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Kirchhoff's laws,there are three types of spectra: continuum, emission line, and absorption line. High pressure, high temperature gas Low pressure,

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Presentation on theme: "Kirchhoff's laws,there are three types of spectra: continuum, emission line, and absorption line. High pressure, high temperature gas Low pressure,"— Presentation transcript:



3 Kirchhoff's laws,there are three types of spectra: continuum, emission line, and absorption line. High pressure, high temperature gas Low pressure, high temperature gas Cool gas in front of continuous spectra source

4 Hydrogen Helium Oxygen Neon Iron


6 Hydrogen Continuum Absorption Lines


8 Doppler effect –Waves compressed with source moving toward you Sound pitch is higher, light wavelength is compressed (bluer) similar in light and sound –Waves stretched with source moving away from you Sound pitch is lower, light wavelength is longer (redder)

9 Red Shift

10 If two stars are similar and one star is 3 times as far away, as the other, its intensity will be 1/9. Inverse square of light


12 Stars are different colors, because they are different temperatures

13 Spectral Classification O B A F G K M 35,000 K3,000 K Sun(G2) A5 K7 Annie Cannon classified stars according to the strength of the hydrogen absorption lines in the sequence A, B, C….P These spectral classes were changed to a temperature-ordered sequence and some were discarded, finally leaving : Oh, Be A Fine Girl (Guy) Kiss Me Subclasses

14 The Spectral Sequence BluestReddest Spectral Sequence is a Temperature Sequence HottestCoolest 50,000K1300K O B A F G K M L

15 O Stars B Stars T = 11, ,000 K; Strong He lines; very weak H lines A Stars Hottest Stars: T>30,000 K; Strong He + lines; no H lines T = ,000 K; Strongest H lines, Weak Ca + lines. F Stars T = K; H grows weaker Ca + grows stronger, weak metals begin to emerge.

16 G Stars T = K; Strong Ca +, Fe + and other metals dominate, K Stars T = K; Strong metal lines, molecular bands begin to appear M Stars T = K; strong molecular absorption bands particularly of TiO Solar Spectrum 4000 A 7000 A

17 Quantum Mechanics Electrons can only orbit the nucleus in certain orbits. n =1 First orbital: Ground State) Lowest energy orbit.

18 Up absorption Down emission Hydrogen Spectrum Hydrogen ( 1 H) consists of: A single proton in the nucleus. A single electron orbiting the nucleus.

19 Emission Lines: Balmer Lines When an electron jumps from a higher to a lower energy orbital, a single photon is emitted with exactly the energy difference between orbitals. No more, no less.

20 Absorption Lines: Balmer Lines An electron absorbs a photon with exactly the energy needed to jump from a lower to a higher orbital. No more, no less.

21 Hydrogen lines absent in the hottest stars because, photons ionize electrons. They are also absent in the coolest stars because, photons don’t have enough energy to move the electrons from n=2 to higher energy levels. No electrons, no lines.

22 In 1905, Danish astronomer Hertzsprung, and American astronomer Russell, noticed that the luminosity of stars decreased from spectral type O to M. To bring some order to the study of stars, they organize them in the HR diagram.

23 H–R Diagram White Dwarfs Giants Supergiants Main Sequence

24 As you move up the H-R diagram on the Main Sequence from M to O, the stars get hotter and larger

25 Star Formation “ All we are is dust in the wind” - Kansas Back to this is your life

26 (GMC) in Orion About 1000 GMCs are known in our galaxy These clouds lie in the spiral arms of the galaxy Protostars form in cold, Giant Molecular Clouds

27 The Cone Nebula Examining a Star Forming Region

28 Giant Molecular Clouds (GMC) are mostly composed of molecular hydrogen. Properties: Radius ~50 pc (~160 ly) Mass ~10 5 M sun Temperature: K Also, small amounts of He,and others

29 Size of cloud – large, Compression area - small A shockwave is needed to trigger formation, and to compress the material. GMC’s resist forming stars because of internal pressure (kinetic energy) so, a cooler gas is needed.

30 Sources of Shockwaves: 1.S upernova explosions: Massive stars die young. 2. Previous star formation can trigger more formations Spirals arms are probably rotating shock waves. 3. Spiral arms in galaxies like our Milky Way:

31 View all images An expanding supernova explosion, occurring about 15,000 years ago.

32 Gravity Contraction As they heat up, blobs glow in the infrared, but they remain hidden. As the cloud is compressed, cool blobs contract into individual stars. The blobs glow faintly in radio or microwave light.

