Notes- Stars
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
... Life Cycle of Stars • The matter inside the star will be compressed so tightly that its atoms are compacted into a dense shell of neutrons. If the remaining mass of the star is more than about three times that of the Sun, it will collapse so completely that it will literally disappear from the univ ...
stellar spectra instructor notes
... classification, e.g. B0, B0.5, B1… B9, B9.5, A0, A … etc. The Otype stars were reclassified numerically, the original temperature ordering becoming O6, O7, O8, O9, O9.5, B0. Luminosity classes were added using the Saha ionization law, although the original scheme was an empirical system based upon t ...
... classification, e.g. B0, B0.5, B1… B9, B9.5, A0, A … etc. The Otype stars were reclassified numerically, the original temperature ordering becoming O6, O7, O8, O9, O9.5, B0. Luminosity classes were added using the Saha ionization law, although the original scheme was an empirical system based upon t ...
The Hidden Lives of Galaxies NSTA 2001
... But the sun does this 1038 times a second ! Sun has 1056 H atoms to burn ! ...
... But the sun does this 1038 times a second ! Sun has 1056 H atoms to burn ! ...
life cycle of stars
... • Size of the Earth with mass of the Sun “A ton per teaspoon” • Inward force of gravity balanced by repulsive force of electrons. ...
... • Size of the Earth with mass of the Sun “A ton per teaspoon” • Inward force of gravity balanced by repulsive force of electrons. ...
Slide 1
... This is called a Type Ia (or white dwarf) supernova. Type Ia supernovae can be identified by their spectra. Since they are formed by uniform, very repeatable conditions. Therefore, all Type Ia supernovae should reach the same maximum brightness. This makes them exceptionally reliable “standard candl ...
... This is called a Type Ia (or white dwarf) supernova. Type Ia supernovae can be identified by their spectra. Since they are formed by uniform, very repeatable conditions. Therefore, all Type Ia supernovae should reach the same maximum brightness. This makes them exceptionally reliable “standard candl ...
Stellar Evolution
... • H-burning shell dumps He into He-burning shell • He-flash (explosive feedback of 3a process [strong temperature dependence!] due to heating of He-burning shell) • Expansion and cooling of H-burning shell • H-burning reduced • Energy production in He-burning shell reduced ...
... • H-burning shell dumps He into He-burning shell • He-flash (explosive feedback of 3a process [strong temperature dependence!] due to heating of He-burning shell) • Expansion and cooling of H-burning shell • H-burning reduced • Energy production in He-burning shell reduced ...
Seating Chart for Wednesday PHOTO ID REQUIRED! SIT IN YOUR ASSIGNED ROW!
... field. • “Precession” (gradual change in direction of major axis) of orbit of ...
... field. • “Precession” (gradual change in direction of major axis) of orbit of ...
PowerPoint File
... unstable and sends thermal pulses through the star, throwing off the outer layers of the star into space. As the outer layers are peeled back, it reveals the extremely hot, ultraviolet-emitting carbon and oxygen core which ionizes the ...
... unstable and sends thermal pulses through the star, throwing off the outer layers of the star into space. As the outer layers are peeled back, it reveals the extremely hot, ultraviolet-emitting carbon and oxygen core which ionizes the ...
• This chapter concentrates on five goals:
... maximum strength is different for each type of atom or molecule. ...
... maximum strength is different for each type of atom or molecule. ...
How do atoms interact with light?
... From the relative strength of absorption lines (carefully accounting for their temperature dependence), one can infer the composition of stars. ...
... From the relative strength of absorption lines (carefully accounting for their temperature dependence), one can infer the composition of stars. ...
Life Cycles of Stars
... • Star expels outermost layers as Planetary Nebulae • Inert core left as white dwarf • Dwarf has such tiny surface area it takes billions of years to cool • Coolest (oldest?) known: 3900 K ...
... • Star expels outermost layers as Planetary Nebulae • Inert core left as white dwarf • Dwarf has such tiny surface area it takes billions of years to cool • Coolest (oldest?) known: 3900 K ...
What We Know About Stars So Far
... Stars can also be organized into different categories based on their absolute brightness. Scientists (Hertzprung and Russell (HR)) found that luminosity is dependent on the surface temperature of the star. When you plot stars on a graph using this system (comparing surface temperature and luminosit ...
... Stars can also be organized into different categories based on their absolute brightness. Scientists (Hertzprung and Russell (HR)) found that luminosity is dependent on the surface temperature of the star. When you plot stars on a graph using this system (comparing surface temperature and luminosit ...
