How Is a Star`s Color Related to Its Temperature?
... On a clear night you have surely noticed that some stars are brighter than others. But stars also have different colors. Rigel is blue, and Betelgeuse is red. Capella and our sun are yellow. In this activity you will make your own HertzsprungRussell diagram. You will see how star brightness, color, ...
... On a clear night you have surely noticed that some stars are brighter than others. But stars also have different colors. Rigel is blue, and Betelgeuse is red. Capella and our sun are yellow. In this activity you will make your own HertzsprungRussell diagram. You will see how star brightness, color, ...
upperMS - CWRU Astronomy
... OBC stars are more difficult to “make” than OBN stars. Mass transfer in a binary can only lead to OBC by stripping part of the carbon-oxygen core of the primary. Carbon enhancement most likely from supernovae. Early forming massive stars could go supernova and enrich nearby protostars. ...
... OBC stars are more difficult to “make” than OBN stars. Mass transfer in a binary can only lead to OBC by stripping part of the carbon-oxygen core of the primary. Carbon enhancement most likely from supernovae. Early forming massive stars could go supernova and enrich nearby protostars. ...
Study Guide
... In words: “More massive M-S stars are more luminous.” Not true of Giants, Supergiants, or White Dwarfs. ...
... In words: “More massive M-S stars are more luminous.” Not true of Giants, Supergiants, or White Dwarfs. ...
Stellar Classification and Evolution What is a star? A cloud of gas
... from helium fusion _____________ much of their mass The ejected material expands and cools, becoming a planetary ________________ (which actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core _____________________ to form a Wh ...
... from helium fusion _____________ much of their mass The ejected material expands and cools, becoming a planetary ________________ (which actually has nothing to do with planets, but we didn’t know that in the 18th century when Herschel coined the term) The core _____________________ to form a Wh ...
(HR) Diagrams
... the laws of physics for the behavior of blackbodies (Wien’s law and the StefanBoltzmann law), it is these temperatures that account for why O and B stars have a bluish tint to their color and M stars have a reddish tint. ...
... the laws of physics for the behavior of blackbodies (Wien’s law and the StefanBoltzmann law), it is these temperatures that account for why O and B stars have a bluish tint to their color and M stars have a reddish tint. ...
Stars - TeacherWeb
... Characteristics of Stars Apparent Magnitude • Is the measure of the brightness of a celestial (star) object as seen from Earth • The lower the apparent magnitude the brighter the object • Negative numbers indicated extreme brightness • Positive numbers indicate faint stars ...
... Characteristics of Stars Apparent Magnitude • Is the measure of the brightness of a celestial (star) object as seen from Earth • The lower the apparent magnitude the brighter the object • Negative numbers indicated extreme brightness • Positive numbers indicate faint stars ...
The HR Diagram Interpreted (PowerPoint version)
... The HR Diagram Interpreted: Properties of Stars ...
... The HR Diagram Interpreted: Properties of Stars ...
The HR Diagram Interpreted: Properties of Stars
... The HR Diagram Interpreted: Properties of Stars ...
... The HR Diagram Interpreted: Properties of Stars ...
Document
... Mass of a star increases moving up the main sequence Gravitational pressure increases with mass, so to maintain equilibrium, fusion reactions in the core must generate a greater radiation pressure Star has to ‘burn’ at a higher temperature, giving it a greater luminosity L α M3.5 ...
... Mass of a star increases moving up the main sequence Gravitational pressure increases with mass, so to maintain equilibrium, fusion reactions in the core must generate a greater radiation pressure Star has to ‘burn’ at a higher temperature, giving it a greater luminosity L α M3.5 ...
Characteristics of Stars
... wire in a light bulb glow? Which color is hotter? Is Betelgeuse a cool or hot star? What color is Betelgeuse? What color is Rigel? Is Rigel a hot or cold star? 7. The brightness of a star depends on what two characteristics? What is a star’s apparent magnitude? What is absolute magnitude? What two t ...
... wire in a light bulb glow? Which color is hotter? Is Betelgeuse a cool or hot star? What color is Betelgeuse? What color is Rigel? Is Rigel a hot or cold star? 7. The brightness of a star depends on what two characteristics? What is a star’s apparent magnitude? What is absolute magnitude? What two t ...
The Stars - Department of Physics and Astronomy
... More On Solar Structure • Hydrogen fusion takes place in a core extending from the Sun’s center to about 0.25 solar radius • The core is surrounded by a radiative zone extending to about 0.71 solar radius – In this zone, energy travels outward through radiative diffusion ...
