Astronomy 12- Interior of the Sun

Temperature in the Sun's core

Approximately 15.5 million Kelvin (15.5x10^6 K).

Mass Defect

The difference between the mass of an atom and the mass of its individual parts.

Binding Energy

The energy required to keep the nucleus of an atom together.

Thermonuclear Fusion

The process of fusing light atomic nuclei into heavier ones; powers all stars, including the Sun.

Hydrogen Fusion

The fusion of hydrogen nuclei into helium nuclei, a key process in stellar energy production.

Proton-Proton Chain

The most common nuclear fusion process in the Sun, transforming hydrogen into helium through several steps.

Hydrostatic Equilibrium

The balance between the inward force of gravity and the outward force of energy from nuclear fusion in the Sun.

Random Walk

The unpredictable zigzag path that photons take when traveling through the Sun's dense interior.

Convection Cell

A circular pattern of fluid motion caused by the heating of a fluid, leading to rising and sinking movements.

Granulation

The grainy appearance of the Sun's photosphere caused by the tops of convection cells.

Neutrino

A nearly massless particle that does not carry an electric charge and interacts very rarely with matter.

Gamma-ray photon

High-energy photon produced during nuclear reactions in the Sun.

Positron

A positively charged electron emitted during the fusion process in the Sun.

Helium-4 nucleus

The product of fusing two Helium-3 nuclei, consisting of 2 protons and 2 neutrons.

Supergranules

Larger convection cells beneath the photosphere of the Sun, which can be up to 30,000 km in diameter.

Einstein's Equation (E=mc^2)

The equation relating mass to energy, used to explain mass loss during nuclear fusion.

What are the sources of neutrinos?

Neutrinos are produced in nuclear reactions, particularly in the Sun, during supernova explosions, and in reactors.

How do neutrinos interact with matter?

Neutrinos interact very weakly with matter, allowing them to pass through thick layers of material without being affected.

Why are neutrinos important in astrophysics?

Neutrinos provide valuable information about stellar processes and the fundamental properties of particles.

What types of neutrinos exist?

There are three types (flavors) of neutrinos: electron neutrinos, muon neutrinos, and tau neutrinos.

What is neutrino oscillation?

Neutrino oscillation is the phenomenon where a neutrino changes its flavor as it travels through space.

What is the significance of the Solar Neutrino Problem?

It refers to the discrepancy between predicted and observed solar neutrinos, leading to insights on neutrino properties.