our sun
DESCRIPTION
OUR SUN. The Core. Innermost layer of the sun. Density 10x that of lead. Fusion produces energy. 27 Million degrees Fahrenheit. Radiative Envelope. Transfers Energy out of the core by radiation. Convective Envelope. - PowerPoint PPT PresentationTRANSCRIPT
The CoreThe Core
Innermost layer of the sun.
Density 10x that of lead.
Fusion produces energy.
27 Million degrees Fahrenheit
Radiative EnvelopeRadiative Envelope
Transfers Energy out of the core by radiation.
Convective EnvelopeConvective Envelope Transfers Energy to the outer part of the Sun by rising and falling gases..
PhotospherePhotosphere
The visible layer of the Sun.Location of magnetic stormsTemperature 10,000 degrees to 7,800 degrees in sunspots.Below Chromosphere and Corona
Sunspots and Granulation
ChromosphereChromosphere
Location of solar flares.
Temperature 50,000 degrees.
Red in color due to an abundance of Hydrogen
Between Photosphere and Corona
Chromosphere
CoronaCorona
Only visible during an eclipse.4 million degrees FahrenheitScientists are trying to figure out why it is hotter than the other layers.Outermost layer of the sun.
Corona
Infrared Corona
Coronal Mass Ejections (CME’S)Coronal Mass Ejections (CME’S)
A massive burst of solar wind, other light isotope plasma, and magnetic fields rising above the solar corona or being released into space.
Associated with sunspots and solar flaresCan cause strong Auroras and disrupt radio and satellite signals.
Coronal Mass Ejections (CME’S)Coronal Mass Ejections (CME’S)
Coronal Mass Ejections (CME’S)Coronal Mass Ejections (CME’S)
During Solar maxima we see 3 CME’s a day
During Solar minima we see 1 CME every three days
How our magnetic Field protects us
How our magnetic Field protects us
How our magnetic Field protects us
How our magnetic Field protects us
During solar flares and CME’s the magnetic field deflects the radiation away from the Earth’s surface