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Structure of the Universe
... by combining smaller elements to form a larger one, specifically two hydrogen atoms form a helium atom, ...
... by combining smaller elements to form a larger one, specifically two hydrogen atoms form a helium atom, ...
Red Giants - Uplift North Hills Prep
... 2. by their color as determined by their blackbody curve 3. by their temperature and luminosity ...
... 2. by their color as determined by their blackbody curve 3. by their temperature and luminosity ...
Chapter 25 Study guide Answer Key
... 3) Which property of a star can be determined by its color? Temperature 4) About how many stars are estimated to occur in pairs or multiples? 50% ...
... 3) Which property of a star can be determined by its color? Temperature 4) About how many stars are estimated to occur in pairs or multiples? 50% ...
Slide 1
... 2. by their color as determined by their blackbody curve 3. by their temperature and luminosity ...
... 2. by their color as determined by their blackbody curve 3. by their temperature and luminosity ...
Slide 1 - Fort Bend ISD
... Absolute Magnitude • Brightness a star would have if it were at a standard distance from the Earth • Scientists study globular clusters to compare brightness of stars • All about same distance from Earth ...
... Absolute Magnitude • Brightness a star would have if it were at a standard distance from the Earth • Scientists study globular clusters to compare brightness of stars • All about same distance from Earth ...
ASTR-1020 Exam 2 Review Questions
... 5. What is the difference between apparent and absolute magnitudes and how are they related to the distance modulus? 6. What is meant by the color index of a star? To what physical parameter of a star (e.g., luminosity, chemical composition, temperature, size, etc.) is the color index related to? 7. ...
... 5. What is the difference between apparent and absolute magnitudes and how are they related to the distance modulus? 6. What is meant by the color index of a star? To what physical parameter of a star (e.g., luminosity, chemical composition, temperature, size, etc.) is the color index related to? 7. ...
TYPES OF STARS
... When astronomers look through their telescopes, they see billions of stars. How do they make sense of all these stars? The goal of this problem set is for you to understand that astronomers classify stars on the basis of two different criteria: (1) the intensity of one of the H absorption lines (cal ...
... When astronomers look through their telescopes, they see billions of stars. How do they make sense of all these stars? The goal of this problem set is for you to understand that astronomers classify stars on the basis of two different criteria: (1) the intensity of one of the H absorption lines (cal ...
The Hertzsprung-Russell Diagram
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
Slide 1
... Most of the brightest stars in the sky are 1) relatively hot small stars. 2) relatively cool giant stars. 3) relatively cool small stars. 4) relatively hot giant stars. ...
... Most of the brightest stars in the sky are 1) relatively hot small stars. 2) relatively cool giant stars. 3) relatively cool small stars. 4) relatively hot giant stars. ...
Chapter 27 Stars and Galaxies
... The shrinking, spinning region begins to flatten into a disk with a central concentration called a protostar ...
... The shrinking, spinning region begins to flatten into a disk with a central concentration called a protostar ...
Gemini
... million years), it is of intermediate age, and contains some post-main sequence stars (including several yellow and orange giants of spectral type late G to early K). Its hottest main sequence star is given as of spectral class B3 (Sky Catalogue 2000.0), and its Trumpler classification as III,3,r by ...
... million years), it is of intermediate age, and contains some post-main sequence stars (including several yellow and orange giants of spectral type late G to early K). Its hottest main sequence star is given as of spectral class B3 (Sky Catalogue 2000.0), and its Trumpler classification as III,3,r by ...
spectral-type
... Later they found many classifications were actually the same spectral type. Finally they realized that the strength of the hydrogen line correlated to the stars color, or temperature. ...
... Later they found many classifications were actually the same spectral type. Finally they realized that the strength of the hydrogen line correlated to the stars color, or temperature. ...
Eclipsing Binaries
... Later they found many classifications were actually the same spectral type. ...
... Later they found many classifications were actually the same spectral type. ...
Understanding Stars
... Astronomers can tell what elements are in a star by the lines in its spectrum Peak color determines the temperature Stars can be classified by their spectra – these are known as spectral types • They are lettered O B A F G K M from hottest/bluest/biggest to coolest/reddest/smallest – See Feb 7 - 10 ...
... Astronomers can tell what elements are in a star by the lines in its spectrum Peak color determines the temperature Stars can be classified by their spectra – these are known as spectral types • They are lettered O B A F G K M from hottest/bluest/biggest to coolest/reddest/smallest – See Feb 7 - 10 ...
