Chapter 19 Notes Stars Stars are bright balls of gas that are trillions
... through a prism. ii. When an element emits light, only some colors of the spectrum show up. d. Emission Lines i. Lines made when certain wavelengths of light or colors ii. Are given off by hot gases. iii. Each element has a unique set of bright emission lines e. Stars are classified according to how ...
... through a prism. ii. When an element emits light, only some colors of the spectrum show up. d. Emission Lines i. Lines made when certain wavelengths of light or colors ii. Are given off by hot gases. iii. Each element has a unique set of bright emission lines e. Stars are classified according to how ...
Space Science Unit - World of Teaching
... • 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 ...
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 ...
Northern and Southern Hemisphere Star Chart
... easily-spotted constellation of Orion the hunter. There you will see the red star Betelgeuse in his shoulder, the bluish white Rigel in his foot. To bring order to star catalogues, astronomers classify stars into what are called spectral types. This means stars are listed and placed in an order base ...
... easily-spotted constellation of Orion the hunter. There you will see the red star Betelgeuse in his shoulder, the bluish white Rigel in his foot. To bring order to star catalogues, astronomers classify stars into what are called spectral types. This means stars are listed and placed in an order base ...
Astronomy 10B List of Concepts– by Chapter
... • What is it Proper motion and how it’s measured? • How do we Measure the rotation rate of stars? • How do we Measure the magnetic fields of stars? • How were spectral type letters originally assigned (strength of H lines) • How are letters now assigned (types of spectral lines) • Spectral types and ...
... • What is it Proper motion and how it’s measured? • How do we Measure the rotation rate of stars? • How do we Measure the magnetic fields of stars? • How were spectral type letters originally assigned (strength of H lines) • How are letters now assigned (types of spectral lines) • Spectral types and ...
Exercise 9
... declination (think of this as a space latitude). The declination runs from -90° (celestial south pole) to +90° (celestial north pole). Both of these coordinates are laminated to the metal pole bases. In addition, the stars have been colored according to their spectral classes; blue balls represent O ...
... declination (think of this as a space latitude). The declination runs from -90° (celestial south pole) to +90° (celestial north pole). Both of these coordinates are laminated to the metal pole bases. In addition, the stars have been colored according to their spectral classes; blue balls represent O ...
Physics@Brock - Brock University
... • Describe luminosity classes and how they are determined. • Explain how the masses of stars are estimated, and apply Newton’s version of Kepler’s third law to determine such masses. • Describe the layout of the Hertzsprung-Russell (H-R) diagram, and infer a star’s size and evolutionary state based ...
... • Describe luminosity classes and how they are determined. • Explain how the masses of stars are estimated, and apply Newton’s version of Kepler’s third law to determine such masses. • Describe the layout of the Hertzsprung-Russell (H-R) diagram, and infer a star’s size and evolutionary state based ...
The Dramatic Lives of Stars
... Given the position of young stars in the HR diagram, which of the following is true? A 0.5 solar mass star mostly: ...
... Given the position of young stars in the HR diagram, which of the following is true? A 0.5 solar mass star mostly: ...
A search for planets around intermediate Mass Stars with the Hobby
... it is much more efficient to utilize the power of the radial velocity (RV) method by exploiting the many narrow spectral lines of GK-giants, the descendants of the main sequence A-F type stars, sufficient to achieve a < 10 ms−1 RV measurement precision. The GK-giant surveys provide constraints on th ...
... it is much more efficient to utilize the power of the radial velocity (RV) method by exploiting the many narrow spectral lines of GK-giants, the descendants of the main sequence A-F type stars, sufficient to achieve a < 10 ms−1 RV measurement precision. The GK-giant surveys provide constraints on th ...
Slides
... The spectrum of a star contains absorption lines which reflect the presence of particular atoms/ molecules. Their prominence is decided by temperature, surface gravity and the metal content of the stars. ...
... The spectrum of a star contains absorption lines which reflect the presence of particular atoms/ molecules. Their prominence is decided by temperature, surface gravity and the metal content of the stars. ...
Document
... • Computer models provide a “fast-forward” look at the evolution of stars. • Stars begin as clouds of gas and dust, which collapse to form a stellar disk. This disk eventually becomes a star. • The star eventually runs out of nuclear fuel and dies. The manner of its death depends on its mass. ...
... • Computer models provide a “fast-forward” look at the evolution of stars. • Stars begin as clouds of gas and dust, which collapse to form a stellar disk. This disk eventually becomes a star. • The star eventually runs out of nuclear fuel and dies. The manner of its death depends on its mass. ...
