Telescopes (continued). Properties of Stars.
... Spectral Type The surface temperature also determines the line spectrum of a star. Hot stars display lines of highly ionized elements, while cool stars show molecular lines. Stars are classified by assigning a spectral type. The hottest stars are called spectral type O, followed by B, A, F, G, K, M ...
... Spectral Type The surface temperature also determines the line spectrum of a star. Hot stars display lines of highly ionized elements, while cool stars show molecular lines. Stars are classified by assigning a spectral type. The hottest stars are called spectral type O, followed by B, A, F, G, K, M ...
dtu7ech11 - Fort Thomas Independent Schools
... the apparent color of its visible light. The insets show stars of about these surface temperatures. ...
... the apparent color of its visible light. The insets show stars of about these surface temperatures. ...
Life Cycle of Stars
... lower right when plotted according to luminosity and surface temperature on the Hertzsprung-Russell diagram ...
... lower right when plotted according to luminosity and surface temperature on the Hertzsprung-Russell diagram ...
powerpoint version
... they were coming from a common source. In between was a T Tauri star, buried in the ISM, visible only in the infrared. PHYS1142 ...
... they were coming from a common source. In between was a T Tauri star, buried in the ISM, visible only in the infrared. PHYS1142 ...
Space Science Unit
... • This chart uses surface temperature of the star and the absolute magnitude (brightness) of the star to help astronomers decide which phase of the star’s life cycle the star is in and other important information about the star. • Most stars are what we consider main sequence (including our sun). Th ...
... • This chart uses surface temperature of the star and the absolute magnitude (brightness) of the star to help astronomers decide which phase of the star’s life cycle the star is in and other important information about the star. • Most stars are what we consider main sequence (including our sun). Th ...
WebQuest-The-Life-Cycle-of-Stars-1
... and see pictures of the protostars of M16: The Eagle Nebula and other nebulae on this page. Continue by reading up on Main Sequence Stars and find out how our sun compares in mass to other stars. 1) Compare the mass of our sun to Sirius? To Proxima Centauri? 2) Based on its mass, will our sun be aro ...
... and see pictures of the protostars of M16: The Eagle Nebula and other nebulae on this page. Continue by reading up on Main Sequence Stars and find out how our sun compares in mass to other stars. 1) Compare the mass of our sun to Sirius? To Proxima Centauri? 2) Based on its mass, will our sun be aro ...
The colour-magnitude diagram
... Around 1910, Ejnar Hertzsprung and Henry Norris Russell plot stars in an `absolute magnitude – spectral type´ diagram They realize that stars do not appear at random but into specific areas: • most stars are located along the main sequence ...
... Around 1910, Ejnar Hertzsprung and Henry Norris Russell plot stars in an `absolute magnitude – spectral type´ diagram They realize that stars do not appear at random but into specific areas: • most stars are located along the main sequence ...
Star Powerpoint notes
... Stars range from more than 1000 times the Sun’s diameter to less than 1/100 the Sun’s diameter. Are most stars isolated from other stars, as the Sun is? No. In the vicinity of the Sun, two-thirds of the stars are ...
... Stars range from more than 1000 times the Sun’s diameter to less than 1/100 the Sun’s diameter. Are most stars isolated from other stars, as the Sun is? No. In the vicinity of the Sun, two-thirds of the stars are ...
Supernova’s
... • Starts off with a blue white color • Expands, cools, turns yellow • Pulsates for few months • Turns into Red Supergiant Star – 1,000 larger than our Sun ...
... • Starts off with a blue white color • Expands, cools, turns yellow • Pulsates for few months • Turns into Red Supergiant Star – 1,000 larger than our Sun ...
Death of Stars - Astronomy @ Walton High School
... Sketch a diagram of an HR diagram in your books. Annotate it appropriately. Try and do it from memory If you are struggling use the internet to help If you complete this try and describe what the diagram tells us about the birth and death of a star? ...
... Sketch a diagram of an HR diagram in your books. Annotate it appropriately. Try and do it from memory If you are struggling use the internet to help If you complete this try and describe what the diagram tells us about the birth and death of a star? ...
Document
... object with respect to a distant background is called parallax. As Earth moves in its orbit, astronomers are able to observe stars from two different positions. Astronomers measure the parallax of nearby stars to determine their distance from Earth ...
... object with respect to a distant background is called parallax. As Earth moves in its orbit, astronomers are able to observe stars from two different positions. Astronomers measure the parallax of nearby stars to determine their distance from Earth ...
