The Story of our Sun Flashcards

1
Q

Radius

A

7 × 10^8 m 109 Earth radii

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2
Q

Radius

A

7 × 10^8 m 109 Earth radii

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3
Q

Mass

A

2 × 10^30 kg (330,000 Earth masses)

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4
Q

Density

A

Density 1.4 × 10^3 kg/m3 (1.4 times water)

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5
Q

Distance

A

Distance 150 × 10^6 km ( Defined as 1 A.U.)

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6
Q

Surface Temp

A

5780 K

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7
Q

Core Temp

A

15,000,000 K

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8
Q

Composition

A

71% hydrogen, 27% helium, 2% heavy elements

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9
Q

Power output

A

3.9 × 10^26 J/s

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10
Q

Age

A

4.5 billion years

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11
Q

Expected lifetime

A

12-15 billion years

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12
Q

The Sun age,

A

our nearest star, is estimated to be about 4.6 billion years old. This age is determined through various methods, including radiometric dating of meteorites and the study of the Sun

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13
Q

Structure and hydrostatic
equilibrium

A

the structure of a star is maintained by the equilibrium between gravity and the pressure generated by nuclear fusion reactions. This balance is crucial for stabilizing the star and allowing it to shine steadily over long periods of time.

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14
Q

Nuclear Fusion

A

is a process in which atomic nuclei combine to form a heavier nucleus, releasing a tremendous amount of energy in the process.

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15
Q

Future evolution

A

Main Sequence: -> Red Giant -> Helium Flash -> AGB

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16
Q

Red giants and planetary
nebulae

A

As a red giant star nears the end of its evolution, it undergoes a dramatic transformation into a planetary nebula.

Mass Loss: Ionized Gas: Complex Structures core becomes white dwarf

17
Q

AGB nucleosynthesis

A

refers to the process by which certain elements are synthesized in the advanced stages of stellar evolution on the Asymptotic Giant Branch (AGB). AGB stars are evolved, low- to intermediate-mass stars that have exhausted the hydrogen fuel in their cores and have expanded to become red giants