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On the Main Sequence What holds a star up while it is on the MS? Parts of a MS star How does energy get out? Radiation & Convection May take a million.

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Presentation on theme: "On the Main Sequence What holds a star up while it is on the MS? Parts of a MS star How does energy get out? Radiation & Convection May take a million."— Presentation transcript:



3 On the Main Sequence What holds a star up while it is on the MS? Parts of a MS star How does energy get out? Radiation & Convection May take a million years to reach the surface.

4 Brown Dwarfs : Stars with core mass <.08 Msun (failed stars). Brown Dwarfs do not get hot enough to fuse H, but they do fuse Deuterium for a very short time. Deuterium is an isotope of H, with a neutron. About 1,000 Brown Dwarfs have been found. They radiate in the infrared wavelength. The smallest stars

5 Red Dwarfs : Stars with a core mass of.08 to 0.4 solar mass Coolest and dimmest of all MS stars. They remain on MS hundreds of billions of years. When all the H is converted to He fusion ceases, they cool down, moving down and to the right in the H-R diagram.

6 Red Dwarfs are very low mass stars with no more than 40% of the mass of the Sun and represent the majority of the stars.. They have relatively low temperatures in their cores; red dwarfs transport energy from the core to the surface by convection. A low-mass main-sequence star of spectral classes M and L. Red dwarf stars range from about 0.6 solar mass at class M0 down to 0.08 solar mass in cool M

7 Death of Low Mass Star 0.5 - 1.4 White Dwarf Core Mass Final State

8 Thermodynamics When Fusion stops, core shrinks & temperature of core rises. When the Envelope expands its temperature cools down.

9 Main Sequence Phase Energy Source: H fusion in the core Using P-P cycle H fuses to He Slowly builds up an inert He core Evolution of Low-Mass Stars 0.5 - 1.4 Msun He Fusing Envelope

10 When the H in the core is almost completely converted into He, H fusion stops in core. The left over H is pushed out into a shell ring around the He core. The core collapses & heats up. Outer layer expands and cool forming a Red Giant The increasing temp will cause the H shell to fuse forming He that will join the core

11 (On the H_R Diagram) The star gets brighter and redder, climbs up the Giant Branch. (Takes 1 Byr) At the top of the Giant Branch, the star’s envelope is about the size of Venus’ orbit

12 The core will contract until it gets hot enough to fuse the He in the core into Carbon & Oxygen. When the fusion begins, the burning occurs rapidly because of the H shell burning and the He burning in the core. This is called the “Helium Flash”. Some of the outer layers are blown outward causing the star to loose mass.

13 The star gets hotter, and moves onto the Horizontal B ranch

14 C-O core collapses and heats up He burning shell outside the C-O core H burning shell outside the He burning shell The core never gets hot enough to fuse the Carbon & Oxygen Outside: Envelope swells &cools because of H & He burning Climbs the Asymptotic Giant Branch Once the He fuses and forms C & O, the core contracts.

15 Climbs the Giant Branch again, slightly to the left, and higher, becoming a super red giant..

16 With weight of envelope taken off, core never reaches Carbon fusion temp of 600 Million K Outer envelope gets slowly ejected. This is a non-violent ejection; a series of puffs or burps. Expanding envelope forms a ring nebula around the contracting C-O core. Core and Envelope separate, takes ~ 100,000 yr C-O core continues to contract:

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

18 Planetary Nebulae

19 Fig. 13.16c Butterfly Nebula

20 Outer shells of red supergiant “puffed off” Ejection not explosive Nebula shell expands Hot dwarf left behind Cools down to form a WD Planetary Nebula The nebula is ionized, and heated by the. Ultra- violet radiation from the hot star After ~ 50,000 years, the nebula spreads so far that the nebulosity simply fades from view.

21 White Dwarfs have a mass that is less than 1.4 Mo They will shine for a long time but no fusion is taking place. Contraction of the core is stopped by electron degeneracy. The electrons repel each other as they are pressed closer together and a White Dwarf forms. One teaspoon weighs about 5 tons.

22 Electron energy levels Only two electrons (one up, one down) can go into each energy level. In a degenerate gas, all low energy levels are filled.

23 White Dwarf’s mass < than the Chandrasekhar mass (1.4 Solar Mass) Radius (a little smaller than Earth!) Temp. – anywhere from 100,000 to 2500 K. White dwarfs shine by leftover heat, no fusion. WD will cool off and fade away slowly, becoming a "Black Dwarf“. Takes ~10 Tyr to cool off, so none exists yet. White Dwarfs are planetary in size, but have a stellar mass

24 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. White Dwarfs are so small, that they can only be seen if close-by, or in a binary systems.

25 A lone white dwarf is a cooling corpse but a white dwarf in a binary system can be revived

26 There is more !! A 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

27 Type 1a super NOVA !! W.D. can take on material but, if the W.D. exceeds 1.4 solar masses ( Chandrasekar limit) powerful explosions take place and they could happen more than once. The star will get down below 1.4 solar mass.

