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GCSE Astronomy > Topic 10 > Flashcards

Topic 10 Flashcards

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1
Q

Name 2 methods of safely observing the Sun

A

Telescopic projection- point telescope at Sun and use eyepiece to project the image of the Sun onto card
(DO NOT LOOK IN THE TELESCOPE

H-alpha filter- H-alpha is a specific band of wavelength in the SUn’s light spectrum observing this band of wavelength allows us to safely see emissions and the sun’s surface, the filter focuses on the h-alpha wavelengths and filters out the others

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2
Q

Name the internal divisions of the Sun

A

Starting from centre:
-Core
-Radiative and Convection zones
-Photosphere

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3
Q

Name the components of the solar atmosphere

A

Chromosphere
Corona

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4
Q

How hot are the core, radiative and convection zones, and photosphere

A

15,000,000 degrees K, 2,000,000-6,000 degrees K, 5,800 degrees K

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5
Q

WHat happens at the core

A

Where the sun produces energy.
It is so hot the SUn is able to react Hydrogen nuclei into Helium via nuclear fusion

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6
Q

What happens at the radiative and convection zones

A

Light photons and heat pass through these regions. In the radiative zone photons are scattered by electrons and in the convection zone, thermal energy is transferred by rising currents of hot plasma

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7
Q

What happens at the photosphere

A

This is the surface layer of the SUn that we are able to see. Features of the photosphere include a process called granulation- these are circular areas with a thin darker area around them. Sunspots are also visible in the photosphere

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8
Q

What is the chromosphere (sphere of colour)

A

The chromosphere

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9
Q

What are the brighter regions of granules

A

The top of convection currents, which are hot plasma rising

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10
Q

What is the SUn’s core

A

an extremely hot environment, which is so hot that the Sun can react hydrogen nuclei into Helium through nuclear fusion

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11
Q

What is the Sun’s radiative zone?

A

Photons are scattered and emitted by electrons

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12
Q

What is the SUn’s convection zone

A

Thermal energy is transferred by rising currents of hot plasma

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13
Q

What is the photosphere

A

The layer of the Sun we can see
-granulation happens here which is circular areas with a thin darker area around them
-the granules are the tops of convection currents

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14
Q

What is the chromosphere

A

the lower region of the Sun’s atmosphere
-Only briefly observed during a solar eclipse as a bright rim around the Sun

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15
Q

What is the corona?

A

Upper region of the Sun’s atmosphere, made of gases expelled from the Sun
-best observed during a solar eclipse where it appears as a ‘halo’
-it emits x-rays
-it generates high energy particles which interact with the magnetic field of the Sun
->some of these particles are pulled back towards the SUn while others are so energised they fly out of the corona at high speeds to form the SOlar wind

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16
Q

What is the solar minimum

A

When the least and most sunspots are, this is an 11 year cycle which forms half of a 22 year cycle of solar activity, after the minimum and maximum is reached, the polarity of the magnetic field reverses

17
Q

What is nuclear fusion

A

At high temperatures, hydrogen nuclei fuse to form helium
-through the proton-proton chain
-releasing lots of energy

18
Q

What are sunspots?

A

> Areas on the photosphere that are cooler than the surrounding area and appear darker as a result
They have a high magnetic field strength which keeps internal heat from reaching the areas

SUNSPOT UMBRA: 4000K
SUNSPOT PENUMBRA: 5600K

19
Q
A
20
Q

What are the origins of SUnspots

A

caused by changes in the Sun’s magnetic field.
Coronal loops are ejected and drawn back to the Sun.
-They can build up to form prominences when they land they ‘puncture’ the chromosphere and decrease the temperature
-They can last from several hours to months

21
Q

WHat is evidence for the solar cycke

A

Sunspots are good evidence for what the SUn goes through every 11 years.
-It can be visualised using the butterfly diagram
-THe more sunspots, the more heat
-THe more sunspots mean the more active the Sun is

22
Q

How can we observe the rotation of the Sun?

A

We can observe the rotation of the SUn by recording the speed of Sunspots across the photosphere

23
Q

WHy doesn’t the Sun rotate like a terrestrial planet, what are the times of rotation at the equator and pole?

A

The Sun is a ball of gas and plasma so doesn’t rotate like a terrestrial planet.
Its poles rotate slower
equator- 25 days
poles- 36 days

24
Q

What is the Solar wind?

A

Charged particles are produced by the corona at high velocities
-THe magnetic field draws some particles back to the Sun
-others gain enough energy to overcome the Sun’s gravity and are ejected into space- becoming solar wind

25
Q

What does the solar wind help shape

A

the Earth’s magnetosphere

26
Q

What can the solar wind storms disrupt

A

Can disrupt communications and navigational equipment, damage satellites and cause blackouts.

27
Q

WHat are solar flares

A

Caused by twists in the magnetic field of the SUn near sunspots which cause explosions of energy and radiation

28
Q

Violent outbursts of particles that blast away from the Sun in all directions
-THey accompany solar flares
-We experience the effects of the them on Earth

A

Coronal Mass Ejections

29
Q

Coronal Mass Ejections

A

Violent outbursts of particles that blast away from the Sun in all directions
-THey accompany solar flares
-We experience the effects of the them on Earth

30
Q

List 4 effects of solar wind

A

-Aurorae (Borealis[n] & Australis[s])
-Comets
-Geomagnetic storms
-Satellites, aircraft, and space missions

31
Q

How does solar wind cause aurorae

A

ions from solar wind collide with atmospheric particles

32
Q

How does solar wind affect comets

A

radiation in solar wind interact with the comet to form a tail (pointing away from the Sun)

33
Q

How does solar wind cause/effect geomagnetic showers

A

these are increased plasma from coronal mass ejections interacting with the Earth’s magnetosphere, which can affect the altitude of aurorae and electrical supply on Earth

34
Q

How does solar wind effect satellites, aircraft, and space missions

A

solar wind can hear up machines, and interact with the ionosphere to disrupt radio communications

35
Q

What is the magnetosphere and what is it caused by

A

Earth has a huge magnetic field surrounding it (magnetosphere)
this is caused by its iron based core and rotation, it is shaped b the solar wind

36
Q

Why is there a bow shock line

A

THe Earth is protected by magnetic belts of the magnetosphere from solar wind, where the magnetosphere meets the solar wind, there is a shock wave called the bow shock line

37
Q

What does the magnetosphere contain

A

belts which trap radiation and charged particles from the Sun

38
Q

What are the Van Allen belts

A

Charged particles move along the belts to the poles, and in the atmosphere these ions collide with oxygen and nitrogen to form coloured displays of light called aurorae

GCSE Astronomy (19 decks)

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