© 2004 Pearson Education Inc., publishing as Addison-Wesley 15. Our Star This weeks homework: 2 tutorials: “Formation of the Solar System” “Detecting Extrasolar.

© 2004 Pearson Education Inc., publishing as Addison-Wesley 15.1 Why Does the Sun Shine? What process creates energy in the Sun? Why does the Sun’s size remain stable? How did the Sun become hot enough for fusion in the first place? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Sun’s Energy Source The first scientific theories involved chemical reactions or gravitational collapse. chemical burning ruled out…it can not account for the Sun’s luminosity conversion of gravitational potential energy into heat as the Sun contracts would only keep the Sun shining for 25 million years late 19 th -century geological research indicated the Earth was older than that Development of nuclear physics led to the correct answer the Sun generates energy via nuclear fusion reactions Hydrogen is converted into Helium in the Sun’s core the mass lost in this conversion is transformed into energy the amount of energy is given by Einstein’s equation: E = mc 2 given the Sun’s mass, this will provide enough energy for the Sun to shine for 10 billion years

© 2004 Pearson Education Inc., publishing as Addison-Wesley Striking a Balance The Sun began as a cloud of gas undergoing gravitational collapse. the same heating process, once proposed to power the Sun, did cause the core of the Sun to get hot & dense enough to start nuclear fusion reactions Once begun, the fusion reactions generated energy which provided an outward pressure. This pressure perfectly balances the inward force of gravity. deep inside the Sun, the pressure is strongest where gravity is strongest near the surface, the pressure is weakest where gravity is weakest This balance is called gravitational equilibrium. it causes the Sun’s size to remain stable

© 2004 Pearson Education Inc., publishing as Addison-Wesley Core T = 1.5 x 10 7 K; depth = 0 – 0.25 R  This is where the Sun’s energy is generated. Interior Zones T < 8 x 10 6 K; depth = 0.25 – 0.86 R  Energy is transported through the interior. The interior is divided into two zones: Radiation Zone Convection Zone Boundary between them is at: T = 2 x 10 6 K; depth = 0.70 R 

© 2004 Pearson Education Inc., publishing as Addison-Wesley Chromosphere T = 1 – 5 x 10 4 K; depth = 2,500 km A thin layer above the photosphere where most of the Sun’s UV light is emitted. courtesy of SOHO/SUMER consortium SOHO is a project of ESA and NASA UV image of the Sun light emitted from neutral Helium at 20,000 K

© 2004 Pearson Education Inc., publishing as Addison-Wesley Corona T = 2 x 10 6 K; depth  600,000 km The hot, ionized gas which surrounds the Sun. –it emits mostly X-rays It can be seen in visible light during an eclipse. X-ray image (YOHKOH telescope) Visible image

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Cosmic Crucible Why does fusion occur in the Sun’s core? Why is energy produced in the Sun at such a steady rate? Why was the Sun dimmer in the distant past? How do we know what is happening inside the Sun? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley Why does fusion occur in the Sun’s core ? Nuclear fusion a reaction where heavier nuclei are created by combining (fusing) lighter nuclei. all nuclei are positively charged Electromagnetic force causes nuclei to repel each other. for fusion to occur, nuclei must be moving fast enough to overcome E-M repulsion this requires high temperatures & pressures When nuclei touch, the nuclear force binds them together

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Solar Thermostat The rate of fusion reactions depends on temperature. the higher the T, the faster the rate, the more energy is produced This fact, coupled with gravitational equilibrium, acts as a mechanism which regulates the Sun’s energy output. its energy output (luminosity) remains stable

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Solar Luminosity The Sun’s luminosity is stable over the short-term. However, as more Hydrogen fuses into Helium: four H nuclei convert into one He nucleus the number of particles in Sun’s core decreases with time the Sun’s core will contract, causing it to heat up the fusion rate will increase to balance higher gravity a new equilibrium is reached for stability at a higher energy output the Sun’s luminosity increases with time over the long-term Models indicate the Sun’s luminosity has increased 30% since it formed 4.6 billion years ago. it has gone from 2.9 x 10 26 watts to today’s 3.8 x 10 26 watts