33 As protostar compresses: Density increases Temperature rises. Photospheres (~3000K) Rotation increases as it shrinks in size. What types of stars form ? OB - Few AFG - More KM - Many, Many

34 Many of the cooler stars, spectral classes G,K,M, become heavy gas-ejecting stars called T-Tauri stars. Stars blows away their cocoon Leave behind a T Tauri star with an accretion disk and a jet of hot gas.

35 False Color: Green = scattered starlight and red = emission from hot gas. A T-Tauri star can lose up to 50% of its mass before settling down as a main sequence star.

36 Motion of Herbig-Haro 34 in Orion You can actually see the knots, called Herbig-Haro objects, in the jet move with time They can have wind velocities of km/s. This phase lasts about 10 million years.

37 When core temperature ~ 10 Million K: Core ignites, P-P chain fusion begins Settles slowly onto the Main Sequence Has a rotating disk, from which planets might form. Collapse is slower for lower masses : 1 M sun (solar Mass) ~30 Myr 0.2 M sun ~1 Billion years Low-Mass Protostars

38 Actual Protoplanetary Disks The disks are 99% gas and 1% dust. The dust shows as a dark silhouette against the glowing gas of the nebula.

39 When core Temperature >10 Million K: Ignite first P-P Chain then CNO fusion in the core. High-Mass Protostars Collapse is very rapid: 30 solar mass protostar collapses in ~30,000 years

40 near the stars Clouds are blown away from the new stars


42 Protostars! The Cocoons of proto-stars are exposed when the surrounding gas is blown away by winds and radiation from nearby massive stars.

43 Finally: Pressure=Gravity & collapse stops. Becomes a Zero-Age Main Sequence Star, (ZAMS). The Main Sequence Core temperature & pressure rise Collapse begins to slow down

44 Pre-main sequence evolutionary tracks Most everything about a star's life depends on its MASS.

45 Meanwhile, back in the GMC, things are still happening



48 The original stars are growing, especially O & B stars.


50 Stars Form in Clusters Our own Sun is part of an open cluster that includes Alpha Centauri and Barnard's star. Gravitational interactions will cause some stars to eventually leave over time

51 Extreme :Minimum Mass: ~0.08 M sun Below this mass, the core never gets hot enough to ignite H fusion. Star becomes a Brown Dwarf Resemble "Super Jupiters" Only about 100 are known Shine mostly in the infrared

52 The core of a very massive star gets so hot: Radiation pressure overcomes gravity, star becomes unstable & disrupts. Upper mass limit is not well known. Such stars are very rare. Extreme :Maximum Mass: M sun

53 Main Sequence Star spends 90% of their life on the MS

54 The star neither expands nor contracts. Stars on the Main Sequence, are in Hydrostatic Equilibrium. Gravity pulling inward wants to contract the star Pressure pushing outward wants to make the star expand

55 Core-Envelope Structure Outer layers press down on the inner layers. The deeper you go, the greater the pressure. The star develops a : hot, dense, compact central CORE surrounded by a cooler, less dense, ENVELOPE CORE Core Envelope

56 Energy is transferred inside stars by: Radiation (core) Energy is carried by photons from core. Photons hit atoms and get scattered. Slowly stagger to the surface Takes ~1 Million years to reach the surface. Convection (Envelope) Energy carried from hotter regions to cooler regions above by the motions of the gas. Everyday examples of convection are boiling water.

57 Energy in a Main-Sequence star is generated by fusion of H into He This process is performed in two ways 1. Proton-Proton (P-P) Chain: (Low mass stars) 4 1 H into 1 4 He. + energy. Efficient at low core Temperatures (T C <18M K) 2. CNO Cycle: (High mass stars) Carbon acts as a catalyst Efficient at high core Temperatures(T C >18MK )

58 Main Sequence Lifetimes Spectral TypeMass (Solar masses) Main sequence lifetime (million years) O5401 B01610 A F BY G BY K BY M BY More massive stars have the shorter life time O & B stars burn fuel like an airplane! M stars burn fuel like a compact car! Every M dwarf ever created is still on the main sequence!!