Microsoft Power Point version
... 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 How long before it is used up? Time = Amount/(rate it is being used) ...
... 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 How long before it is used up? Time = Amount/(rate it is being used) ...
Foundations III The Stars
... classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements ...
... classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements ...
Lecture 13: The Stars –
... classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements • Provided a convincing argument that stars are mostly made of hydrogen. ...
... classification scheme. • Showed that the differences in spectra (absorption lines) are due to temperature and thermal ionization of atoms not abundance of elements • Provided a convincing argument that stars are mostly made of hydrogen. ...
Morning Announcements
... Tables I and II. 1) For each star, indicate its position on the graph below with a small ―x. The Sun (G2, 4.8) has been plotted for you. Plot the bright stars (Table I) and near stars (Table II) in different colors by using, for instance, pencil for the bright ones and blue ink for the near ones. NO ...
... Tables I and II. 1) For each star, indicate its position on the graph below with a small ―x. The Sun (G2, 4.8) has been plotted for you. Plot the bright stars (Table I) and near stars (Table II) in different colors by using, for instance, pencil for the bright ones and blue ink for the near ones. NO ...
Stars
... – 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 ...
... – 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 ...
Document
... 3. The temperature of the layer of gas that produces the visible light of the Sun is about _______. a) 15 million K, b) 300,000 K, c) 10 million K, d) 1 million K, e) 5800 K 4. What is the net result of the proton-proton chain? a) 2 heliums are fused into 1 carbon, 1 neutrinos + energy b) 4 hydrogen ...
... 3. The temperature of the layer of gas that produces the visible light of the Sun is about _______. a) 15 million K, b) 300,000 K, c) 10 million K, d) 1 million K, e) 5800 K 4. What is the net result of the proton-proton chain? a) 2 heliums are fused into 1 carbon, 1 neutrinos + energy b) 4 hydrogen ...
3.6 spectral classes
... • Absorption spectra are used to classify stars into nine principal types, called spectral classes. • Hydrogen lines are much stronger in the spectra of some stars than in the Sun’s spectrum. • Astronomers once mistakenly thought that these stars had more hydrogen than other stars. • They classified ...
... • Absorption spectra are used to classify stars into nine principal types, called spectral classes. • Hydrogen lines are much stronger in the spectra of some stars than in the Sun’s spectrum. • Astronomers once mistakenly thought that these stars had more hydrogen than other stars. • They classified ...
Stellar Death
... have to try to kill the stars. … Imagine if a man each day should have to try to kill the sun? We were born lucky” --Earnest Hemingway, The Old Man and the Sea ...
... have to try to kill the stars. … Imagine if a man each day should have to try to kill the sun? We were born lucky” --Earnest Hemingway, The Old Man and the Sea ...
Stellar Nucleosynthesis
... • For the majority of stars (~95%, corresponding to stars with initial masses of less than 8 M-Sun), direct nuclear burning does not proceed beyond helium, and carbon is never ignited. • Most of the nucleosynthesis occurs through slow neutron capture during the asymptotic giant branch (AGB), a brief ...
... • For the majority of stars (~95%, corresponding to stars with initial masses of less than 8 M-Sun), direct nuclear burning does not proceed beyond helium, and carbon is never ignited. • Most of the nucleosynthesis occurs through slow neutron capture during the asymptotic giant branch (AGB), a brief ...
galaxies and stars - Valhalla High School
... The temperatures of stars are on the x axis and the brightness is on the y axis. Most stars are on a diagonal line called the Main Sequence, where surface temperature increases as brightness increases. Giants and supergiants are higher and farther to the right. White dwarfs are hot but not v ...
... The temperatures of stars are on the x axis and the brightness is on the y axis. Most stars are on a diagonal line called the Main Sequence, where surface temperature increases as brightness increases. Giants and supergiants are higher and farther to the right. White dwarfs are hot but not v ...
Question: Fossilized footprints of Coelophysis
... boundary between Earth’s mantle and core? Key words: temperature, mantle, core, star Picking the right table: The Inferred Properties of Earth’s Interior table (p. NY28) has a diagram of Earth’s interior, along with graphs that show how pressure and temperature change with depth. From this table, yo ...
... boundary between Earth’s mantle and core? Key words: temperature, mantle, core, star Picking the right table: The Inferred Properties of Earth’s Interior table (p. NY28) has a diagram of Earth’s interior, along with graphs that show how pressure and temperature change with depth. From this table, yo ...
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.