Slide 1 - Physics @ IUPUI
... • The pulses normally come in the radio. • However, they also emit a lot of X-rays. • The Crab for example spins 30 times per ...
... • The pulses normally come in the radio. • However, they also emit a lot of X-rays. • The Crab for example spins 30 times per ...
File
... 3. Stellar Distances There are two ways that astronomers determine the distance of stars from an observer: a) Doppler Effect -The Absorption Spectrum produced by a star or planet changes depending on whether the star is moving towards or away from the observer. ...
... 3. Stellar Distances There are two ways that astronomers determine the distance of stars from an observer: a) Doppler Effect -The Absorption Spectrum produced by a star or planet changes depending on whether the star is moving towards or away from the observer. ...
chapter10
... 1 teaspoon of white dwarf material: mass ≈ 16 tons!!! Chunk of white dwarf material the size of a beach ball would outweigh an ocean liner! ...
... 1 teaspoon of white dwarf material: mass ≈ 16 tons!!! Chunk of white dwarf material the size of a beach ball would outweigh an ocean liner! ...
Stars
... Life span of a star depends on its size and mass. – Very large, massive stars burn their fuel much faster than smaller stars – Their main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
... Life span of a star depends on its size and mass. – Very large, massive stars burn their fuel much faster than smaller stars – Their main sequence may last only a few hundred thousand years – Smaller stars will live on for billions of years because they burn their fuel much more slowly ...
Stella Finger Prints
... process. Medium size stars like the Sun can fuel themselves longer than smaller stars by fusing helium into oxygen and carbon. Very large stars can continue the nuclear fusion process much, much longer, making heavier elements like calcium and iron. ...
... process. Medium size stars like the Sun can fuel themselves longer than smaller stars by fusing helium into oxygen and carbon. Very large stars can continue the nuclear fusion process much, much longer, making heavier elements like calcium and iron. ...
Lesson #5: Constellations - Center for Learning in Action
... Ask the students what they know about stars. Try to lead them towards the definition: Stars are massive shining spheres of hot gas. The stars you can see with your naked eye in the night sky are part of the Milky Way Galaxy, a huge system of stars that contains our solar system. Use pictures or over ...
... Ask the students what they know about stars. Try to lead them towards the definition: Stars are massive shining spheres of hot gas. The stars you can see with your naked eye in the night sky are part of the Milky Way Galaxy, a huge system of stars that contains our solar system. Use pictures or over ...
Siderius Nuntius… Light and the Science of Astronomy
... Wavelengths of emission lines unique “fingerprint” of element ...
... Wavelengths of emission lines unique “fingerprint” of element ...
Introduction to Stars ppt
... luminosity, but still much brighter than main sequence stars of same spectral type. The hot, white, small radius stars near the lower left are called white dwarfs. Giants and Supergiants are stars nearing the ends of their lives because they have already exhausted their core hydrogen. Surprisingly, ...
... luminosity, but still much brighter than main sequence stars of same spectral type. The hot, white, small radius stars near the lower left are called white dwarfs. Giants and Supergiants are stars nearing the ends of their lives because they have already exhausted their core hydrogen. Surprisingly, ...
The Life Cycle of the Stars
... Like all stars, our Sun was formed from a cloud of hydrogen gas and dust that almost certainly included the ashes from an earlier star gone supernova. In its death throes, it created elements heavier than iron that our solar system inherited. Gravity pulled the cloud together into a giant ball. When ...
... Like all stars, our Sun was formed from a cloud of hydrogen gas and dust that almost certainly included the ashes from an earlier star gone supernova. In its death throes, it created elements heavier than iron that our solar system inherited. Gravity pulled the cloud together into a giant ball. When ...
powerpoint - Physics @ IUPUI
... • Where does the energy the pulsars emit come from? • A) heat • B) nuclear fusion • C) gravity • D) Spin ...
... • Where does the energy the pulsars emit come from? • A) heat • B) nuclear fusion • C) gravity • D) Spin ...
AST 207 Homework 5 Due 14 October 2011
... 2. Life on Deneb. Here you will find out what it means to live near a giant like Deneb. Recall that the luminosity of a star, where T is its temperature and R is its radius. Star ...
... 2. Life on Deneb. Here you will find out what it means to live near a giant like Deneb. Recall that the luminosity of a star, where T is its temperature and R is its radius. Star ...
Lab 5 Takehome
... twice as big in radius has four times higher luminosity (because the surface area of a sphere is 4πr2 ...
... twice as big in radius has four times higher luminosity (because the surface area of a sphere is 4πr2 ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.