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Neutrino Problem Neutrinos come to us directly from the core of the Sun, a product of the proton-proton chain. We have detected them, proving that the theory of nuclear fusion reactions is correct! Solar neutrino problem was that we only detected about 30% - 50% of the neutrinos predicted by theoretic models. We have since discovered three types of neutrinos: electron ( e ), muon (  ), and tau (  ) our neutrino detectors can register only electron neutrinos Solved in 2002, neutrinos can change type after being created…

© 2004 Pearson Education Inc., publishing as Addison-Wesley 16.1 Snapshot of the Heavens How can we learn about the lives of stars, which last millions to billions of years? What two basic physical properties do astronomers use to classify stars? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley How can we Study the Life Cycles of Stars? A star can live for millions to billions of years. we will never observe a particular star evolve from birth to death so how can we study stellar evolution? The key is that all stars were not born at the same time. the stars which we see today are at different stages in their lives we observe only a brief moment in any one star’s life by studying large numbers of stars, we get a “snapshot” of one moment in the history of the stellar community we can draw conclusions just like we would with human census data…we do stellar demographics! The stars we observe also have different masses. by counting stars of different masses, we can determine how long stars of a given mass remain in a certain stage of life

© 2004 Pearson Education Inc., publishing as Addison-Wesley Classification of Stars Stars were originally classified based on: their brightness their location in the sky This classification is still reflected in the names of the brightest stars…those we can see with our eyes:  Orionis  Geminorum Order of brightness within a constellation Latin Genitive of the constellation

© 2004 Pearson Education Inc., publishing as Addison-Wesley Classification of Stars The old classification scheme told us little about a star’s true (physical) nature. a star could be very bright because is was very close to us; not because it was truly bright two stars in the same constellation might not be close to each other; one could be much farther away In the 20 th Century, astronomers developed a more appropriate classification system based on: a star’s luminosity a star’s surface temperature Since these properties depend on a star’s mass and its stage in life: measuring them allows us to reconstruct stellar life cycles

© 2004 Pearson Education Inc., publishing as Addison-Wesley 16.2 Stellar Luminosity What is luminosity and how do we determine it? How do we measure the distance to nearby stars? How does the magnitude of a star depend on its apparent brightness? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley Luminosity of Stars Apparent brightness refers to the amount of a star’s light which reaches us per unit area. the farther away a star is, the fainter it appears to us how much fainter it gets obeys an inverse square law its apparent brightness decreases as the (distance) 2 (App. Brightness) Flux = L / 4  d 2 Luminosity – the total amount of power radiated by a star into space. The apparent brightness of a star depends on two things: How much light is it emitting: luminosity (L) [watts] How far away is it: distance (d) [meters]

© 2004 Pearson Education Inc., publishing as Addison-Wesley Measuring Distances to Stars d = 1 / p If p is in arcsec and d is in parsecs A star with a parallax of 1 arcsec is 1 parsec distant From math on the triangle we can get 1 parsec  206,265 A.U. = 3.26 light years

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Brightness of Stars Astronomers still use an ancient method for measuring stellar brightness which was proposed by the Greek astronomer Hipparchus (c. 190 – 120 B.C.) This scale runs backwards: The bigger the number, the fainter the star Brightest stars are #1, next brightest are #2, etc.