59 “It’s the end of the world as we know it”. REM Death of Low Mass Star

60 The End-States for Low and High Mass Stars Initial Stellar MassFinal Core MassFinal State White dwarf Neutron Star > 30> 3.0 Black hole

61 Evolution of Low-Mass Stars Main Sequence Phase Energy Source: H core fusion (P-P cycle) Slowly builds up an inert He core Lifetime: ~10 Byr for a 1 M sun star( Sun) ~10 Tyr for a 0.1 M sun star (red dwarf)

62 Outer layer expands and cools Star becomes a Red Giant He core collapses and heats up High temperatures ignites H burning in a shell When all H in core converted to He

63 Outside: The star gets brighter and redder, climbs up the Giant Branch. (Takes 1 Byr) Envelope ~ size of orbit of Venus

64 At the top of the Red Giant Branch: T core reaches 100 Million K He fusion begins in core Fusion of three 4 He nuclei into one 12 C nucleus. * A secondary reaction forms Oxygen from Carbon & Helium:

65 Helium Flash in the core. Short period of fast burning, then. star contracts, gets a little dimmer, but hotter. Moves onto the horizontal branch.

66 Structure: He-burning core H-burning shell Build up of a C-O core, still too cool to ignite Carbon Horizontal Branch Phase

67 After 100 Myr, core runs out of He. Inside: C-O core collapses and heats up He burning shell outside the C-O core H burning shell outside the He shell Outside: Star swells & cools

68 Climbs the Giant Branch again, slightly to the left of the original Giant Branch.

69 With weight of envelope gone, core never reaches 600 million K, no Carbon fusion Core contraction is stopped by electron degeneracy. Helium shell flash produces a new powerful explosion, that pushes the outer envelope outward. Core and Envelope separate.

70 A Planetary Nebula forms Hot C-O core is exposed, moves to the left Becomes a White Dwarf

71 Called planetary nebula because look like a tiny planet in a small telescope. The nebula expands at the ~ 35,000 to 70,000 miles/hour. Expanding envelope forms a ring nebula around the White Dwarf core. Ring is Ionized and heated by the hot central core of WD. Expands away in ~ 10,000 yrs

72 Planetary Nebulae Often asymmetric, possibly due to : Stellar rotation Magnetic fields The Hour Glass Nebula The Butterfly Nebula

73 White Dwarf Properties Radii ~ km (~ size of Earth!) Temp. – from 100,000 to 2500 K. So small, that they can only be seen if close-by, or in a binary systems. White Dwarf’s mass < than the Chandrasekhar mass (1.4 Solar Masses ).

74 White Dwarf Properties The core is tightly packed One teaspoon weighs about 5 tons. Shine by leftover heat, no fusion. Fade slowly, becoming a " Black Dwarf“. Takes ~10 Tyr to cool off, so none exists yet.

75 Sirius B Temp. 25,000 K Size: 92% Earth's diameter Mass: 1.2 solar masses Sirius B The most famous W.D. is Sirius’ companion. The mass of a star, in the size of a planet.

76 About half the stars in the sky are binaries. What about Binary Stars with one being a W.D. ! Mass could transfer from the star to the W.D. But wait that’s not all!

77 White Dwarf in a binary system….. White Dwarf Evolving (dying) star Roche Lobes Evolving (dying) star White Dwarf Accretion Disk Roche Lobe filled Evolving (dying) star I II III

78 Type 1a super NOVA !! A w.d. can take on material but, if the w.d. exceeds 1.4 solar masses, p owerful explosions take place, and they can repeat.

79 Since the Type 1a supernova is always a white dwarf they can be used to judge very great distances (using the inverse square law).

80 Stellar Graveyard High Mass Stars

81 The End-States for Low and High Mass Stars Initial Stellar Mass (Solar Mass) Final Core MassFinal State White dwarf Neutron Star > 30 > 3.0 Black hole

82 massive stars evolve more rapidly due to greater gravity. massive stars can produce heavier elements Evolution of High Mass Stars Massive stars go through about the same internal changes as low mass stars, except :

83 Evolution of High-Mass Stars O & B Stars (M > 8 M sun ): ( The James Dean of stars ) Burn Hot Live Fast Die Young Main Sequence Phase: Burn H to He in core using the CNO cycle Build up a He core, like low-mass stars But this lasts for only ~ 10 Myr

84 After H core exhausted: Inert He core contracts & heats up H burning in a shell The Envelope expands and cools Envelope ~ size of orbit of Jupiter

85 Moves horizontally across the H-R diagram, becoming a Red Super giant star Takes about 1 Myr to cross the H-R diagram.

