The Evolutionary Cycle of Stars
... may briefly outshine its entire host galaxy before fading from view over several weeks or months. The explosion expels much or all of a star's material ...
... may briefly outshine its entire host galaxy before fading from view over several weeks or months. The explosion expels much or all of a star's material ...
Page R63 - ClassZone
... The Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram is a graph that shows stars plotted according to brightness and surface temperature. Most stars fall within a diagonal band called the main sequence. In the mainsequence stage of a star’s life cycle, brightness is closely related ...
... The Hertzsprung-Russell Diagram The Hertzsprung-Russell (H-R) Diagram is a graph that shows stars plotted according to brightness and surface temperature. Most stars fall within a diagonal band called the main sequence. In the mainsequence stage of a star’s life cycle, brightness is closely related ...
the lab handout here
... How does the temperature and luminosity of the Sun compare to that of the other stars on the Main Sequence? ________________________________________________________ ...
... How does the temperature and luminosity of the Sun compare to that of the other stars on the Main Sequence? ________________________________________________________ ...
21-2 - Laconia School District
... with a parallax. A parallax is a apparent change in position of an object when you look at it from different places. This means that if you stick your thumb out and close one eye, it will be in a spot. Then close that eye and open the other eye and it will change positions. This is an example of a p ...
... with a parallax. A parallax is a apparent change in position of an object when you look at it from different places. This means that if you stick your thumb out and close one eye, it will be in a spot. Then close that eye and open the other eye and it will change positions. This is an example of a p ...
Study Guide
... Period: ___________________ Date: ___________________ Study Guide Chapter 12 Stars, Galaxies, and the Universe ...
... Period: ___________________ Date: ___________________ Study Guide Chapter 12 Stars, Galaxies, and the Universe ...
g9u4c12part3
... they collapse in on themselves causing a massive explosion called a supernova. the remaining core of the supernova will eventually collapse to form a neutron star. A sphere only 10 km ...
... they collapse in on themselves causing a massive explosion called a supernova. the remaining core of the supernova will eventually collapse to form a neutron star. A sphere only 10 km ...
Slide 1
... The Suns Absorption Spectrum from 420 – 430 nm. (TOP) The emission spectrum of Iron (Bottom) ...
... The Suns Absorption Spectrum from 420 – 430 nm. (TOP) The emission spectrum of Iron (Bottom) ...
Homework, November 16, 2006 AST110-6
... mean by the stages we call hydrogen shell burning, helium burning, and double-shell burning? ...
... mean by the stages we call hydrogen shell burning, helium burning, and double-shell burning? ...
The Hertzsprung-Russell Diagram
... Most stars lie in the main sequence because if a star is hotter it is brighter. Thus you would expect stars of the same size but different temperatures to form a diagonal line since “hotter means brighter” That Main-Sequence is steeper than a ‘same-size diagonal” shows that larger mass ‘normal’ star ...
... Most stars lie in the main sequence because if a star is hotter it is brighter. Thus you would expect stars of the same size but different temperatures to form a diagonal line since “hotter means brighter” That Main-Sequence is steeper than a ‘same-size diagonal” shows that larger mass ‘normal’ star ...
Astrophysics 11 - HR Diagram
... You would see little evidence of Balmer Lines. You would see spectral lines for iron and calcium. You would also see evidence for molecules of ...
... You would see little evidence of Balmer Lines. You would see spectral lines for iron and calcium. You would also see evidence for molecules of ...
Stars…Giants, Supergiants, Dwarfs….
... When the pressure goes up, atoms “feel their neighbors” and have identity crises. The atomic energy levels, instead of being crisp and unique, get “fuzzed out”. “Fuzzed out” is technical terminology for a change in the energy which depends on how close the neighbors are, how many of them there are, ...
... When the pressure goes up, atoms “feel their neighbors” and have identity crises. The atomic energy levels, instead of being crisp and unique, get “fuzzed out”. “Fuzzed out” is technical terminology for a change in the energy which depends on how close the neighbors are, how many of them there are, ...
Main Sequence Stars
... Denmark, and Henry Norris Russell at Princeton University, around 1913. They plotted the locations of stars on a graph with the horizontal coordinate being spectral type (equivalent to temperature) and the vertical coordinate being absolute magnitude (equivalent to luminosity). The result, called th ...
... Denmark, and Henry Norris Russell at Princeton University, around 1913. They plotted the locations of stars on a graph with the horizontal coordinate being spectral type (equivalent to temperature) and the vertical coordinate being absolute magnitude (equivalent to luminosity). The result, called th ...
Star Characteristics
... Color + Temperature = Length of life Blue and white are the brightest Yellow stars last 10 billion years Red stars last longer It then turns into a super giant or red giant. ...
... Color + Temperature = Length of life Blue and white are the brightest Yellow stars last 10 billion years Red stars last longer It then turns into a super giant or red giant. ...
22.2 Stars Change Over Their Life Cycles
... All stars are balls of glowing gas that produce or have produced energy by fusion ...
... All stars are balls of glowing gas that produce or have produced energy by fusion ...
Stellar Properties and Stellar Evolution Study Guide Name Why
... 5. A shock wave may be the stimulus that causes a nebula to start condensing to form new ...
... 5. A shock wave may be the stimulus that causes a nebula to start condensing to form new ...
05spectralclasses
... • Why do spectral lines depend upon temperature? – Populations of various atomic states depends upon temperature • Degeneracy of levels – Stage of ionization • Depends on Pressure and density… ...
... • Why do spectral lines depend upon temperature? – Populations of various atomic states depends upon temperature • Degeneracy of levels – Stage of ionization • Depends on Pressure and density… ...
ASTR2050 Spring 2005 • In this class we will ...
... of individual stellar radii See Studio Laboratory this Friday ...
... of individual stellar radii See Studio Laboratory this Friday ...
Stars are classified according to their color
... • Stars are classified according to their color temperature: ...
... • Stars are classified according to their color temperature: ...
Slide 1
... B. Luminosity Class I-V (I--supergiant, V--main sequence). The Evolution of a Star: Hertzsprung-Russell Diagram (1910): A plot of Luminosity vs Surface Temperature, T (see overlay). A one solar mass star like the sun goes through the stages of: protostar, main sequence, red giant, planetary nebula, ...
... B. Luminosity Class I-V (I--supergiant, V--main sequence). The Evolution of a Star: Hertzsprung-Russell Diagram (1910): A plot of Luminosity vs Surface Temperature, T (see overlay). A one solar mass star like the sun goes through the stages of: protostar, main sequence, red giant, planetary nebula, ...
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.