through the process of fusion, it becomes a star: the birth of the star is the start of fusion. therefore, it is after fusion that it is classified as a star.
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 nuclear fusion of hydrogen into helium
When matter is pulled into a protostar, it heats up and increases in density. This process leads to the formation of a protostar as gravitational forces pull matter towards the center, eventually igniting nuclear fusion and forming a stable star.
A protostar becomes balanced when the gravitational forces pulling matter inward are balanced by the outward pressure due to nuclear fusion at its core. This marks the transition from a contracting protostar to a stable star in the main sequence phase of its lifecycle.
The temperature of nuclear fusion is typically around 15 million degrees Celsius. This extreme temperature is required to overcome the electrostatic repulsion between positively charged atomic nuclei and allow them to fuse together to release energy.
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.
For nuclear fusion.
When the core of a protostar surpasses 18 million degrees Celsius, nuclear fusion of hydrogen into helium begins in earnest. This marks the transition from a protostar to a main sequence star, as the core temperature becomes high enough to sustain the fusion reactions that release energy. The resulting energy creates an outward pressure that balances the inward gravitational pull, stabilizing the star and allowing it to enter a prolonged phase of hydrogen burning. This process initiates the star's main sequence phase, where it will spend the majority of its life.
The temperature required for nuclear fusion to occur is around 100 million degrees Celsius.
The lowest temperature on the surface of the sun is about 5,500 degrees Celsius (9,932 degrees Fahrenheit). However, temperatures in the sun's core, where nuclear fusion occurs, can reach over 15 million degrees Celsius (27 million degrees Fahrenheit).
the centre of the sun reaches 15million degrees celsius.
The sun is hotter at its core, where nuclear fusion reactions take place, reaching temperatures of about 15 million degrees Celsius. The surface temperature, called the photosphere, is cooler at around 5,500 degrees Celsius.
A protostar; also a brown dwarf.
The temperature at the inner core of the sun reaches around 15 million degrees Celsius (27 million degrees Fahrenheit). This extreme heat is generated by nuclear fusion reactions that occur at the core.
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!
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.
It does not have any particular temperature, the nuclear reactions are not influenced by temperature, though the behaviour of a nuclear reactor does depend on its temperature since this influences the neutron spectrum. In a PWR the coolant exit temperature is about 325 degC.