![Star Types](http://s1.studyres.com/store/data/008084033_1-6a5cb3631468e85d271aa680837a276c-300x300.png)
Lecture 10 February 13
... No White Dwarf Can have more than 1.4M~ Otherwise it will groan and collapse under its own weight. We’ll come back to this later. ...
... No White Dwarf Can have more than 1.4M~ Otherwise it will groan and collapse under its own weight. We’ll come back to this later. ...
Astronomy Worksheet
... In this lab you will determine the spectral type of a star by doing spectral analysis. In the process you will review how spectra are used to interpret various stellar parameters. The traditional spectra studied in a high school lab look like a series of colored strips. Researchgrade spectroscopes d ...
... In this lab you will determine the spectral type of a star by doing spectral analysis. In the process you will review how spectra are used to interpret various stellar parameters. The traditional spectra studied in a high school lab look like a series of colored strips. Researchgrade spectroscopes d ...
Herzsprung-Russell Diagram
... Only 3 of the 43 nearest stars is among the 20 brightest stars: Sirius, Alpha Centauri, Procyon. 13 out of 44 nearest stars are binaries total of 59 stars. 43 out of these 59 stars have less than 0.01 Ls. ...
... Only 3 of the 43 nearest stars is among the 20 brightest stars: Sirius, Alpha Centauri, Procyon. 13 out of 44 nearest stars are binaries total of 59 stars. 43 out of these 59 stars have less than 0.01 Ls. ...
The Life Cycle of Stars
... It is red because it is cooler than it was in the main sequence star stage and it is a giant because the outer shell has expanded outward. In the core of the red giant, helium fuses into carbon. All stars evolve the same way up to the red giant phase. The amount of mass a star has determines which l ...
... It is red because it is cooler than it was in the main sequence star stage and it is a giant because the outer shell has expanded outward. In the core of the red giant, helium fuses into carbon. All stars evolve the same way up to the red giant phase. The amount of mass a star has determines which l ...
Name: ____________________________ Date: _____________ Per. _________ Stars Study Guide (Ch. 21)
... 13. What is a graph that shows the relationship between absolute brightness and surface temperature of a star? __________________ ...
... 13. What is a graph that shows the relationship between absolute brightness and surface temperature of a star? __________________ ...
Quiz Questions
... C. chemical burning of carbon atoms B. nuclear fission D. heat from gravitational contraction 4. Why does hydrogen fusion only occur in the deep interiors of the Sun (and other stars)? A. because this is the only place in the Sun where there is sufficient hydrogen B. because only in the core is the ...
... C. chemical burning of carbon atoms B. nuclear fission D. heat from gravitational contraction 4. Why does hydrogen fusion only occur in the deep interiors of the Sun (and other stars)? A. because this is the only place in the Sun where there is sufficient hydrogen B. because only in the core is the ...
Starlight and What it Tells Us
... Radiation is Reflected from Some Other Source • The Sun Emits Black-Body Radiation, the Moon Does Not ...
... Radiation is Reflected from Some Other Source • The Sun Emits Black-Body Radiation, the Moon Does Not ...
The Galactic Super Star Cluster Westerlund 1
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
... times the mass of Orion. Therefore, we would have expected diffuse emission with L x = 3x10 35 erg s-1, which is five times more flux than we observe. We suggest that the IMF is nonstandard, as is often claimed for young, massive star clusters. ...
notes
... from our Sun (T = 5800 K) • We moved it to an M-type star (T = 3000 K) and placed it at the same distance that it currently is from our Sun • In each of these cases, where should we place the Earth to prevent these effects? ...
... from our Sun (T = 5800 K) • We moved it to an M-type star (T = 3000 K) and placed it at the same distance that it currently is from our Sun • In each of these cases, where should we place the Earth to prevent these effects? ...
Chapter 10. Stellar Spectra
... Some lines of some “metals” (for astronomers, the term metals is used for everything other than Hydrogen or Helium – no one ever said we were good chemists!), such as Sodium (Na) there are lines visible in the optical region of the spectrum that arise from the ground state of the neutral atom (NaI). ...
... Some lines of some “metals” (for astronomers, the term metals is used for everything other than Hydrogen or Helium – no one ever said we were good chemists!), such as Sodium (Na) there are lines visible in the optical region of the spectrum that arise from the ground state of the neutral atom (NaI). ...
