Time From the Perspective of a Particle Physicist
... • Stars range from .0001xLS to 1,000,000xLS Another scale: “magnitude” often used. A log scale to the power of ~2.5. YOU DON’T NEED TO KNOW. The lower the Mag the brighter the object PHYS 162 ...
... • Stars range from .0001xLS to 1,000,000xLS Another scale: “magnitude” often used. A log scale to the power of ~2.5. YOU DON’T NEED TO KNOW. The lower the Mag the brighter the object PHYS 162 ...
Document
... The extra burning to oxygen, 12C(,)16O raises this to 7.5 x 1017 erg g-1, or about 10% of what hydrogen burning gave. Because helium burning produces less energy and because the luminosities are actually greater, helium burning is a shorter stage in the life of a star than the main sequence. ...
... The extra burning to oxygen, 12C(,)16O raises this to 7.5 x 1017 erg g-1, or about 10% of what hydrogen burning gave. Because helium burning produces less energy and because the luminosities are actually greater, helium burning is a shorter stage in the life of a star than the main sequence. ...
The Later Evolution of Low Mass Stars (< 8 solar masses)
... The extra burning to oxygen, 12C(,)16O raises this to 7.5 x 1017 erg g-1, or about 10% of what hydrogen burning gave. Because helium burning produces less energy and because the luminosities are actually greater, helium burning is a shorter stage in the life of a star than the main sequence. ...
... The extra burning to oxygen, 12C(,)16O raises this to 7.5 x 1017 erg g-1, or about 10% of what hydrogen burning gave. Because helium burning produces less energy and because the luminosities are actually greater, helium burning is a shorter stage in the life of a star than the main sequence. ...
Stellar Physics - University of Reading
... Classical Mechanics and Optics Thermodynamics and Statistical Mechanics Atomic and Molecular Physics Ideas from Observational Astronomy ...
... Classical Mechanics and Optics Thermodynamics and Statistical Mechanics Atomic and Molecular Physics Ideas from Observational Astronomy ...
Astronomy Quiz 12 “Stars
... A. The statement is incorrect. High mass stars are the oldest stars. B. High mass inhibits the gravitational force, slowing fusion. C. High mass stars have atomic nuclei “bumping” against each other at rates high enough to trigger a supernova. D. High mass causes stronger gravity, which forces fusio ...
... A. The statement is incorrect. High mass stars are the oldest stars. B. High mass inhibits the gravitational force, slowing fusion. C. High mass stars have atomic nuclei “bumping” against each other at rates high enough to trigger a supernova. D. High mass causes stronger gravity, which forces fusio ...
Branches of Earth Science
... Light Year- Astronomers use light years to measure the distances ______________ stars o A light year is the distance that light ______________ in one year 9,460,730,472,580.8 km 5,878,630,000,000 miles Parallax- the apparent change in the ______________ of a star in the sky. o The change is due ...
... Light Year- Astronomers use light years to measure the distances ______________ stars o A light year is the distance that light ______________ in one year 9,460,730,472,580.8 km 5,878,630,000,000 miles Parallax- the apparent change in the ______________ of a star in the sky. o The change is due ...
ď - Google Sites
... Which of the following is the “best” conclusion of this laboratory activity a. A star’s temperature has no effect on its color. b. A star’s color determines its temperature. c. A star’s temperature determines its brightness. d. The hottest stars emit shorter wavelengths of light and appear bluer, wh ...
... Which of the following is the “best” conclusion of this laboratory activity a. A star’s temperature has no effect on its color. b. A star’s color determines its temperature. c. A star’s temperature determines its brightness. d. The hottest stars emit shorter wavelengths of light and appear bluer, wh ...
AS2001 - University of St Andrews
... Measure line strengths (equivalent widths) for individual elements. Equivalent Width measures the strength (not the width) of a line. ...
... Measure line strengths (equivalent widths) for individual elements. Equivalent Width measures the strength (not the width) of a line. ...
Lecture 10 Spectra of Stars and Binaries
... Colors of Stars • Stars are made of hot, dense gas – Con$nuous spectrum from the lowest visible ...
... Colors of Stars • Stars are made of hot, dense gas – Con$nuous spectrum from the lowest visible ...
Universe 8e Lecture Chapter 17 Nature of Stars
... sequence star or a white dwarf. These define the luminosity classes shown on the left occupying distinct regions on the HR diagram. ...
... sequence star or a white dwarf. These define the luminosity classes shown on the left occupying distinct regions on the HR diagram. ...
Branches of Earth Science Tools Used to Study Stars Constellations
... Spectroscope: Breaks light from a distant star into its characteristic colors o SPECTRUM: the band of colors that forms as light passes through a prism o Used to see if galaxies are moving away or toward the earth Telescopes: device that makes distant objects appear closer Types of Telescopes o Opti ...
... Spectroscope: Breaks light from a distant star into its characteristic colors o SPECTRUM: the band of colors that forms as light passes through a prism o Used to see if galaxies are moving away or toward the earth Telescopes: device that makes distant objects appear closer Types of Telescopes o Opti ...