1 au d p = 1 au d
... The IMF is a more fundamental theoretical quantity which is obviously related to the star formation process. Note that the IMF only gives the distribution of stellar masses immediately after stars have formed - it is not the mass distribution in, say, the Galactic disk today. ...
... The IMF is a more fundamental theoretical quantity which is obviously related to the star formation process. Note that the IMF only gives the distribution of stellar masses immediately after stars have formed - it is not the mass distribution in, say, the Galactic disk today. ...
MULTIPLE CHOICE. Choose the one alternative that best
... 2) Studies of sunquakes, or helioseismology, have revealed that A) ʺsunquakesʺ are caused by similar processes that create earthquakes on Earth. B) the Sun generates energy by nuclear fusion. C) our mathematical models of the solar interior are fairly accurate. D) the Sun vibrates only on the surfac ...
... 2) Studies of sunquakes, or helioseismology, have revealed that A) ʺsunquakesʺ are caused by similar processes that create earthquakes on Earth. B) the Sun generates energy by nuclear fusion. C) our mathematical models of the solar interior are fairly accurate. D) the Sun vibrates only on the surfac ...
Study Guide – Midterm 3
... field. • “Precession” (gradual change in direction of major axis) of orbit of ...
... field. • “Precession” (gradual change in direction of major axis) of orbit of ...
Stellar Distances and Magnitudes
... Luminosity vs. Color of Stars • In 1911, Ejnar Hertzsprung investigated the relationship between luminosity and colors of stars in within clusters. • In 1913, Henry Norris Russell did a similar study of nearby stars. ...
... Luminosity vs. Color of Stars • In 1911, Ejnar Hertzsprung investigated the relationship between luminosity and colors of stars in within clusters. • In 1913, Henry Norris Russell did a similar study of nearby stars. ...
09astrophysics_2007Nov
... Classes: (hot to cold): O B A F G K M Subclasses: (hot to cold) B7 B8 B9 A0 A1 A2 etc. Russell suggests Oh Be A Fine Girl Kiss Me ...
... Classes: (hot to cold): O B A F G K M Subclasses: (hot to cold) B7 B8 B9 A0 A1 A2 etc. Russell suggests Oh Be A Fine Girl Kiss Me ...
Lecture 13 (pdf from the powerpoint)
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
Stellar Spectroscopy (GA 3.0) - National Optical Astronomy
... The three types of spectra are shown in the diagram below: continuous, emission line and absorption line. A continuous spectrum includes all wavelengths of light; i.e., it shows all the colors of the rainbow (case “a” in the diagram below). It is produced by a dense object that is hot, either a dens ...
... The three types of spectra are shown in the diagram below: continuous, emission line and absorption line. A continuous spectrum includes all wavelengths of light; i.e., it shows all the colors of the rainbow (case “a” in the diagram below). It is produced by a dense object that is hot, either a dens ...
The Hertzsprung-Russell Diagram
... you know the stars are all at the same distance. Then apparent brightness vs spectral type is basically the same as luminosity vs temperature. They found that stars only appear in certain parts of the diagram. ...
... you know the stars are all at the same distance. Then apparent brightness vs spectral type is basically the same as luminosity vs temperature. They found that stars only appear in certain parts of the diagram. ...
Stars Study Guide KEY
... Use this KEY to check your study guide for accuracy. Answers do not need to be word-for-word the same(but important facts/details should not be missing! Goal 1: Diagram the life cycle of stars. Explain how the cycle for low-mass stars differs from that of highmass stars. ...
... Use this KEY to check your study guide for accuracy. Answers do not need to be word-for-word the same(but important facts/details should not be missing! Goal 1: Diagram the life cycle of stars. Explain how the cycle for low-mass stars differs from that of highmass stars. ...
Stars: some basic characteristics
... How can we estimate stellar temperatures? Since stars emit a thermal spectrum (at least approximately), by measuring the ratio of a star’s brightness at a blue wavelength and a redder wavelength, we can estimate it’s temperature. ...
... How can we estimate stellar temperatures? Since stars emit a thermal spectrum (at least approximately), by measuring the ratio of a star’s brightness at a blue wavelength and a redder wavelength, we can estimate it’s temperature. ...
Spectra PowerPoint
... • Astronomers classify stars by the lines and bands in their spectra. – For example, if it has weak Balmer lines and lines of ionized helium, it must be an O star. ...
... • Astronomers classify stars by the lines and bands in their spectra. – For example, if it has weak Balmer lines and lines of ionized helium, it must be an O star. ...
annie jump cannon
... as a long-term project to obtain optical spectra of as many stars as possible and to index and classify stars by their spectra.” ...
... as a long-term project to obtain optical spectra of as many stars as possible and to index and classify stars by their spectra.” ...
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.