The SunStructure of the Sun

&

Solar Activity

Parts of the SunCore: enormous pressure & high temperatures cause the fusion of hydrogen into helium (15 million ºC)

Radiation Zone: energy from the core moves through the radiative zone in the form of electromagnetic radiation (2-7 million ºC)

Convective Zone: hot gasses move outward, cool, contract, sink, repeat (2 million ºC)

Photosphere: innermost layer of atmosphere – VISIBLE LIGHT (6 thousand ºC)

Chromosphere: gives off redish light from Hydrogen (4-50 thousand ºC)

Corona: very hot, creates solar wind, only visible during a solar eclipse (1 million ºC)

1st Year of SDO

Solar Activity (not part of your notes)

• The sun is in constant motion.The sun is in constant motion.• Parts of the sun rotate faster Parts of the sun rotate faster

than others. than others. • The equator moves the fastest, The equator moves the fastest,

the poles the slowest.the poles the slowest.• It takes an average of It takes an average of 27 days27 days

for the sun to make one for the sun to make one rotation.rotation.

Solar Activity (Ejections)

• Affected by the Affected by the sunspot cyclesunspot cycle

• Solar EjectionsSolar Ejections are when the are when the sun emits sun emits atomic particles:atomic particles:–ProminencesProminences

–Solar FlaresSolar Flares

–Coronal Mass Ejections Coronal Mass Ejections (CME’s)(CME’s)

Sunspots

Sunspots

Dark areas of the photosphere of the sun, that are cooler than the surrounding areas, and have a strong magnetic field.

Caused by magnetic fields created through the movement of gasses (rotation and convection).

The sunspot cycle lasts 11 years.

Sunspot Cycle Graph

11 years from low to low

SUNSPOTS• Sept 27, 2001 • Sept 27, 2008

(200+ days with no sunspots)

2008 also experienced a 50 year low in solar wind pressure.

Prominences

Huge arches of glowing gasses that connect areas (in the sun’s atmosphere) that have positive magnetic energy to areas with negative magnetic energy.

Caused by the same magnetic fields that create sunspots.

Prominences

Prominence

Solar Flares

• Sudden outward eruption of charged particles

• The trigger is unknown.

• During a peak , 5-10 can occur in one day

• Particles that escape will increase the strength of the solar wind.

Solar Flare

Coronal Mass Ejection

Particles (or parts of the corona) are thrown off the sun.

Strike Earth’s magnetosphere creating disturbances called geomagnetic storms.

Geomagnetic storms can disturb radio communication, damage satellites and cause auroras.

Earth’s Magnetosphere

Earth

Earth’s Magnetosphere

A magnetic field surrounding the earth – affected by solar wind and the magnetic fields of other space objects.

Protects the majority of the Earth from the solar wind.

Solar wind is a stream of electrically charged particles (protons & electrons) flowing from the sun.

Earth’s Magnetosphere

Computer Animation of a CME creating Auroras on Earth – notice Earth’s magnetosphere. (Wait for animation to start )

Auroras

Solar Wind

Geomagnetic Storm Effects

• Radiation Hazards to humans– especially those in space

• Migratory animals less able to navigate (esp. homing pigeons)

• Communication Disruptions: ground-to-air, ship-to-shore, shortwave, broadcast, and amateur radio.

Geomagnetic Storm Effects

• GPS & Loran navigationdisruptions

• Satellite hardware damage

• Power Grid Outages – 1989 Quebec & NE US was out for 9 hours (affecting 6 million people)

Examples for Foldable