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Modern Magnitude System apparent magnitude brightness of a star as it appears from Earth = -2.5 log (app bright) each step in magnitude is 2.5 times in brightness absolute magnitude the apparent magnitude a star would have if it were 10 pc away

© 2004 Pearson Education Inc., publishing as Addison-Wesley 16.3 Stellar Surface Temperature How are stars classified into spectral types? Does a star’s spectral type depend on its composition? What are the two main elements in all stars? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley Spectral Types of Stars Spectral types are defined by the: existence of absorption lines belonging to various elements, ions, & molecules in a star’s spectrum the relative strengths of these line However, spectral type is not determined by a star’s composition. all stars are made primarily of Hydrogen & Helium Spectral type is determined by a star’s surface temperature. temperature dictates the energy states of electrons in atoms temperature dictates the types of ions or molecules which exist this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum this fact was discovered by Cecilia Payne-Gaposchkin in 1925

© 2004 Pearson Education Inc., publishing as Addison-Wesley 16.4 Stellar Masses What is the most important property of a star? What are the three major classes of binary star systems? How do we measure stellar masses? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley Masses of Stars Mass is the single most important property of any star. at each stage of a star’s life, mass determines… what its luminosity will be what its spectral type will be The mass of a star can only be measured directly by … observing the effect which gravity from another object has on the star This is most easily done for two stars which orbit one another…a binary star!

© 2004 Pearson Education Inc., publishing as Addison-Wesley Binary Stars (two stars which orbit one another) Optical doubles two unrelated stars which are in the same area of the sky Visual binaries a binary which is spatially resolved, i.e. two stars are seen (e.g. Sirius)

© 2004 Pearson Education Inc., publishing as Addison-Wesley Binary Stars Spectroscopic binaries a binary which is spatially unresolved, i.e only one star is seen; the existence of the second star is inferred from the Doppler shift of lines.

© 2004 Pearson Education Inc., publishing as Addison-Wesley Binary Stars The stars orbit each other via gravity. So the laws of Kepler & Newton apply! Remember Newton’s version of Kepler’s Third Law: P 2 = 4  2 a 3 / G (m 1 + m 2 ) If you can measure the orbital period of the binary (P) and the distance between the stars (a), then you can calculate the sum of the masses of both stars (m 1 + m 2 ).

© 2004 Pearson Education Inc., publishing as Addison-Wesley 16.5 The Hertzsprung-Russell Diagram What is the Hertzsprung-Russell (HR) diagram? What are the major features of the HR diagram? How do stars differ along the main sequence? What determines the length of time a star spends on the main sequence? What are Cepheid variable stars and why are they important to astronomers? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Hertzsprung-Russell Diagram MVMV Spectral type bright faint hot cool A very useful diagram for understanding stars We plot two major properties of stars: Temperature (x) vs. Luminosity (y) Spectral Type (x) vs. Absolute Magnitude (y) Stars tend to group into certain areas

© 2004 Pearson Education Inc., publishing as Addison-Wesley Photo marks milestone in planet search Confirmed image shows hot planet near distant star The bright young star GQ Lupi is at the center of this image, and the outlying planet can be seen to the right, labeled "b." -astronomers have finally obtained the first photograph of a planet beyond our solar system New Result! - first directly imaged and confirmed companion to a sunlike star, marking the dawn of a new era in planet detection

© 2004 Pearson Education Inc., publishing as Addison-Wesley New Result! Planet ~1-2 times as massive as Jupiter Star GQ Lupi is like a young version of the Sun System is young, so the planet is rather warm, making it easier to see in the glare of its host star compared with more mature planets. Also, the planet is very far from the star — about 100 times the distance between Earth and the sun, another factor in helping to separate the light between the two objects. 3 images using the Very Large Telescope of the European Southern Observatory in Chile.

© 2004 Pearson Education Inc., publishing as Addison-Wesley Spectral Type Classification System O B A F G K M Oh Be A Fine Girl/Guy, Kiss Me! 50,000 K 3,000 K Temperature Each lettered type subdivided into numbered categories based on details of spectrum …A0 A1 A2 A3 A4 A5 A6 A7 A8 A9 F0 F1 … e.g. hottest A stars are A0, coolest A stars are A9 A9 are slightly hotter than F0

© 2004 Pearson Education Inc., publishing as Addison-Wesley Stellar Luminosity How can two stars have the same temperature, but vastly different luminosities? The luminosity of a star depends on 2 things: surface temperature surface area (radius) L =  T 4 4  R 2 The stars have different sizes!! The largest stars are in the upper right corner of the H-R Diagram.

