

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