KMS Universe Test Study Guide
... 6) Why does the sun have such a great apparent magnitude, when it has only an average absolute magnitude? The Sun is very close to us, so it appears to be brighter than it is compared to other stars in the Universe. 7) Why are red giant stars so bright, when they are among the coolest of stars? Beca ...
... 6) Why does the sun have such a great apparent magnitude, when it has only an average absolute magnitude? The Sun is very close to us, so it appears to be brighter than it is compared to other stars in the Universe. 7) Why are red giant stars so bright, when they are among the coolest of stars? Beca ...
An introduction to the HR diagram File
... • They are using up their hydrogen fuel tremendously quickly. So they are extremely short lived (c10 000 000 years) • These high mass stars finish their lives in massive supernova explosions • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so ...
... • They are using up their hydrogen fuel tremendously quickly. So they are extremely short lived (c10 000 000 years) • These high mass stars finish their lives in massive supernova explosions • At the bottom right the stars are cool. These low mass stars are very long lived as they use their fuel so ...
Planetary Configurations
... Chandrasekhar Limit: MWD < 1.4Mo, otherwise gravity overwhelms electron degeneracy pressure For normal stars, bigger M yields bigger R, but opposite for WDs Radius is fixed, and WD still glows, so it just continues to cool and fade (i.e., temperature drops over time) ...
... Chandrasekhar Limit: MWD < 1.4Mo, otherwise gravity overwhelms electron degeneracy pressure For normal stars, bigger M yields bigger R, but opposite for WDs Radius is fixed, and WD still glows, so it just continues to cool and fade (i.e., temperature drops over time) ...
Stars and Constellations
... • The object switches to become a “true star” and it is then able to make its own heat and light. • The life of the star then depends on its mass. ...
... • The object switches to become a “true star” and it is then able to make its own heat and light. • The life of the star then depends on its mass. ...
The Life Cycle of Stars
... It is red because it is cooler than it was in the main sequence star stage and it is a giant because the outer shell has expanded outward. In the core of the red giant, helium fuses into carbon. All stars evolve the same way up to the red giant phase. The amount of mass a star has determines which l ...
... It is red because it is cooler than it was in the main sequence star stage and it is a giant because the outer shell has expanded outward. In the core of the red giant, helium fuses into carbon. All stars evolve the same way up to the red giant phase. The amount of mass a star has determines which l ...
Name _________ Date _____________ Period ______ Skills
... d. their size. _____ 18. Stars are now classified by a. their elements. b. their temperature. c. their age. d. their size. _____ 19. Class O stars, the hottest stars, are a. yellow. b. orange. c. red. d. blue. 20. Early astronomers called the brightest stars in the sky ______________________ stars. ...
... d. their size. _____ 18. Stars are now classified by a. their elements. b. their temperature. c. their age. d. their size. _____ 19. Class O stars, the hottest stars, are a. yellow. b. orange. c. red. d. blue. 20. Early astronomers called the brightest stars in the sky ______________________ stars. ...
H-R Diagram Notes
... • Temperature ______________________ as you move to the Right on the X-axis • Absolute Magnitude ________________________ as you move up on the Y-axis. • NEGATIVE absolute magnitude values are ____________________ than POSITIVE absolute magnitude values A star… • Starts off in the lower right hand c ...
... • Temperature ______________________ as you move to the Right on the X-axis • Absolute Magnitude ________________________ as you move up on the Y-axis. • NEGATIVE absolute magnitude values are ____________________ than POSITIVE absolute magnitude values A star… • Starts off in the lower right hand c ...
Twinkle, Twinkle, Little Star
... The brightness of a star depends on both the size and temperature of the star. But, how bright it APPEARS to us depends on how far it is from Earth and how bright it truly is. ...
... The brightness of a star depends on both the size and temperature of the star. But, how bright it APPEARS to us depends on how far it is from Earth and how bright it truly is. ...
11.1 Stars - St John Brebeuf
... Stars form from the dust and gases found in a nebula, when enough gravity causes all the molecules to collapse in on themselves. If enough matter gathers, the gravity becomes so massive that hydrogen atoms join to form helium atoms, producing huge amounts of energy through the process of ...
... Stars form from the dust and gases found in a nebula, when enough gravity causes all the molecules to collapse in on themselves. If enough matter gathers, the gravity becomes so massive that hydrogen atoms join to form helium atoms, producing huge amounts of energy through the process of ...
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.