86 Star becomes a Blue Supergiant. Core Temperature reaches 170 Million K Helium Flash : Helium Ignites producing C & O

87 He runs out in the core: Inert C-O core collapses & heats up H & He burning shells expand Star becomes a Red Supergiant again

88 C-O Core collapses until: T core > 600 Million K Ignites Carbon Burning in the Core. Carbon Burning: C fuse to form : Mg, Ne and O Carbon burning: 1000 years

89 . Fusion now takes place rapidly Neon burning: ~10 years Oxygen burning: ~1 year Silicon burning: ~1 day Finally builds up an inert Iron core. End of the road !

90 Core of a massive star at the end of Silicon Burning: Onion Skin

91 Collapse is final :Protons & electrons form neutrons & neutrinos.. At the start of Iron Core collapse: Radius ~ 6000 km (~radius of earth) Density ~ 10 8 g/cc A second later!!, the properties are: Radius ~50 km Density ~10 14 g/cc Collapse Speed ~0.25 c !

92 Material falling inwards is stopped by neutron degeneracy pressure. This material rebounds, causing the outer atmosphere, and shells, to be blown off in a violent explosion called a supernova.

93 The supernova star will outshine all the other stars in the galaxy combined. Elements heavier than Lead are produced in the explosion. The Famous Supernova SN 1987A type II Supernova


95 The Crab Nebula. This nebula is the result of a supernova that, exploded in The supernova was brighter than Venus for weeks before fading from view. The nebula is expanding at more than 3 million miles per hour.

96 Inside a Neutron Star Structure of a Neutron Star Diameter- 10 km in diameter 3> Mass > 1.4 times that of our Sun. One teaspoonful would weigh a billion tons! Rotation Rate: 1 to 100 rotations/sec

97 We will see regular, sharp pulses of light (optical, radio, X-ray), if its pointed toward the earth. Lighthouse Model: field generates a Spinning magnetic a strong electric field. Pulsar Magnetic axis is not aligned with the rotation axis.

98 The discovery of a pulsar in the crab nebula was the key connecting pulsars and neutron stars.

99 Black Holes We know of no mechanism to halt the collapse of a compact object with mass > 3 M sun.

100 The effect of gravity on light Relativity implies nothing can go faster than light. As you travel faster, time slows down, you get more massive and your length appears to get shorter.

101 Singularities Position Time singularity Event horizon Particle paths in a collapsing star If the core of a star collapses with more than 3 solar masses, electron degeneracy and neutron degeneracy can’t stop the gravitational collapse. The star collapses to a radius of zero, with infinite density and gravity—called a Singularity.

102 The Schwarzschild Black Hole The simplest of all black holes. A static, non-rotating mass. The Schwarzschild Radius defines the Event Horizon. We have no way of finding out what’s happening inside the “ Event horizon”

103 The Kerr Rotating Black Hole The singularity of a Kerr Black Hole is in infinitely thin ring around the center of the hole. The event horizon is surrounded by the ergosphere, where nothing can remain at rest. Here spacetime is being pulled around the rotating black hole.

104 It may be possible to avoid the singularity. An object is moving fast enough, can enter the ergosphere and fly out again. If the object stops in the ergosphere, it must fall into the Black Hole. General Relativity predicts Wormholes for Kerr Black Holes, but Astrophysicists are skeptical.

105 Various Black Holes Primordial – can be any size (created with Big Bang). “ Stellar mass ” black holes – must be at least 3 M o – many examples are known Intermediate black holes – range from 100 to 1000 M o - located in normal galaxies – many seen Massive black holes – about 10 6 M o – such as in the center of the Milky Way – many seen Supermassive black holes – about M o - located in Active Galactic Nuclei, have jets – many seen

106 Candidate For Black Hole Cygnus X-1 Binary Star w/ two objects: M=30 M sun primary, M=7 M sun companion Bright in X-rays. –Far too massive to be a white dwarf or neutron star. –The simplest interpretation is : – A 30 M  star and a 7 M  black hole Measured orbital motion of HDE

107 Evidence for BH The speed of the gas around the center indicates that the object at the centre is 1.2 billion times the mass of our Sun. 800 light years A disk of dust fueling a massive black hole in the centre of a galaxy.

108 Signature of a Black Hole

109 Thanks to the following for allowing me to use information from their web site : Nick Stobel Bill Keel Richard Pogge NASA


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