© 2004 Pearson Education Inc., publishing as Addison-Wesley Mass-Luminosity Relation L  m 3.5 for main sequence stars only We use binary stars to measure directly the masses of stars of every type. This leads to the: As one moves to the upper-left of the main sequence: stars become more massive stars become even much more luminous x2 in mass -> x11.3 in Lum stars become fewer in number

© 2004 Pearson Education Inc., publishing as Addison-Wesley Mass–Luminosity Relation All main sequence stars fuse H into He in their cores. Luminosity depends directly on mass because: more mass means more weight from the star’s outer layers nuclear fusion rates must be higher in order to maintain gravitational equilibrium

© 2004 Pearson Education Inc., publishing as Addison-Wesley Lifetime on the Main Sequence How long will it be before MS stars run out of fuel? i.e. Hydrogen? How much fuel is there? M How fast is it consumed? L  M 3.5 How long before it is used up? M/L = M/M 3.5 = M -2.5

© 2004 Pearson Education Inc., publishing as Addison-Wesley Lifetime on the Main Sequence O & B Dwarfs burn fuel like a bus! M Dwarfs burn fuel like a compact car! Our Sun will last 10 10 years on the Main Sequence (MS Lifetime  = 10 10 yrs / M 2.5 )

© 2004 Pearson Education Inc., publishing as Addison-Wesley Lifetime on the Main Sequence So for example: B2 dwarf (10 M  ) lasts3.2 x 10 7 yr F0 dwarf (2 M  ) lasts1.8 x 10 9 yr M0 dwarf (.5 M  ) lasts5.6 x 10 10 yr But the Universe is 1.37 x 10 10 yr old! Every M dwarf that was ever created is still on the main sequence!!

© 2004 Pearson Education Inc., publishing as Addison-Wesley Cepheid Variables prototype:  Cephei F - G Bright Giants (II) whose pulsation periods (1-100 days) get longer with increased luminosity Distance Indicator!!

© 2004 Pearson Education Inc., publishing as Addison-Wesley The Instability Strip There appears to be an almost vertical region on the H-R Diagram where all stars within it (except on the Main Sequence) are pulsating and variable.

© 2004 Pearson Education Inc., publishing as Addison-Wesley 16.6 Star Clusters What are the two major types of star cluster? Why are star clusters useful for studying stellar evolution? How do we measure the age of a star cluster? Our goals for learning:

© 2004 Pearson Education Inc., publishing as Addison-Wesley Clusters are useful for studying stellar evolution! all stars are the same distance use apparent magnitudes all stars formed at about the same time they are the same age Plot an H-R Diagram!

