Understanding the Sun's Structure and Energy

The balance of inward gravitational forces and outward pressure forces within a star, like the Sun.

Process within the Sun's core that creates energy.

Force equals pressure multiplied by area (F=PA).

Force acting per unit area.

Force of attraction between masses.

Maintaining balance between inward and outward forces within a star.

Nuclear reactions in a star's core.

Sun's core pressure supports the outer layers preventing collapse.

The process by which the Sun produces energy.

The erratic path of photons as they travel through the Sun's interior

Region in the Sun where hot gas rises and cool gas falls, causing circulation.

The visible surface of the Sun.

The part of the convection zone where hot materials move upward.

The part of the convection zone where cool materials move downward.

Part of the Sun where convection occurs, related to rising and falling gas.

A computer model used to visualize processes in the solar convection zone.

The total energy radiated per second by the Sun.

The amount of energy received from the Sun at Earth's distance (1 AU).

The time period during which a star like the Sun primarily fuses hydrogen into helium to produce energy.

The intensity of radiation from a source decreases with the square of the distance from the source.

Astronomical Unit; the average distance between Earth and the Sun

A measure of the total energy radiating from a star.

The rate at which the Sun produces energy through nuclear fusion.

The rate at which the Sun loses energy by radiating it into space.

The process of fusing hydrogen nuclei to form helium nuclei.

The total duration of a star's existence.

A cooler, darker region on the Sun's surface caused by intense magnetic fields inhibiting energy flow.

The darkest and coolest part of a sunspot, located in the center.

The lighter, surrounding area of a sunspot, less cool than the umbra.

Invisible forces that influence the behavior of electrically charged particles, like those in the Sun.

Imaginary lines representing the direction of a magnetic field.

Magnetic poles (north and south) that attract each other.

Heat transfer that occurs when fluids (like gas in the Sun) circulate.

Areas on the Sun where convection is inhibited by strong magnetic fields, leading to lower temperatures.

The splitting of spectral lines in the presence of a magnetic field.

Intense magnetic fields suppress the flow of hot plasma, making them cooler and darker than surrounding areas.

The amount of splitting in spectral lines reveals the strength of the magnetic field within sunspots.

A period of very low sunspot activity lasting from about 1645 to 1715.

A period of colder global temperatures that coincided with the Maunder Minimum.

While some studies suggest a link, it is a complex issue with several factors involved. More research is needed.

Sunspots are a sign of intense solar activity, indicating powerful magnetic fields on the Sun.

A continuous stream of charged particles, primarily protons and electrons, flowing outward from the Sun's corona.

Regions in the Sun's corona with lower temperature and density than surrounding areas, characterized by open magnetic field lines.

A periodic variation in the Sun's activity, marked by changes in the number and intensity of sunspots, flares, and coronal mass ejections.

High-speed solar winds originate from coronal holes, where open magnetic field lines allow charged particles to escape easily.

The period of lowest solar activity during a solar cycle, characterized by fewer sunspots and weaker solar flares.

Coronal holes are largest and most prominent during the solar minimum, allowing stronger and faster solar winds to escape.

A comet that fell into the Sun, observed by the SOHO spacecraft.

Solar and Heliospheric Observatory, a joint ESA and NASA mission studying the Sun.

The Sun's energy comes from nuclear fusion in its core, where hydrogen atoms combine to form helium, releasing immense energy.

A balance between the outward pressure of the Sun's hot core and the inward pull of gravity, keeping the Sun stable.

The Sun shines because nuclear fusion in its core generates energy, which is then radiated outward. This fusion process is sustained due to a balance between gravity and pressure.

The Sun’s region below the convection zone where energy travels by the random bouncing of photons, taking thousands of years to reach the surface.

Changes on the Sun's surface, like sunspots and flares, caused by magnetic fields that create disruptions and energy releases.