* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Download Star Formation 1/18/2015
Survey
Document related concepts
Formation and evolution of the Solar System wikipedia , lookup
Aquarius (constellation) wikipedia , lookup
Negative mass wikipedia , lookup
Planetary habitability wikipedia , lookup
Corvus (constellation) wikipedia , lookup
Big Bang nucleosynthesis wikipedia , lookup
Timeline of astronomy wikipedia , lookup
Stellar kinematics wikipedia , lookup
H II region wikipedia , lookup
Astronomical spectroscopy wikipedia , lookup
Type II supernova wikipedia , lookup
Standard solar model wikipedia , lookup
Stellar evolution wikipedia , lookup
Transcript
1/18/2015 Star Formation Large Scale Star Formation ____________________(_____) •Giant - millions of solar masses (M) •Cool , around 10 K •Molecules - H2, CO, CO2, CH, H2O, SiO, + many more Size of cloud - large Small compression area Localized Star formation Types of stars formed? Sizes of stars formed? ____________- Few ____________- More ____________- Many, Many OB Stars are the most influential Characteristics? _______! Type of light? _______ So? _______ light ionizes Hydrogen Produces large cloud of hot glowing gas - _____________ 1 1/18/2015 OB Stars H II Region Orion 2 1/18/2015 3 1/18/2015 4 1/18/2015 Small Scale Star Formation Less Mass - fewer stars formed Harder to see - IR 5 1/18/2015 High Mass Low Mass 6 1/18/2015 Main Sequence Middle Age for stars (and just about as exciting for them as for us) What do MS stars do? Why are more stars on the MS than anywhere else? Are they happy? What sort of retirement plan do they have? What makes the Sun shine? How does it produce energy? The answer is....... found in the ___________________________by Albert Einstein E= _________ ___________ - the fusing together of atoms to create energy (Not fission the breaking apart of atoms) More energy, less waste than fission Why not do it on the Earth? Requirements Densities around 100 gm/cc, Temperature over 13 million K 7 1/18/2015 Step 1 - proton + proton Deuterium, positron(e+), neutrino (n) Positron + Two Protons Deuterium n Neutrino Step 2 - Deuterium + proton He3, and energy Proton Helium 3 Deuterium g Gamma-ray Step 3 - He3 + He3 He4+ 2 protons Two Helium 3 Proton Helium 4 Proton 8 1/18/2015 Proton - Proton Cycle - What goes in? ________________________________ What comes out? ________________________________ How much energy produced? Gamma ray of 0.00000000004 Watts That’s not much! However, the Sun does this 100,000,000,000,000,000,000,000,000,000,000,000,000 times every second! End result a lot of energy! Energy is in the Core _____________ Zone _______ How does it get out? With great difficulty _____________ Zone ________ ____________ Zone Photosphere (surface) 9 1/18/2015 Main Sequence Trends Uniform characteristics from top to bottom At the top _______ Mass _______ Luminosity _______ Temperature _______ life At the bottom _______ Mass _______ Luminosity _______ Temperature _______ life MASS DETERMINES EVERYTHING! 10