Asteroseismology primarily relies on photometric observations to measure the variations in a star's brightness caused by pulsations.

Radial pulsations involve the expansion and contraction of the entire star, causing variations in its overall brightness.

Asteroseismology specifically refers to the study of stellar pulsations and their impact on the star's structure and evolution.

Non-radial pulsations involve the expansion and contraction of specific regions of the star, resulting in asymmetric patterns.

Asteroseismology allows astronomers to determine various stellar parameters, including mass, radius, temperature, and luminosity, by analyzing the frequencies and patterns of stellar pulsations.

A supernova is a catastrophic explosion that occurs when a massive star reaches the end of its life and undergoes a sudden collapse and subsequent explosion.

Type II supernovae are associated with the collapse of massive stars, leading to the formation of a neutron star.

A neutron star is the compact remnant left behind after a massive star undergoes a supernova explosion.

Type Ia supernovae are caused by the thermonuclear explosion of a white dwarf in a binary system.

A planetary nebula is a glowing shell of gas and dust ejected by a star during the late stages of its life.

Novae are sudden brightening events that occur when a white dwarf undergoes a runaway thermonuclear fusion reaction.

Stellar flares are sudden and intense bursts of energy released by stars, often associated with magnetic activity.

Novae are less violent explosions compared to supernovae, but they still involve a significant ejection of mass and energy.

Microlensing is a phenomenon where the gravity of a massive object, such as a star or a black hole, bends light from a distant object, causing it to appear brighter and distorted.

Supernovae are the most energetic stellar explosions, leading to the complete disruption of the star and the ejection of a large amount of mass and energy.