ZhaoZoharEX 
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**[NOTE: the following is taken from a cursory glance at sources ranging from Google and Wikipedia, to Quora and Reddit in addition to other sources. While this information is as accurate as I can reasonably achieve in a short amount of time I have, do take it with a grain of salt.]**
To answer the actual question, your average supernova emits an estimated 1–2·10^44^ Joules of energy, which is equivalent to approximately 2.4–4.8·10^28^ megatons of TNT, or about 24—48 octillion tons. This would be equivalent to the energy generated from a mass 10^12^ (one trillion) times that of Earth, which is approximately 5.972·10^24^ kilograms. For reference, a solar mass (a mass equal to 1 Sun) is about 1.989·10^30^ kg. The Sun accounts for 99.86% of all of the mass of the Solar System which is an estimated 1.0014 solar masses
For those that don't know or understand how exponents work, keep in mind that the difference between 10^9^ and 10^10^ is ten times, so 10^10^ is ten times more than 10^9^, one hundred times more than 10^8^ and so on up the chain.
A star (or really most stellar object) needs to move into a threshold of 8–15 solar masses before it can be capable of going supernova. The reason supernovae happen is because of all that extra mass collapsing in on itself due to gravitational force. A star produces nuclear fusion it it's core and the energy produces pressure that counteracts gravity. That pressure condenses the outer layers of the star and it runs out of hydrogen in those layers, it uses the hydrogen deeper in its core; this causes the outer layers to expand as it cools, this expanding into a red giant. When the star runs out of hydrogen, it starts using the helium to continue further nuclear reaction, then further elements until it gets to iron, from which it can't decay further. There is no more reaction to be had and this the pressure is superseded by the gravitational forces.
A star the size of our Sun will simply eject the outer layers when it runs out of fuel while a star that meets the above threshold will collapse back on itself and the resulting force of this causes a monumental release of energy. Depending on the size of the star, it will become one of a few class of either neutron star or black hole.
In other words: Forget the Sun; there is literally not enough mass within the *entire solar system* that comes anywhere remotely close to equaling what's required for the power of a supernova, which mind you briefly outshines *entire galaxies* during it's duration.
I got a little off track, but that's about the answer the the question of "what yield is a supernova". The sun *can't* go supernova, it doesn't have enough mass, but hypothetically if it *could*, the answer would probably be about the same as the amount of energy it's emitted in it's entire lifetime.
I'm sure someone will critique my wall of text and find errors, and please do. I won't learn otherwise and I admit my research was sloppy.
To answer the actual question, your average supernova emits an estimated 1–2·10^44^ Joules of energy, which is equivalent to approximately 2.4–4.8·10^28^ megatons of TNT, or about 24—48 octillion tons. This would be equivalent to the energy generated from a mass 10^12^ (one trillion) times that of Earth, which is approximately 5.972·10^24^ kilograms. For reference, a solar mass (a mass equal to 1 Sun) is about 1.989·10^30^ kg. The Sun accounts for 99.86% of all of the mass of the Solar System which is an estimated 1.0014 solar masses
For those that don't know or understand how exponents work, keep in mind that the difference between 10^9^ and 10^10^ is ten times, so 10^10^ is ten times more than 10^9^, one hundred times more than 10^8^ and so on up the chain.
A star (or really most stellar object) needs to move into a threshold of 8–15 solar masses before it can be capable of going supernova. The reason supernovae happen is because of all that extra mass collapsing in on itself due to gravitational force. A star produces nuclear fusion it it's core and the energy produces pressure that counteracts gravity. That pressure condenses the outer layers of the star and it runs out of hydrogen in those layers, it uses the hydrogen deeper in its core; this causes the outer layers to expand as it cools, this expanding into a red giant. When the star runs out of hydrogen, it starts using the helium to continue further nuclear reaction, then further elements until it gets to iron, from which it can't decay further. There is no more reaction to be had and this the pressure is superseded by the gravitational forces.
A star the size of our Sun will simply eject the outer layers when it runs out of fuel while a star that meets the above threshold will collapse back on itself and the resulting force of this causes a monumental release of energy. Depending on the size of the star, it will become one of a few class of either neutron star or black hole.
In other words: Forget the Sun; there is literally not enough mass within the *entire solar system* that comes anywhere remotely close to equaling what's required for the power of a supernova, which mind you briefly outshines *entire galaxies* during it's duration.
I got a little off track, but that's about the answer the the question of "what yield is a supernova". The sun *can't* go supernova, it doesn't have enough mass, but hypothetically if it *could*, the answer would probably be about the same as the amount of energy it's emitted in it's entire lifetime.
I'm sure someone will critique my wall of text and find errors, and please do. I won't learn otherwise and I admit my research was sloppy.