Welcome to Environmental Science!!!

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1 Welcome to Environmental Science!!!

2 The Sun

3 Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 million earths inside the sun! 70% Hydrogen, 28% Helium, 2% other stuff.

4 Distance to the sun The average earth-sun distance is called an Astronomical Unit (AU) 92.8 Million Miles Keppler knew the distance to the planets in terms of the Earth- Sun distance, but not the distance itself (in meters)

5 Interior of the Sun VERY hot (27 million F) and dense (150 times denser than water) in the center (core) Density & Temp drop rapidly toward the outside 10,000 F at the surface

6 the Sun The sun is far away (93 million miles) And that s why it looks so small! The sun is hot (10,000 F on surface) The sun is big (1 million Earth s fit inside) Lots of gravity! This adds up to Temperature and pressure being very high on the sun.

7 Quick Chem review

8 Core of the sun The temperature and pressure on the sun is amazingly high. How high? High enough to push hyrdogen protons together. They fuse to form helium. What is this called?

9

10 Core of the sun Every second on the sun, 600 million tons of hydrogen is converted into 595 million tons of helium. Huh? You can t do that!

11 Why not? CONSERVATION OF MASS! The law implies that matter can neither be created nor destroyed, although it may be rearranged.

12 Core of the sun If 600 millions tons of hydrogen is converted into 595 million tons of helium what happens to the lost mass?

13 Core of the sun Einstein s theory of relativity states that under enough heat and pressure (like in the core of the sun) energy and mass are interchangeable (E = M) Therefore the lost mass is turned into HUGE amounts of energy (E=mc 2 ) Thanks Einstein. Again, nuclear fusion occurs in the core of the sun.

14 Fusion in the sun

15 The Sun s Future? The sun is currently crushing hydrogen into helium in the process of nuclear fusion. The sun is currently 70% hydrogen and 28% helium. How will these numbers change as time goes on?

16 Photosphere Photosphere brightest in optical this is where most of the light from the sun comes from. The spectrum is formed here.

17 Photosphere Optical light comes from here Sunspots are areas of intense magnetic field

18

19 The End

20 Chromosphere Activity starts at sunspots and gas travels along magnetic field lines If the gas loops back prominence If the gas escapes to the corona -- flare

21 Coron a The top picture is in X- ray The bottom two are in optical from SOHO You can see material leaving the sun

22 Energy transfer The energy created in the center of the sun has to travel to the outside. This happens in an orderly fashion in the interior Near the outside, energy is transferred with convection

23 Measurements What we can measure Distance to Venus (radar) Apparent mag. of sun (and D) Period of the Earth s orbit (and D) Spectrum of the sun Sunspots What we can calculate Distance to the sun Absolute mag. (Luminosity) Mass of Sun Temperature, chemical composition, rotation Rotation Rotation, magnetic field

24 The sun as a main sequence star The sun is a G2 main sequence star with an absolute magnitude of 4.85 All main sequence stars change H to He All spectra come from the photospheres of the stars We can only detect the chromosphere and corona of a few stars besides the sun

25 Properties of Stars

26

27 Properties of Stars Brightness Luminosity (brightness and distance) Magnitude scale Temperature (Color, spectrum) Composition (Spectrum) Velocity, rotation, magnetic field (spectrum) Distance (parallax, comparison)

28 Triangulating the Stars Image from Nick Strobel s Astronomy Notes (

29 Brightness and Luminosity Apparent magnitude measures the brightness of a star The true property of the star is luminosity. Luminosity, the total power coming from the surface of a star, is measured using Absolute Magnitude

30 Calculating Magnitude s You need to know the distance to the star in question (parallax for the nearest stars harder for everything else) Then you can calculate the absolute magnitude, M

31 Putting it together: an HR diagram Luminosity is measured in Watts or absolute magnitude Brightness is measured in Watts/m 2 or apparent magnitude Temperature is measured in color or spectral type (OBAFGKM)

32 Types of HR diagrams Theorist s Observer s Color-magnitude

33 Absolute Magnitude Absolute Magnitude vs. Spectral Type Here is an HR diagram for a few hundred randomly selected stars from the HD catalog Notice the main sequence Spectral type

34 Luminosity Classes of Stars Again, on the basis of the appearance of the spectra of stars, astronomers discovered that the density of gas and the strength of gravity at the surface of a star indicate that some stars are much larger than other, even if their temperatures are the same. This difference is denoted by the luminosity class of a star. The sequence of luminosity classes is: Luminosity Class Name assigned to class: I or Ia Supergiants II Bright Giants III Giants IV Sub-giants V Dwarfs VI Sub-dwarfs The complete classification of a star is based upon the spectral type and luminosity class of a star. Thus, it turns out that the sun is classified as a G2V star. Our old friend Betelgeuse is an M1I star.

Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 m

Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 m The Sun Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 million earths inside the sun! 70% Hydrogen,

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