© 2004 Pearson Education Inc., publishing as Addison-Wesley Cluster H-R Diagrams Indicate Age All stars arrived on the MS at about the same time. The cluster is as old as the most luminous (massive) star left on the MS. All MS stars to the left have already used up their H fuel and are gone. The position of the hottest, brightest star on a cluster’s main sequence is called the main sequence turnoff point.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? How can we learn about the lives of stars, which last millions to billions of years? By taking observations of many stars, we can study stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. What two basic physical properties do astronomers use to classify stars? Stars are classified by their luminosity and surface temperature. These properties, in turn, depend primarily on a star’s mass and its stage of life.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? What is luminosity and how do we determine it? A star’s luminosity is the total power (energy per unit time) that it radiates into space. It can be calculated from a star’s measured apparent brightness and distance, using the luminosity-distance formula: apparent brightness = luminosity / (4   distance 2 ). How do we measure the distance to nearby stars? The distance to nearby stars can be measured by parallax, the shift in theapparent position of a star with respect to more distant stars as the Earth moves around the Sun. How does the magnitude of a star depend on its apparent brightness? The magnitude scale runs backward, so a star of magnitude 5 star is brighter than a star of magnitude 18.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? How are stars classified into spectral types? Stars are classified according to their spectra, with different spectral types generally corresponding to different temperatures. In order from hottest to coolest, the major spectral types are O, B, A, F, G, K, and M. These are subdivided into numbered categories; for example, the hottest A stars are type A0 and the coolest A stars are type A9, which is slightly hotter than F0. Does a star’s spectral type depend on its composition? No. All stars are made primarily of hydrogen and helium, and the main factor in determining a star’s spectral type is its surface temperature. What are the two main elements in all stars? Hydrogen and helium.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? What is the most important property of a star? A star’s most important property is its mass, which determines its luminosity and spectral type at each stage of its life. What are the three major classes of binary star systems? A visual binary is a pair of orbiting stars that we can see distinctly. An eclipsing binary reveals its binary nature because of periodic dimming that occurs when one star eclipses the other as viewed from Earth. A spectroscopic binary reveals its binary nature because we can see the spectral lines of one or both stars shifting back and forth as the stars orbit each other.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? How do we measure stellar masses? We can directly measure mass only in binary systems in which we are able to determine the period and separation of the two orbiting stars. We can then calculate mass using Newton’s version of Kepler’s third law.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? What is the Hertzsprung-Russell (HR) diagram? It is the most important classification tool in stellar astronomy. Stars are located on the HR diagram by their surface temperature (or spectral type) along the horizontal axis and their luminosity along the vertical axis. Temperature decreases from left to right on the HR diagram. What are the major features of the HR diagram? Most stars occupy the main sequence, which extends diagonally from lower right to upper left. The giants and supergiants inhabit the upper right region of the diagram, above the main sequence. The white dwarfs are found near the lower left, below the main sequence.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? How do stars differ along the main sequence? All main sequence stars are fusing hydrogen to helium in their cores. Stars near the lower right of the main sequence are lower in mass and have longer lifetimes than stars further up the main sequence. Lower mass main-sequence stars are also much more common than higher mass stars. What determines the length of time a star spends on the main sequence? A star’s mass determines how much hydrogen fuel it has and how fast it fuses that hydrogen into helium. The most massive stars have the shortest lifetimes because they fuse their hydrogen much faster than lower mass stars.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? What are Cepheid variable stars and why are they important to astronomers? A Cepheid variable is a type of very luminous pulsating variable star that follows a period–luminosity relation, which means we can calculate its luminosity by measuring its pulsation period. Once we know a Cepheid’s luminosity, we can calculate its distance from the luminosity–distance formula. This property of Cepheids enables us to measure distances to many other galaxies in which these variable stars have been observed.

© 2004 Pearson Education Inc., publishing as Addison-Wesley What have we learned? What are the two major types of star cluster? Open clusters contain up to several thousand stars and are found in the disk of the galaxy. Globular clusters are much denser, containing hundreds of thousands of stars, and are found in both the halo and disk of the galaxy. Globular cluster stars are among the oldest stars known, with ages of about 12 to 15 billion years. Open clusters are generally much younger than globular clusters. Why are star clusters useful for studying stellar evolution? The stars in star clusters are all at roughly the same distance and, since they were born at about the same time, are about the same age. How do we measure the age of a star cluster? The age of a cluster is equal to the main-sequence lifetime of hottest and most luminous main-sequence stars remaining in the cluster. On an HR diagram of the cluster, these stars sit farthest to the upper left, defining the main-sequence turnoff point of the cluster.

© 2004 Pearson Education Inc., publishing as Addison-Wesley 15. Our Star This weeks homework: 2 tutorials: “Formation of the Solar System” “Detecting Extrasolar.

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© 2004 Pearson Education Inc., publishing as Addison-Wesley 15. Our Star This weeks homework: 2 tutorials: “Formation of the Solar System” “Detecting Extrasolar.

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Presentation on theme: "© 2004 Pearson Education Inc., publishing as Addison-Wesley 15. Our Star This weeks homework: 2 tutorials: “Formation of the Solar System” “Detecting Extrasolar."— Presentation transcript:

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