... More On Solar Structure • Hydrogen fusion takes place in a core extending from the Sun’s center to about 0.25 solar radius • The core is surrounded by a radiative zone extending to about 0.71 solar radius – In this zone, energy travels outward through radiative diffusion ...
Electromagnetic Radiation from the Sun
... and frequencies. Even to human eyes which can “see” only wavelengths in the visible spectrum, it appears white due to the blending of these colors. Why then are we taught in elementary school to color the sun yellow? 4. Why do we care so much about the Balmer series in atomic spectra? What is H? Th ...
... and frequencies. Even to human eyes which can “see” only wavelengths in the visible spectrum, it appears white due to the blending of these colors. Why then are we taught in elementary school to color the sun yellow? 4. Why do we care so much about the Balmer series in atomic spectra? What is H? Th ...
Fingerprints in Starlight: Spectroscopy of Stars Inquiry Questions
... frequencies. Even to human eyes which can “see” only wavelengths in the visible spectrum, it appears white due to the blending of these colors. Why then are we taught in elementary school to color the Sun yellow? 4. Why do we care so much about the Balmer series in atomic spectra? What is H ? The Ba ...
... frequencies. Even to human eyes which can “see” only wavelengths in the visible spectrum, it appears white due to the blending of these colors. Why then are we taught in elementary school to color the Sun yellow? 4. Why do we care so much about the Balmer series in atomic spectra? What is H ? The Ba ...
6. 1 Star Distances 6. 2 Apparent Brightness, Intrinsic Brightness
... The hydrogen Balmer lines are weak in cool stars because atoms are not excite(! out of the ground state. In hot stars, the Balmer lines are weak because atoms are excited to higher orbits or are ionized. Only at intermediate temperatures are the Balmer lines strong. ...
... The hydrogen Balmer lines are weak in cool stars because atoms are not excite(! out of the ground state. In hot stars, the Balmer lines are weak because atoms are excited to higher orbits or are ionized. Only at intermediate temperatures are the Balmer lines strong. ...
Lars Bildsten - nnpss
... your house, the heat is transported by diffusion of photons, which have a mean free path l, giving: ...
... your house, the heat is transported by diffusion of photons, which have a mean free path l, giving: ...
Lecture 13
... • These stars have finished fusing H to He in their cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hyd ...
... • These stars have finished fusing H to He in their cores are no longer on the main sequence. • They may be fusing He to Carbon in their core or fusing H to He in shell outside the core … but there is no H to He fusion in the core. • All stars become larger and redder after exhausting their core hyd ...
Exploring Space
... In 1961, President John F. Kennedy called for the US to put a person on the moon and began the space race. The race to the moon was undertaken in 3 ...
... In 1961, President John F. Kennedy called for the US to put a person on the moon and began the space race. The race to the moon was undertaken in 3 ...
White Dwarfs - Indiana University
... – All WDs have a common origin (PNN) with some hydrogen, upper limit of 10-4 solar masses to 10-15 solar masses of hydrogen (recall that 10-4 is the limit where H burning stops) – Only about 10-15 is needed to produce an optically thick H layer at the ...
... – All WDs have a common origin (PNN) with some hydrogen, upper limit of 10-4 solar masses to 10-15 solar masses of hydrogen (recall that 10-4 is the limit where H burning stops) – Only about 10-15 is needed to produce an optically thick H layer at the ...
Neutron Stars - Otterbein University
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
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 ...
Be Stars
... B-type stars with understrength helium lines and strong hydrogen spectra. Other chemically strange B-types stars are mercury–manganese stars. Finally, there are Be stars that show a prominent emission spectrum of hydrogen this is because they have a rapid rate of rotation, with an equatorial rotatio ...
... B-type stars with understrength helium lines and strong hydrogen spectra. Other chemically strange B-types stars are mercury–manganese stars. Finally, there are Be stars that show a prominent emission spectrum of hydrogen this is because they have a rapid rate of rotation, with an equatorial rotatio ...
Chapter 25 - Notes Super Size
... _________________, medium sized stars are in the middle of the Main Sequence like the Sun. Dwarfs, Giants, & Supergiants _________________of stars are not main sequence. Stars that are very hot (white-blue,) but are dim are called the _________________ Dwarfs. Stars that are cooler (red-______ ...
... _________________, medium sized stars are in the middle of the Main Sequence like the Sun. Dwarfs, Giants, & Supergiants _________________of stars are not main sequence. Stars that are very hot (white-blue,) but are dim are called the _________________ Dwarfs. Stars that are cooler (red-______ ...
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.