Review Day
... between temperature and brightness. Identifies four characteristics of stars Temperature Brightness Color Category ...
... between temperature and brightness. Identifies four characteristics of stars Temperature Brightness Color Category ...
Lecture 9: Stellar Spectra
... Edward Pickering & Willamina Fleming made a first attempt to classify ~10,000 stars by their spectra. Sorted by Hydrogen absorption-line strength Spectral Type “A” = strongest Hydrogen lines Followed by types B,C,D, etc. (weaker) Problem: The other lines didn’t fit into this sequence ...
... Edward Pickering & Willamina Fleming made a first attempt to classify ~10,000 stars by their spectra. Sorted by Hydrogen absorption-line strength Spectral Type “A” = strongest Hydrogen lines Followed by types B,C,D, etc. (weaker) Problem: The other lines didn’t fit into this sequence ...
Elements and Isotopes - University of California, Berkeley
... Inside the Sun The temperature and pressure in the core are extreme enough for fusion (and the Sun’s gravity keeps them that way). Most energy is produced in the inner 20%. Convection carries the energy in the outer 30%. Most of the mass is in the inner 50% because the density is much higher. ...
... Inside the Sun The temperature and pressure in the core are extreme enough for fusion (and the Sun’s gravity keeps them that way). Most energy is produced in the inner 20%. Convection carries the energy in the outer 30%. Most of the mass is in the inner 50% because the density is much higher. ...
Astronomy Learning Objectives and Study Questions for Chapter 12
... E. white dwarfs 5. At the end of its main-sequence life, H-fusion in a medium mass star like Sol will shift to a shell outside the core and the star will become a _____. A. red dwarf B. red giant C. white dwarf D. blue-white supergiant E. supernova 6. The period during which an RR Lyrae or Cepheid v ...
... E. white dwarfs 5. At the end of its main-sequence life, H-fusion in a medium mass star like Sol will shift to a shell outside the core and the star will become a _____. A. red dwarf B. red giant C. white dwarf D. blue-white supergiant E. supernova 6. The period during which an RR Lyrae or Cepheid v ...
Stellar Evolution – Test Review Answers
... 7. Why do astronomers see an absorption spectrum when they take spectra of stars? The light that moves outward through the sun is a continuous spectrum since the interior regions of the sun have high density. However, when the light reaches the low density region of the solar atmosphere, some colors ...
... 7. Why do astronomers see an absorption spectrum when they take spectra of stars? The light that moves outward through the sun is a continuous spectrum since the interior regions of the sun have high density. However, when the light reaches the low density region of the solar atmosphere, some colors ...
Solutions to problems
... 1. Stars are composed principally of H and He, 75% and 25%, respectively. Stars also are composed of heavier elements produced by stars and disseminated by their explosive deaths. These heavier elements are important to prospect of planets because we believe the planets begin forming with the conden ...
... 1. Stars are composed principally of H and He, 75% and 25%, respectively. Stars also are composed of heavier elements produced by stars and disseminated by their explosive deaths. These heavier elements are important to prospect of planets because we believe the planets begin forming with the conden ...
hw4
... be determined by isolating certain spectral wavelength regions or by locating the peak wavelength. By making assumptions it is possible to estimate the radius and mass of a star from spectral characteristics. For example, giant stars have thinner spectral lines generally than small stars due to dens ...
... be determined by isolating certain spectral wavelength regions or by locating the peak wavelength. By making assumptions it is possible to estimate the radius and mass of a star from spectral characteristics. For example, giant stars have thinner spectral lines generally than small stars due to dens ...
Stars - Images
... Ways of tracking where the constellations are located during the different seasons of the year. Remember as the earth revolves around the sun, it also rotates causing the stars to “shift” in the ...
... Ways of tracking where the constellations are located during the different seasons of the year. Remember as the earth revolves around the sun, it also rotates causing the stars to “shift” in the ...
The H-R Diagram
... Color. The brightest stars are at the top and the hottest stars at the left. The radius increases diagonally towards the upper right. Only for main sequence stars (m.s. stars) the mass increases diagonally to the upper left. The stars in different areas have distinctly different physical properties ...
... Color. The brightest stars are at the top and the hottest stars at the left. The radius increases diagonally towards the upper right. Only for main sequence stars (m.s. stars) the mass increases diagonally to the upper left. The stars in different areas have distinctly different physical properties ...
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.