Radiation pressure from the star's intense radiation field exerts a force on the outer layers of the star, pushing material outward.

Red giants have large surface areas and low surface gravities, making them more susceptible to mass loss through stellar winds.

In the solar wind, magnetic pressure from the Sun's magnetic field lines drives the outward flow of material.

The solar wind typically travels at speeds of around 500 km/s near Earth's orbit.

Wolf-Rayet winds are associated with massive stars and are known for their high mass-loss rates and fast outflow velocities.

Thermal pressure from the hot corona of the star accelerates the stellar wind particles outward.

Planetary nebula winds are produced during the final stages of stellar evolution when the star ejects its outer layers, forming a beautiful and colorful nebula.

The solar wind typically has a mass-loss rate of around 10^9 kg/s.

Red giant winds are known for their slow outflow velocities and relatively low mass-loss rates compared to other types of stellar winds.

The solar wind typically has a temperature of around 10^6 K near Earth's orbit.

Wolf-Rayet winds are associated with massive stars and are known for their high mass-loss rates and fast outflow velocities.

Thermal pressure from the hot corona of the Sun accelerates the solar wind particles outward.

Planetary nebula winds are produced during the final stages of stellar evolution when the star ejects its outer layers, forming a beautiful and colorful nebula.

The solar wind typically has a mass-loss rate of around 10^9 kg/s.

Red giant winds are known for their slow outflow velocities and relatively low mass-loss rates compared to other types of stellar winds.