2 Star Field as seen through the Hubble Space Telescope 2
3 Stars –1. Definition- a large gaseous body that generates energy through nuclear fusion in its core( Although the term is often also applied to objects that are in the process of becoming stars or to the remains of stars that have died.)2. Spectra (light) of Stars-- Allows astronomers to determine the star’sa. Compositionb. Temperaturec. Luminosityd. Velocity and Rotation rate in Spacee. MassThere are three different types of spectra produced when light is passed through a prism depending on the source of the light:
4 Stars (cont.) 2. Spectra (light) of Stars(cont.) A. Continuous Spectra-produced by a glowing solid, liquid, or very high density gas under certain conditions. (A normal light bulb produces a continuous spectra.)B. Absorption Spectra (Dark Line)-produced when a cooler gas lies between the observer and the object emitting a continuous spectra.- The gas absorbs some of the wavelengths of light leaving behind dark lines. The wavelengths absorbed depends on the composition of the gas and the temperature of the light source.-This is the spectra used to classify stars
5 Stars (cont.) 2. Spectra (light) of Stars(cont.) C. Emissions Spectra (Bright Line) –-produced when a glowing gas emits energy at specific wavelengths, characteristic of the element composing the gas.- used to study nebulae (Clouds of gas)
8 Stars (cont.) 3. Classifications of Stars- - Cooler Stars appear Red - Stars are essentially all made of the same material!!!- So WHY don’t they all have the same color or absorption line spectra?***The spectral difference is due to the difference in temperature of the star.The different temperatures also leads to the difference in colors that we see:- Hotter stars appear Blue- Cooler Stars appear RedA. Classification systemThe classification scheme used today divides the star up into seven major spectral or temperature classesO, B, A , F, G , K, M (Oh Be A Fine Girl (Guy) Kiss MeO – Hottest StarsM – Coolest Stars
10 Stellar Spectra Absorption Lines and Classifications
11 The Spectral Sequence Color Example O Spectral ClassTemperatureColorSpectral LinesExampleO30,000 to 50,000 KBlue-VioletIonized HeliumMinatakaB11,000 to 30,000 KBlue-WhiteNeutral HELIUM, HydrogenRigel, SpicaA7,500 to 11,000 KWhiteHydrogen (Strong)Sirius, VegaF5,900 to 7,500 KYellow-WhiteIonized MetalsProcyonG5,200 to 5,900 KYellowIonized CALCIUM,Ionized and Neutral MetalsThe Sun, CapellaK3,900 to 5,200 KOrangeNeutral MetalsArcturus, AldebaranM2,500 to 3,900 KRed-OrangeNeutral Metals,Molecular BandsBetelgeuse, Antares
12 Stars (cont.) 3. Classifications of Stars (cont)- A. Classification system (cont.)Since 1995 Astronomers have found new stars with surface temps even lower than spectral class M. These bodies which are not truly stars are called Brown Dwarfs- Heat is generated by contraction of gases not Nuclear Fusion. (Give off a lot of light in the infrared range.)B. H-R Diagram (Hertzsprung + Russel)- In 1912 classification scheme for stars invented- Stars are plotted according to:1. Luminosity (Absolute Magnitude)Brightest Stars at the Top2. Temperature (Spectral Class)Hotter Stars on the Left – Temperature Decreases as you move to the right
14 H-R Diagram of Some of the Most Prominent Stars in the Night Sky
15 Stars (cont.) 3. Classifications of Stars (cont)- B. H-R Diagram (cont.)3. Super-giants:- Very few rare stars that are bigger and brighter than typical giantstimes larger than the SunEX- Betelguese in Orion and Antares in Scorpius4. White dwarfs-- Remaining 9% of stars located in the lower left of the H-R Diagram- Although Very Hot, they have low luminosities due to their small size. (About the size of Earth)- (So dim can only be seen with a telescope)**- NO nuclear Fusion in core, only shines due to stored heat remaining from contraction of core.EX- Sirius B a companion star to Sirius A.
