Problem Set 2
... ellipse’s semi-major axis. What is the distance d to the supernova? Finally, at its brightest, SN1987A had an apparent magnitude of mV ≈ 3 mag. What was its peak absolute magnitude? Given that the Sun has an absolute magnitude of MV = 4.78 mag in the V band, what was its peak luminosity (in solar u ...
... ellipse’s semi-major axis. What is the distance d to the supernova? Finally, at its brightest, SN1987A had an apparent magnitude of mV ≈ 3 mag. What was its peak absolute magnitude? Given that the Sun has an absolute magnitude of MV = 4.78 mag in the V band, what was its peak luminosity (in solar u ...
binary star
... Death of Massive Stars • In contrast to sunlike stars, stars that are over three times the sun’s mass have relatively short life spans, which end in a supernova event. • A supernova is an exploding massive star that increases in brightness many thousands of times. • The massive star’s interior con ...
... Death of Massive Stars • In contrast to sunlike stars, stars that are over three times the sun’s mass have relatively short life spans, which end in a supernova event. • A supernova is an exploding massive star that increases in brightness many thousands of times. • The massive star’s interior con ...
- National Optical Astronomy Observatory
... Figure 1: (X=color index (b-v), Y=Brightness (v)) According to the graph, the tip of the main sequence appears to lie around NGC 1496-1. This star’s color index is approximately 0.062, classifying it as a spectral type A star. Based on this observation, the age of the cluster is estimated to be no ...
... Figure 1: (X=color index (b-v), Y=Brightness (v)) According to the graph, the tip of the main sequence appears to lie around NGC 1496-1. This star’s color index is approximately 0.062, classifying it as a spectral type A star. Based on this observation, the age of the cluster is estimated to be no ...
Astronomical Ideas Fall 2012 Homework 4 Solutions 1. Two stars
... Convert the white dwarf radius into meters: 104 km = 107 m, and plug numbers into the above equation. 106 K: L ~ 7 * 1031 W. The Sunʼs luminosity is ~4 * 1026 , so this hot white dwarf is about 100,000 times the luminosity of the Sun. 104 K: L ~ 7 * 1024 W. The Sunʼs luminosity is ~4 * 1026 , so thi ...
... Convert the white dwarf radius into meters: 104 km = 107 m, and plug numbers into the above equation. 106 K: L ~ 7 * 1031 W. The Sunʼs luminosity is ~4 * 1026 , so this hot white dwarf is about 100,000 times the luminosity of the Sun. 104 K: L ~ 7 * 1024 W. The Sunʼs luminosity is ~4 * 1026 , so thi ...
Lectures 10 & 11 powerpoint (stellar formation) [movie below]
... The Source of Stellar Energy Stars produce energy by nuclear fusion of hydrogen into helium. Q: How does the sun fuse H to He? ...
... The Source of Stellar Energy Stars produce energy by nuclear fusion of hydrogen into helium. Q: How does the sun fuse H to He? ...
(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. ...
HR Diagram
... 6. Then select File>Load Plot>Select Cluster Data. Start with the intermediate age NGC 752. Double click to load graph. Under tools choose Zero Age Main Sequence. Adjust the V-Mv scroll bar to get the best fit between the ZAMS (green line) and the data. The older the cluster the fewer the stars left ...
... 6. Then select File>Load Plot>Select Cluster Data. Start with the intermediate age NGC 752. Double click to load graph. Under tools choose Zero Age Main Sequence. Adjust the V-Mv scroll bar to get the best fit between the ZAMS (green line) and the data. The older the cluster the fewer the stars left ...
Universe Now - Course Pages of Physics Department
... when the orbital period is known (as stated by Kepler’s III law). – Can be classified according to the distance between the components: • Detached binaries: the stars affect each other only by gravity, no mass transfer. Most binaries belong to this class. • Semidetached binaries: one star is stretch ...
... when the orbital period is known (as stated by Kepler’s III law). – Can be classified according to the distance between the components: • Detached binaries: the stars affect each other only by gravity, no mass transfer. Most binaries belong to this class. • Semidetached binaries: one star is stretch ...
