Search results
Results from the WOW.Com Content Network
In astrophysics, silicon burning is a very brief [1] sequence of nuclear fusion reactions that occur in massive stars with a minimum of about 8–11 solar masses. Silicon burning is the final stage of fusion for massive stars that have run out of the fuels that power them for their long lives in the main sequence on the Hertzsprung–Russell diagram.
In main sequence stars more than 1.3 times the mass of the Sun, the high core temperature causes nuclear fusion of hydrogen into helium to occur predominantly via the carbon-nitrogen-oxygen (CNO) cycle instead of the less temperature-sensitive proton–proton chain. The high temperature gradient in the core region forms a convection zone that ...
Flames of charcoal. A flame (from Latin flamma) is the visible, gaseous part of a fire.It is caused by a highly exothermic chemical reaction made in a thin zone. [1] When flames are hot enough to have ionized gaseous components of sufficient density, they are then considered plasma.
Similarly, for stars with a mass of less than 9 solar masses (without accretion of additional mass) oxygen ignites in the core or not at all. However, in the 9–10.3 solar mass range, oxygen ignites off-center. For stars in this mass range neon-burning occurs in a convective envelope rather than at the core of the star. For the particular ...
Typical boundary conditions set the values of the observable parameters appropriately at the surface (=) and center (=) of the star: () =, meaning the pressure at the surface of the star is zero; () =, there is no mass inside the center of the star, as required if the mass density remains finite; () =, the total mass of the star is the star's ...
An M-type flare star stripping away the atmosphere of its planet. A flare star is a variable star that can undergo unpredictable dramatic increases in brightness for a few minutes. It is believed that the flares on flare stars are analogous to solar flares in that they are due to the magnetic energy stored in the stars' atmospheres.
The neon-burning process is a set of nuclear fusion reactions that take place in evolved massive stars with at least 8 Solar masses.Neon burning requires high temperatures and densities (around 1.2×10 9 K or 100 keV and 4×10 9 kg/m 3).
T Tauri stars generally increase their rotation rates as they age, through contraction and spin-up, as they conserve angular momentum. This causes an increased rate of lithium loss with age. Lithium burning will also increase with higher temperatures and mass, and will last for at most a little over 100 million years.