1 THE SUN Nada Al-Haddad KU Leuven SHINE 2011. 2 OUTLINES Properties Core Radiative Zone Convective Zone Photosphere Chromosphere Corona 2.

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Presentation transcript:

1 THE SUN Nada Al-Haddad KU Leuven SHINE 2011

2 OUTLINES Properties Core Radiative Zone Convective Zone Photosphere Chromosphere Corona 2

3 Main Sequence G star M = 2x10 30 kg R = 7x10 8 m = 7x10 5 km L = 3.9x10 26 W (Solar Constant = 1350 W/m 2 ) Mean Density = Mass/Volume = M/((4/3)πR 3 )= 1400 kg/m 3 = 1.4 g/cm 3 Properties 3

4 Main Regions 4

5 The core Energy generation through nuclear burning 5 Main Regions

6 Adapted from George Rafflet at Jigsaw, India 2007 The core Energy generation through nuclear burning 6 Main Regions

7 Radiative Zone Energy transportation through Radiation 7 Main Regions

88 Convective Zone Energy transportation through Convection

9 Convective Zone Energy generation through nuclear burning 9 Main Regions

10 Photosphere Source of Photons 6000 K SUNSPOTS Low temperature in the photosphere ~ 4780 K Intense magnetic field Days-Weeks Features: 10

Km 10^-4 the intensity of the photosphere Temperature increase K He II, Fe II, Si II, Cr II and Ca II Chromosphere Features: Flares Prominences 11

12 Transition region 12

13 Corona Very high temperature Visible at total eclipse No well defined outer boundary Low density 5273 K 2,000,273 K Features: Coronal holes Dark in X-ray and EUV Low density High speed Solar wind 13

14 Solar wind Constant stream of charged particles (Plasma) from Sun to beyond pluto ( 5900 million km) 95% protons & electrons, 5% isotopes: helium-3, helium-4, neon-20, neon-21, neon-22, and argon-36 Average speed 450 km/s Average Density 4 atoms/cm 3 Shapes the magnetosphere 14

15 Solar wind Constant stream of charged particles (Plasma) from Sun to beyond pluto ( 5900 million km) 95% protons & electrons, 5% isotopes: helium-3, helium-4, neon-20, neon-21, neon-22, and argon-36 Average speed 450 km/s Average Density 4 atoms/cm 3 Shapes the magnetosphere 15

16 Solar Cycle 16

17 Solar Cycle

18 Coronal Mass Ejections explosions in the Sun's coronacorona huge bubbles of gas threaded with magnetic field lines 10^6 K A lot of material is thrown out into the solar windsolar wind CME's can seriously disrupt the Earth's environment Earth's environment 18

19 Dank U Wel! 19

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