Astr604-Ch1
... 1.2.3 Masses and radii of stars The mass of a star can be measured only by its gravitational effect. Under certain conditions, the mass of star that is member of a binary system can calculate based on spectral line shifts. The radii of a number of stars have been found directly from measurement of t ...
... 1.2.3 Masses and radii of stars The mass of a star can be measured only by its gravitational effect. Under certain conditions, the mass of star that is member of a binary system can calculate based on spectral line shifts. The radii of a number of stars have been found directly from measurement of t ...
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 ...
O star
... spectral type and the luminosity class of a star from its spectrum. This is extraordinarily valuable, as it means that, just from the spectrum of a star, one can plot it in on the H-R diagram. BUT: if you can plot a star on the H-R diagram, you know its absolute magnitude! And if you know its absolu ...
... spectral type and the luminosity class of a star from its spectrum. This is extraordinarily valuable, as it means that, just from the spectrum of a star, one can plot it in on the H-R diagram. BUT: if you can plot a star on the H-R diagram, you know its absolute magnitude! And if you know its absolu ...
Some Facts and Hypotheses regard
... large and variable ranging up to 500 miles a second. It has been conjectured, that in the case of Eta Argus, two large bodies may have passed very near eaoh other and thus produced great tidal disturbances, oausing immense eruptions corresponding to solar prominencies, only on a vastly larger scale. ...
... large and variable ranging up to 500 miles a second. It has been conjectured, that in the case of Eta Argus, two large bodies may have passed very near eaoh other and thus produced great tidal disturbances, oausing immense eruptions corresponding to solar prominencies, only on a vastly larger scale. ...
Astronomy and Space Science
... A: The ratio of brightness between two stars with magnitude m1 and m2 is 100(m2-m1)/5. One can easily check this formula with the definition. Now if a star of apparent magnitude m and distance d is moved to 10 pc from us and its new apparent magnitude is M, then the ratio of brightness is 100(M-m)/5 ...
... A: The ratio of brightness between two stars with magnitude m1 and m2 is 100(m2-m1)/5. One can easily check this formula with the definition. Now if a star of apparent magnitude m and distance d is moved to 10 pc from us and its new apparent magnitude is M, then the ratio of brightness is 100(M-m)/5 ...
Report Sheet
... 17. What is the minimum temperature a Protostar must achieve to begin hydrogen fusion? ____________F 18. Define hydrogen fusion- ____________________________________________________________________ 19. If our Sun is blowing up like a bomb, why does it not just blast itself into space? _____________ ...
... 17. What is the minimum temperature a Protostar must achieve to begin hydrogen fusion? ____________F 18. Define hydrogen fusion- ____________________________________________________________________ 19. If our Sun is blowing up like a bomb, why does it not just blast itself into space? _____________ ...
Formation of Stars - mcp
... There are 7 different classes of stars 1. O – Hottest stars (30 – 60,000 K), typically blue in color and very large 2. B – Blue – white in color 3. A – White in color 4. F – Yellow-white color 5. G – Yellow in color, our sun is a G-class star (5-6000 K) 6. K – Yellow - Orange 7. M – Coolest stars (> ...
... There are 7 different classes of stars 1. O – Hottest stars (30 – 60,000 K), typically blue in color and very large 2. B – Blue – white in color 3. A – White in color 4. F – Yellow-white color 5. G – Yellow in color, our sun is a G-class star (5-6000 K) 6. K – Yellow - Orange 7. M – Coolest stars (> ...
Milky Way structure
... associated tidal stream of material in relation to our Milky Way Galaxy. The Canis Major dwarf and other satellite galaxies are slowly being gravitationally ripped apart as they travel around and through our Galaxy. ...
... associated tidal stream of material in relation to our Milky Way Galaxy. The Canis Major dwarf and other satellite galaxies are slowly being gravitationally ripped apart as they travel around and through our Galaxy. ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.