Between 10 and 15 million degrees.
Hydrogen undergoes nuclear fusion to form helium at a temperature of 107 K
The core of the protostar reached an extremely high temperature
A protostar must reach about 10 million degrees Celsius for nuclear fusion to start in its core, triggering the transition into a true star. This marks the point where hydrogen atoms begin fusing into helium, releasing energy in the process. So, a protostar will become a full-fledged star after nuclear fusion begins at this temperature.
The next nuclear fusion cycle after helium fusion in a massive star is carbon fusion. This process involves fusing helium nuclei to form carbon. Carbon fusion typically occurs in the core of a massive star after helium fusion is completed.
The core of a protostar must reach temperatures of at least 10 million degrees Celsius for nuclear fusion to begin. At this temperature, hydrogen atoms can overcome their mutual repulsion and fuse to form helium, releasing energy in the process.
Hydrogen undergoes nuclear fusion to form helium at a temperature of 107 K
The core will reach between 250,000,000 to 500,000,000'C at its stable temperature. Beforehand it will rapidly gain heat from hundreds of thousands to its stable temperature, where it can begin the process of nuclear fusion. Hope that helps!
The core of the protostar reached an extremely high temperature
A protostar is heated up by gravitational forces causing it to contract and increase in temperature. Once the core reaches a high enough temperature and pressure, nuclear fusion reactions begin, releasing energy and making the protostar shine as a star.
A protostar must reach about 10 million degrees Celsius for nuclear fusion to start in its core, triggering the transition into a true star. This marks the point where hydrogen atoms begin fusing into helium, releasing energy in the process. So, a protostar will become a full-fledged star after nuclear fusion begins at this temperature.
For nuclear fission reactors there is no critical temperature, though they do have a temperature coefficient which makes the efficiency of the chain reaction vary slightly with temperature. This can be negative or positive, obvously a negative coefficient is preferred and is safer. Nuclear fusion is another matter, and very high temperatures are required in tokamaks to get fusion started
The next nuclear fusion cycle after helium fusion in a massive star is carbon fusion. This process involves fusing helium nuclei to form carbon. Carbon fusion typically occurs in the core of a massive star after helium fusion is completed.
Nuclear fusion is the process that causes a star to begin producing vast amounts of energy by converting hydrogen into helium through a series of fusion reactions in its core.
The core of a protostar must reach temperatures of at least 10 million degrees Celsius for nuclear fusion to begin. At this temperature, hydrogen atoms can overcome their mutual repulsion and fuse to form helium, releasing energy in the process.
The minimum temperature is about 10,000,000 degrees Celsius.
It is generally thought that as the gasses needed to create a star collect, the gravity that is pulling them together will compress and heat that gas so much that at some point fusion will spontaneously begin.
Gravitational attraction pulls gas and dust together in a nebula, causing it to condense and heat up. When the pressure and temperature in the core of the nebula become high enough, nuclear fusion reactions begin, initiating the process of becoming a star.