Interpreting the HR diagram of stellar clusters
... Q: How do we know that they are very large? Red giant stars are no longer fusing hydrogen to helium in their cores. As we shall see soon, they have started to fuse helium nuclei into carbon. If we continue to watch as the stars age, we see a gradual progression of stars from the main sequence to the ...
... Q: How do we know that they are very large? Red giant stars are no longer fusing hydrogen to helium in their cores. As we shall see soon, they have started to fuse helium nuclei into carbon. If we continue to watch as the stars age, we see a gradual progression of stars from the main sequence to the ...
Homework 5 (stellar properties)
... 14. (2 pts.) If two stars orbit each other with a period of 6 years and a separation of 4 AU, what is their total mass? (Hint: Think Kepler.) What else would we need to know if we wanted to find the individual masses? (Assume that this is a visual binary.) ...
... 14. (2 pts.) If two stars orbit each other with a period of 6 years and a separation of 4 AU, what is their total mass? (Hint: Think Kepler.) What else would we need to know if we wanted to find the individual masses? (Assume that this is a visual binary.) ...
HR Diagram and Stellar Fusion
... • …Ejnar Hertzsprung and H. N. Russell, graph (see illustration) showing the luminosity of a star as a function of its surface temperature. The luminosity, or absolute magnitude, increases upwards on the vertical axis; the temperature (or some temperature-dependent characteristic such as spectral cl ...
... • …Ejnar Hertzsprung and H. N. Russell, graph (see illustration) showing the luminosity of a star as a function of its surface temperature. The luminosity, or absolute magnitude, increases upwards on the vertical axis; the temperature (or some temperature-dependent characteristic such as spectral cl ...
Ch16: The Milky Way
... The orbital speed (v) and radius (r) of a star on a circular orbit around the galaxy tells us the total mass (Mr) contained within that orbit ...
... The orbital speed (v) and radius (r) of a star on a circular orbit around the galaxy tells us the total mass (Mr) contained within that orbit ...
SECTION 30.2 Measuring the Stars 1. Constellations are a. the
... 5. When estimating the distance of stars from Earth, astronomers use the fact that nearby stars shift in position as observed from Earth, which is called a. parsec. b. parallax. c. precision. d. shafting. 6. Ancient Greek classification system based on how bright a star appears to be is ___________. ...
... 5. When estimating the distance of stars from Earth, astronomers use the fact that nearby stars shift in position as observed from Earth, which is called a. parsec. b. parallax. c. precision. d. shafting. 6. Ancient Greek classification system based on how bright a star appears to be is ___________. ...
PSC100 Transparant Replacement for Chapter 8 Measurement of
... * Calculate distance as speed of light x time of travel. Stellar Parallax * Measure angle to star at two different times. * Use largest base line possible, the diameter of Earth’s orbit around the Sun * This means data readings must be taken 6 months apart. * Calculate distance using triangulation. ...
... * Calculate distance as speed of light x time of travel. Stellar Parallax * Measure angle to star at two different times. * Use largest base line possible, the diameter of Earth’s orbit around the Sun * This means data readings must be taken 6 months apart. * Calculate distance using triangulation. ...
Sample final exam
... Essay section part one — Choose two of the following questions, and answer them in paragraph style or with drawings, as the question states. 19. On page 184, the text states “Understand the fact that we [the Milky Way] are moving toward M31 and that the Large Magellenic Cloud [LMC] is moving toward ...
... Essay section part one — Choose two of the following questions, and answer them in paragraph style or with drawings, as the question states. 19. On page 184, the text states “Understand the fact that we [the Milky Way] are moving toward M31 and that the Large Magellenic Cloud [LMC] is moving toward ...
The Milky Way
... • These units contain a LOT more material than what we actually went over in class. • You ARE responsible for understanding the topics covered in class (including details in the book that I may not have mentioned). • You are NOT responsible for other stuff in these chapters not covered at all in lec ...
... • These units contain a LOT more material than what we actually went over in class. • You ARE responsible for understanding the topics covered in class (including details in the book that I may not have mentioned). • You are NOT responsible for other stuff in these chapters not covered at all in lec ...
Powerpoint Presentation (large file)
... • Our own Sun is a rather average star of intermediate luminosity ...
... • Our own Sun is a rather average star of intermediate luminosity ...
Today`s Powerpoint
... While on Main Sequence, stellar core has H -> He fusion, by p-p chain in stars like Sun or less massive. In more massive stars, “CNO cycle” becomes more important. ...
... While on Main Sequence, stellar core has H -> He fusion, by p-p chain in stars like Sun or less massive. In more massive stars, “CNO cycle” becomes more important. ...
Powerpoint
... birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but make few UV photons. Why "H II Region? H I: Hydrogen atom H II: Ionized Hydrogen ...
... birth, so emission nebulae mark sites of ongoing star formation. Many stars of lower mass are forming too, but make few UV photons. Why "H II Region? H I: Hydrogen atom H II: Ionized Hydrogen ...
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.