A star is quite simple. Gravity squeezes star, trying to collapse. The inner core becomes extremely dense and hot. This is what triggers Nuclear fusionHeat and pressure pushes gravity back.
While a star is at its main sequence, the two forces are balanced. It’s easy peasy. The details are very complex.
It is very difficult to model the interior of stars accurately, even with sophisticated computer models. Now we have a Computer simulations are now available.Change is possible.
The flow of heat in a star is generally not balanced, even though the pressure inside and the gravitational mass of the star are. All of the heat and power generated within a star’s core has to be released at some point.
First is through a radiant exchange. The high-energy gamma radiation scatters against the nuclei of the core and gradually loses energy as it migrates to the surface. The interior of the star is so dense, that It can take thousands or even millions of years..
Convective flow is the second method. The hot material in the core of the star attempts to expand and pushes its way towards the surface. Cooler material at the surface of the star condenses as it sinks toward the core.
This creates a flow of material which transfers heat energy from the surface to the star. Convection is what churns a star’s interior. It is difficult to model because of factors such as viscosity, turbulent vortices and other physical properties.
Stars have two zones: a convective and a radiant zone. Location and size of the zones depends on a stars mass. Small stars have a convective nature, while larger stars such as the Sun are divided into an inner and outer zone.
In massive stars, the situation is reversed, with an inner radiative zone and an outside convective one. Convection can cause a star’s surface to move like water in a pot. The brightness of the star will then flicker.
This new study shows how convection zones in a luminous star affect the way it flickers. They found that the convective flow affects sound waves as they rippling in a star. This, in turn, changes how a star flickers.
It means that astronomers can, in theory, study the interior of stars by observing their flicker of lights.
The flickers are currently too small to be observed by the current telescopes. With larger, more sensitive telescopes, we may be able study them.
Helioseismology allows us to observe the effect of sound waves on the Sun. In the future, we will be able study nearby stars.
This article was first published by Universe Today. You can read the Original article.