16 Stars (cont.) 3. Classifications of Stars (cont)- B. H-R Diagram (cont.)- Data points (Stars) on the diagram are NOT scattered randomly, but rather appear grouped in a few distinct regions:1. Main Sequence Stars:- About 90% of stars fall in this band stretching diagonally across the diagram.-Extends from the hot, luminous blue stars to the cool, dim red starsEx- Sun is a Main sequence star2. Giants:- Upper right hand side of diagram- Stars are both luminous and cool.In order to be as luminous as they are they must be large or giants- Approximately 10 to 100 times larger than our SunEx- Aldebaran in Taurus
19 H-R Diagram of the Brightest Stars in the Night Sky
20 Stars (cont.) 4. Stellar Evolution- - Stars DO NOT Live forever - Eventually the fuel which powers the nuclear reactions will run out and the star will cease to shine.- Changes that a star undergoes is referred to as its LIFE CYCLEA. Pre-Main Sequence Stage Star- Stars form in a dense cold, cloud of dust and gas (Mostly Hydrogen and Helium) called a Cocoon Nebula that begins to condense and form a Proto-starPossible Reasons for Condensation-a. Nearby Supernova Outburstb. Stellar Winds from hot nearby stars1. Proto-Star- Forms as the cloud condenses by the gravitational accretion of gas and dust. As it grows the contraction of the particles causes it to heat and begin to glow.
21 Stars (cont.) 4. Stellar Evolution (cont.) A. Pre-Main Sequence Stage (cont.)2. Protostar(cont.)- As protostar begins to heat and glow, it spins faster. Which starts Bipolar Outflow- NO FUSION YET – Heat only generated by contraction- Evidence of star formation:a. T-Tauri Starsb. Herbig-Haro Objects- Bipolar outflow collides with surrounding interstellar mediumc. EGG’s (Evaporating Gaseous Globules) smalll dense clouds in the act of contractingd. Protoplanetary disks (PROPLYDS)- If you see any of these there would most likely be a star forming there, but no planets and no fusion yet!!!!
31 Protoplanetary Disk- Photo taken by Hubble Space Telescope 31
32 Time Frame for Interstellar Evolution and Star Formation
33 Stars (cont.) 4. Stellar Evolution (cont.) A. Pre-Main Sequence Stage (cont.)2. Protostar(cont.)-Eventually contraction of gasses produces a high enough temperature at the core so that Nuclear Fusion Starts.***-Once Hydrogen fusion begins A MAIN SEQUENCE STAR IS BORN-Time frame for formation:A. The more mass there is, the more heat generated by contraction, the faster the Star forms(15- solar masses takes about 60,000 years to form)B. The less mass there is, the less heat generated by contraction, the slower the star forms( .5 solar masses takes 150 million years to form)C. Our sun probably took about 50 million years to form
36 Stars (cont.) 4. Stellar Evolution (cont.) B. Main Sequence Stars- - Once Hydrogen fusion begins the temperature and pressure in the core become strong enough to resist further contraction***- Hydrostatic Equilibrium is reached and the star becomes a stable Main sequence Star
38 Hydrostatic Equilibrium – The outward pressure of Nuclear Fusion is EQUAL to the inward Pull of GravityOur Sun- A Main Sequence Star
39 Hydrogen Vs. Helium Concentrations over the Life of the SUN
40 Stars (cont.) 4. Stellar Evolution (cont.) B. Main Sequence Stars (cont.)-- Time frame for Main sequence Star:1. More Massive Stars have to burn hotter and faster to resist gravitational contraction and therefore use up their fuel quicker.( A 15 solar mass star will burn for about 10 million years)** Higher internal temps makes these stars more luminous2. Less massive stars burn cooler and therefore can last longer( A .5 solar mass star will live for 100 billion years)** Low temps mean they are NOT as luminous3. Our Sun will fuse hydrogen (burn) for about 10 billion years
41 Stars (cont.) 4. Stellar Evolution (cont.) B. Main Sequence Stars (cont.)-- The short life span of massive stars implies that observed ones MUST be YOUNG!!! -> Would you expect to find Life around planets that orbit these massive stars???C. Post Main Sequence Stage-- Core’s Hydrogen supply runs out Fusion stops and core begins to contract under gravity.- The release of heat from contraction causes outer layers of hydrogen to fuse at an incredible rate and outer layer expands to become a RED GIANT STAR1. Red Giant or Super-giant:Very luminous due to its size but heat is spread out over a larger area so cooler than main sequence star….That’s why it turns red!!!Ex- Betelguese in Orion is a Star that has left the Main sequence stage and become a Red Supergiant.
