Astronomers find that 90 % of the stars observed in the sky...

Astronomers find that $90 \%$ of the stars observed in the sky are on the main sequence of an $\mathrm{H}$ -R diagram; why does this make sense? Why are there far fewer stars in the giant and supergiant region?

Key Concepts

Giant and Supergiant Phases

The giant and supergiant phases are advanced stages in stellar evolution that occur after a star has exhausted the hydrogen in its core. These phases are characterized by significant changes in a star's structure and a temporary increase in luminosity. However, because these phases are brief compared to the main sequence, fewer stars are observed in these regions of the Hertzsprung-Russell diagram.

Hertzsprung-Russell Diagram

The Hertzsprung-Russell diagram is a fundamental tool in astrophysics that plots stars according to their luminosity and temperature. It reveals patterns in stellar properties and evolutionary stages, enabling astronomers to classify stars and understand the relationship between a star's brightness, temperature, and age.

Main Sequence

The main sequence represents a long-lasting phase in a star's life where it fuses hydrogen into helium in its core. This phase is the most stable and longest-lasting period for most stars, which is why a large percentage of observed stars are found along the main sequence in the Hertzsprung-Russell diagram.

Stellar Evolution

Stellar evolution describes the process by which a star changes over time, transitioning through various phases such as the main sequence, giant, and supergiant stages. The duration of each phase depends on a star's mass and composition, influencing its position on the Hertzsprung-Russell diagram.

Stellar Lifetimes

Stellar lifetimes refer to the duration a star spends in each phase of its evolution. The main sequence phase is the longest for most stars, which explains why the majority of stars observed are on this part of the Hertzsprung-Russell diagram. In contrast, the giant and supergiant stages are relatively short-lived, leading to their fewer numbers among the overall stellar population.

Transcript

00:01 Hi, everybody.

00:01 So we got to describe the evolution star with a mass similar to that the sun from the quarter star stage to the time it first became a red giant.

00:10 And so stars have life cycles like our own.

00:14 Okay.

00:16 So stars are formed by the concentrated clouds.

00:20 So then we first have nebulas.

00:24 Okay.

00:25 And when the nebula becomes dense.

00:28 So these nebulas become dense.

00:30 So we have these little.

00:31 Clouds and the clouds start becoming denser and denser and denser.

00:38 So all these particles are coming together.

00:42 And this phase is called a proto star phase.

00:45 So we have a proto star and that's when they're starting to come together.

00:51 That's when big chunkies are coming together and etc.

00:54 So the collapsing interstellarment causes enough pressure central area of the protostar and this rapid increase of pressure causes rapid increase of temperature.

01:02 And now the star begins release energy.

01:06 So in this process, we'll move it over here, is that these are causing a lot of pressure.

01:15 And this in return releases energy outward, okay? and as this phase of star, it's called a main sequence phase.

01:29 So we have a main sequence phase.

01:37 Okay...

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