28 Since the Type 1a supernova is always a white dwarf they can be used to judge very great distances (using the inverse square law). Type Ia: No hydrogen lines in the spectrum Type II: Hydrogen lines in the spectrum There is a further subdivision of I into Ia, Ib, Ic

29 Low Mass Stars Sun Core forms a White Dwarf White Dwarf becomes a Black Dwarf (dead star) If the White Dwarf is a binary star, a Supernova type 1a can form, if its mass becomes greater than 1 ¼ solar masses Envelope separates from core and forms a planetary nebula Red Giant Becomes Red Giant when H is almost gone Only H, He in shells, C & O in core left C & O do not fuse Orbit out to almost Venus Becomes a Red Super Giant Red Super Giant

30 Of course you know the relationship is just going to end in a Type 1a supernovae...but I suppose its better to have transferred mass and exploded than to have never transferred mass at all... Wanted

31 Stellar Graveyard High Mass Stars 1.4 < M < 3.0 Neutron Star Final Core Mass Final State

32 massive stars evolve more rapidly due to rapid nuclear burning, and massive stars produce heavier elements Massive stars have the same internal changes as we saw in low mass stars, Evolution of Massive Stars except :

33 Evolution of High-Mass Stars High-Mass Stars O & B Stars core mass >1.4 and <3 M sun 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

34 Red Supergiant Phase After H core exhaustion: Inert He core contracts & heats up the H burning in a shell. Envelope expands due to the burning H shell and cools Envelope ~ size of orbit of Jupiter

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

36 Core Temperature reaches 170 Million K Helium Flash : Helium ignites This Helium flash is not as explosive as the one for low mass stars. Helium Fusion produces C & O in core: Star heats up and becomes a Yellow Supergiant.

37 Star becomes a Yellow Supergiant. Yellow

38 When He exhausted in core Inert C-O core collapses & heats up the H & He burning in shells. Star expands and becomes a Red Supergiant again

39 C-O Core collapses until: T core > 600 MillionK Carbon in the Core ignites. C fuses to form : Ne, and O Core at the end of Carbon Burning Phase:

40 1. Hydrogen burning: 10 Myr 2. Helium burning: 1 Myr 3. Carbon burning: 1000 years 4. Neon burning: ~10 years 5. Oxygen burning: ~1 year 6. Silicon burning: ~1 day Finally builds up an inert Iron core Nuclear burning continues past Helium Things happen fast! End of the line!!

41 Massive star at the end of Silicon Burning: Onion Skin of nested nuclear burning shells

42 Protons & electrons form neutrons & neutrinos. Collapse is final. At the start of Iron Core collapse: Radius ~ 6000 km (~R 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 !

43 Supernova explosion Neutron degeneracy pressure halts the collapse Material falling inwards rebounds. Outer layers of the atmosphere, including shells, are blown off in a violent explosion called a supernova. The star will outshine all the other stars in the galaxy combined.

44 The ejected material often attain speeds of 100,000 km/sec. Elements heavier than Lead are produced in the explosion and ejected into space. Stars do recycle. Close to 150 supernova remnants have been detected in the Milky Way. There are smaller numbers of massive stars and so smaller amount of explosions.

45 The Famous Supernova Before At maximum type II Supernova SN 1987A

46 Supernova remnants Cas A in x-rays (Chandra) Vela SN1998bu Remnant of SN386, with central pulsar (Chandra) Cygnus Loop (HST): green=H, red=S +, blue=O ++

47 The rings of SN 1987A are from previous mass loss

48 1a is binary with a White Dwarf Type II : Hydrogen lines in the spectrum

49 Supernova explosion 1, The iron core collapses 2. Neutrons stop the collapse 3. The rebound of the core sends shock waves causing an explosion that blows the outer atmosphere into space as a super nova

50 The Crab Nebula. A supernova that, according to the Chinese, exploded in 1054. Despite a distance of ~ 7,000 light-years, the supernova was brighter than Venus for weeks before fading from view after nearly two years. Even today, the nebula is still expanding at more than 3 million miles per hour.

51 Structure of a Neutron Star Diameter~ 12 km in diameter Mass -about 1.4 times that of our Sun. One teaspoonful of material would weigh a billion tons! Rotation Rate: 1 to 100 rotations/sec

52 The magnetic axis is miss-aligned with the rotation axis of the neutron star. The star's rotation sweeps the beams outward as it rotates. If we are in the sight path, will see regular, sharp pulses of light (optical, radio, X-ray.) Lighthouse Model: field generates a Spinning magnetic a strong electric field.


54 Pulsars: emitted sharp, 1 millisecond-long pulses every second at an extremely repeatable rate. A typical pulsar signal, received with a radio telescope

55 The connection between pulsars and neutron stars was the discovery of a pulsar in the crab nebula.

56 Iron

57 Proto-stars (born in cool gas GMC) Main Sequence Stars (H Fusion) Core Mass (CM) > 1.4 MO Red Super Giant Yellow Super Giant Supernova (Type II) Neutron Star Black Hole CM > 1.4 & < 3 CM > 3 Black Dwarf Red Giant Red Super Giant Planetary Nebula White Dwarf Binary can produce Type ia supernova Brown Dwarf CM<0,08 Core Mass (CM) 0.5- 1.4 MO Red Dwarf 0.08 - 0.5 MO CM 0.5 – 1.4 MO White Dwarf

58 Neutron Star High Mass Very High Mass Black Hole Supernova Massive Stars Outer layers of the atmosphere, including shells, are blown off in a violent explosion called a supernova Red Supergiant Massive star Becomes Yellow Supergiant when He exhausted Orbit size of Jupiter Becomes Red Supergiant Yellow Supergiant Becomes a Red Supergiant when H exhausted

59 Black Holes We know of no mechanism to halt the collapse of a compact object with mass > 3 M sun. It will collapse into a single point – a singularity: => Becoming a Black Hole!

60 Honeycutt H Has He Caused C No Ne Oxford O Student Si Injury (Iron) Fe To memorize this sequence, use this : Massive stars form the following:H, He, C, Ne, O, Si, Fe. Iron will not fuse. Low mass stars form only H, He, C, O

61 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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