44 Size of Supergiant, Betelguese, compared to orbit of Earth and Jupiter 44
45 Artist’s view of Earth and the Sun as a Red Giant Star 45
46 Stars (cont.)4. Stellar Evolution (cont.)C. Post main Sequence Stage (cont.)what happens to a star after Fusion stops depends on the original mass of the star.a. Low mass stars such as our sun will become Red giantsb. Higher Mass stars will expand much further to become Red Super-giants. (ex- Betelguese)
47 Stars (cont.) 4. Stellar Evolution (cont.) D. Death of a Star – 4 Solar Masses or less- Core of Red Giant will heat up due to contraction and start fusing helium to carbon at a very high rate.- When Helium runs out Fusion stops and Carbon Core begins to contract which again causes outer layers to heat up and expand.- Outer layers of gas will be ejected into space to form a Planetary Nebula:a huge shell of brightly glowing gas and dust lighted by the very hot exposed core of a star. (Will become White Dwarf Star)
58 Stars (cont.) 4. Stellar Evolution (cont.) D. Death of a Star - 4 Solar Masses or less (cont.)- Due to lack of mass carbon will not be able to condense enough to fuse into oxygen.- After Planetary Nebula Gases Spread out all that remains is aWhite Dwarf “Star”:- Stellar Core Remnant that has about 1.4 Solar Masses or less(About the mass of the SUN in what will shrink down to the size of the Earth – 1 teaspoon of matter would weigh 5 tons on earth)- Generates light and heat from contracting of matter under gravity (NOT FUSION)- Very hot but not luminous because of small size- Eventually will stop shrinking (electrons prevent further collapse) and will slowly cool off over 10’s of billions year and become a black dwarf.
59 Sirius B is a white dwarf star shown next to companion star, much brighter Sirius A.
60 White Dwarf Star and Companion Star which wandered to close to white Dwarf will probably lead to a Type I Supernova60
61 Stars (cont.) 4. Stellar Evolution (cont.) E. Death of a Star - 4 Solar Masses or more- Eventually due to extremely high mass of the Star, the core will eventually become hot enough to have fusion all the way to Iron- As it tries to fuse into heavier elements it actually loses energy that is supporting the core against gravity.- The core shrinks very rapidly and rebounds with a tremendous shock wave that blows apart the entire shell of the star in an explosion called a Supernova (Type II)
62 Stars (cont.) 4. Stellar Evolution (cont.) E. Death of a Star - 4 Solar Masses or more (cont.) Supernova (Type II)-- An explosion that causes a star to suddenly increases dramatically in brightness- Energy released is more than 100 times what the sun will radiate over ts entire 10 billion year lifetime- Very rare only about 1 every hundred years per galaxy (But there are billions of galaxies in the universe)- Star will outshine ALL the stars in its own galaxy COMBINED!!- May even be visible on earth during daylight hours-Nucleosynthesis- creation of heavier elements from lighter elements. (All elements heavier than Iron could only be created in Supernova Explosions)
63 Layers of a Super-Giant Red Star right prior to Supernova Explosion
64 Fusion up to Iron Releases energy but Fusion past Iron requires Energy
66 Supernova 1987 A – Same star field seen before supernova and after Supernova explosion
67 1987 Supernova in the Large Magellanic Cloud – Hubble Space Telescope 67
68 Veil Nebula – Remnant of a supernova that exploded about 15,000 years ago 68
69 Crab Nebula- A Remnant of a Supernova Explosion observed in 1054 AD which was bright enough to be seen during the day for over three weeks and during the night for 6 months69
70 Stars (cont.) E. Death of a Star - 4 Solar Masses or more (cont). -After Supernova explosion, stellar remnant is dependant upon how much of core is left.1. Neutron “Star”-- Core remnant is between 1.4 and 3.0 solar masses- Compression will be so great that protons and electrons of matter in core will combine to form neutrons – Atoms will be able to become very close together (Neutrons prevent further collapse)- Only Massive stars 5-10 solar masses can become Neutron stars- More Massive than a white dwarf star BUT only the size of a large city!!!!! (A paper clip made from a Neutron star would outweigh Mt. Everest )- Emit strong radio waves- Pulsars (Pulsating Radio waves) are evidence for the existence of Neutron Stars**- Pulsars detected in at Center of Both Crab and Veil Nebula(Remnants of a Supernova)
74 Stars (cont.) E. Death of a Star - 4 Solar Masses or more (cont). 2. Black Hole- Core remnant is greater than three solar masses- Compression of core is so great that even neutrons cannot hold the core up against its own gravity.- Gravity squeezes three solar masses into an infinitesimally small point (Smaller than the size of a pinhead) called a singularity-The area that separates the black hole from the surrounding space is called the Event Horizon. -> Within the event horizon gravity is so strong that even light does not travel fast enough to escape the gravity.(At the singularity the infinite gravity causes space and time to be jumbled and the laws of physics as we know them do not apply.)
75 Stars (cont.)E. Death of a Star - 4 Solar Masses or more (cont).2. Black Hole (cont.)- Black holes are usually detected in binary star systems where one of those stars has become a black hole- Only massive main sequence star (10 solar masses or more) will become black holes
76 Black Hole’s Effect on the Warping of Space-Time