Name: PowerPoint Presentation
Uploaded: 2022-05-01
Duration: 11 min 46 s
Description: Stellar Evolution. STELLAR LIFE CYCLE Birth Main Seqvence Old Age Oeofh Remnant.

Stellar Evolution. STELLAR LIFE CYCLE Birth Main Seqvence Old Age Oeofh Remnant. 

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STELLAR LIFE CYCLE
Birth
Main Seqvence Old Age
Oeofh
Remnant

Stellar evolution is a description of the way that stars change with time. On human timescales, most stars do not appear to change at all, but if we were to look for billions of years, we would see how stars are born, how they age, and finally how they die.. 

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Stellar evolution is a description of the way that stars change with time. On human timescales, most stars do not appear to change at all, but if we were to look for billions of years, we would see how stars are born, how they age, and finally how they die.

The hottest stars will emit more high frequency light whereas the cooler stars emit more light with lower frequencies.

Low frequency light corresponds to the red end of the visible light spectrum whereas high frequency light corresponds to the blue end.

This means that stars which emit blue light are hotter than white stars, white stars are hotter than yellow stars, yellow stars are hotter than orange stars and orange stars are hotter than red stars, which are the coldest type of star there is.

Classifying Stars. The Hertzsprung -Russell Diagram (H-R Diagram) - a graph that plots the surface temperature of stars against their luminosity. 

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The  Hertzsprung -Russell Diagram (H-R Diagram) - a graph that plots the surface temperature of stars against their luminosity

HERTZSPRUNG -RUSSEII DIAGRAM
RED GIANTS
MAIN StQUENCE
WHIIE WRES
IfMPfRAIURE

X- axis - the temperature of the star Y-axis - the luminosity of the star

An important tool in the study of stellar evolution is the  Hertzsprung -Russell diagram (HR diagram), which plots the absolute magnitudes of stars against their spectral type (or alternatively, stellar luminosity versus effective temperature). As a star evolves, it moves to specific regions in the HR diagram, following a characteristic path that depends on the star’s mass and chemical composition.

Blue Giants
Main Sequence
Wh ite Dwa rfs
Red Supergiants
Red Giants
Main Sequence
000
Temperature (K)

Life cycle of a star. NULA MOSIAR WSS SIR ND SIPtRGANT. 

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A nebula, which means “cloud” or “mist” in Latin, is an interstellar cloud of dust, hydrogen, helium and other ionized gases.

Nebulae are mainly composed of hydrogen. As the dust and gas particles are pulled closer together by the force of gravity, a protostar is formed.

PROTOSTAR. A protostar is a very young star that is still gathering mass from its parent molecular cloud. 

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A protostar is a very young star that is still gathering mass from its parent molecular cloud

It has a dense gaseous nucleus and a dust cloud around it.

The temperature continues to increase in Protostar at about 10, 000, 000 degree Celsius.

Main Sequence Star. The Main-Sequence Stage. 2nd stage (longest in the life of a star). 

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2nd stage (longest in the life of a star)

A star similar to the sun’s mass stays main-sequence for about 10 billion years

More massive stars = 10 million years because they fuse hydrogen rapidly

3rd stage when almost all of the hydrogen atoms in the core have fused into helium atoms

The helium core becomes hotter, it transfers energy into a thin shell of hydrogen surrounding the core

The on-going fusion of hydrogen radiates energy outward, which causes the star to expand greatly

Stellar evolution
low- and medium-mass stars
(including the Sun)
nebula
high-mass stars
giant
red supergiant
main sequence
not to scale
0 2012 Encyclopædia Britannica, lnc
"planetary"
nebula
supernova
white
dwarf
high-mass star
neutron
star
very high-mass star
black
hole

A star grows cooler as it expands. They begin to glow with a reddish color.. 

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A star grows cooler as it expands. They begin to glow with a reddish color.

Giants  – a very large and bright star whose hot core has used most of its hydrogen 10x or more larger than the sun Stars like the sun will become giants

3rd stage -Stars that are much larger than the sun become  supergiants Supergiants  are often at least 100x larger than the sun

The Final Stages of a Sunlike Star. Fusion in the core will stop after the helium atoms have fused into carbon and oxygen. 

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Stellar evolution
low- and medium-mass stars
(including the Sun)
giant
red
"planetary"
nebula
white
dwarf
high-mass star
nebula
sequence
high-mass stars
main sequence
not to scale
0 2012 Encyclopædia Britannica, lnc
neutron
supernova Very high-mass star
black
hole

Red Giant
Red
Supergiant
Planetary Nebula
Supernova
Dwarf
Neutron Star
Black Hole

Fusion in the core will stop after the helium atoms have fused into carbon and oxygen

Red giants transform into white dwarfs by ejecting its outer layer of gas and dust. What remains is a dense, hot core which now emits white light as its surface temperature has increased.

Red supergiants will continue fusing heavier and heavier elements, getting hotter and expanding until they explode in a supernova. The supernova expels dust and gas into space, leaving behind a neutron star, or in the case of very big stars, a black hole.

Stellar Evolution. AVER.ACÆ SIAR NEBUIA Pf010SIAR MASS WPERNOVA. 

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References https://www.thesciencehive.co.uk/stellar-evolution-gcse https://slideplayer.com/slide/2562891/ https://astronomy.swin.edu.au/cosmos/s/Stellar+Evolution

AVER.ACÆ
SIAR
NEBUIA
Pf010SIAR
MASS
WPERNOVA

PowerPoint Presentation

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 References https://www.thesciencehive.co.uk/stellar-evolution-gcse https://slideplayer.com/slide/2562891/ https://astronomy.swin.edu.au/cosmos/s/Stellar+Evolution

PowerPoint Presentation

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