Physics 127 Descriptive Astronomy Homework #20 Key
... 14-3. How did Edwin Hubble prove that the Andromeda “Nebula” is not a nebula within our Milky Way Galaxy? Hubble was able to detect Cepheid variable stars within that “Nebula.” Then by observing their light curves and using the known period- luminosity relation for Cepheids, he obtained and compared ...
... 14-3. How did Edwin Hubble prove that the Andromeda “Nebula” is not a nebula within our Milky Way Galaxy? Hubble was able to detect Cepheid variable stars within that “Nebula.” Then by observing their light curves and using the known period- luminosity relation for Cepheids, he obtained and compared ...
ASTR3007/4007/6007, Tutorial 4: Deuterium Burning in Protostars
... While the star is burning deuterium, it essentially ceases contracting, because deuterium burning provides energy to counter the loss of radiation to space, and keep the star in equilibrium. Contraction only resumes once most of the deuterium has been used up. Exercise 6. The mass of a deuterium nuc ...
... While the star is burning deuterium, it essentially ceases contracting, because deuterium burning provides energy to counter the loss of radiation to space, and keep the star in equilibrium. Contraction only resumes once most of the deuterium has been used up. Exercise 6. The mass of a deuterium nuc ...
2. Stellar Physics
... fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant fusion, gravitational potential energy is radiated as the radius of the forming star contracts. Protostellar or pre ...
... fusion reactions in the stellar interior Other energy sources are dominant during star formation and stellar death: • Star formation - before the interior is hot enough for significant fusion, gravitational potential energy is radiated as the radius of the forming star contracts. Protostellar or pre ...
Packet 3
... 10. What are the 2 types of motion of stars? A) _______________________ B) _____________________ 11a. How’s the actual motion of star’s measured? 11b. What causes the apparent motion of stars? 12. How come when you go outside on an October night you see different stars than on an April night? 13. Th ...
... 10. What are the 2 types of motion of stars? A) _______________________ B) _____________________ 11a. How’s the actual motion of star’s measured? 11b. What causes the apparent motion of stars? 12. How come when you go outside on an October night you see different stars than on an April night? 13. Th ...
Characteristics of Main Sequence Stars
... value of ∇rad , and convective instability. In this region, convective energy transport is extremely efficient, and ∇ ≈ ∇ad . • Because of the extreme temperature sensitivity of CNO burning, nuclear reactions in high mass stars are generally confined to a very small region, much smaller than the siz ...
... value of ∇rad , and convective instability. In this region, convective energy transport is extremely efficient, and ∇ ≈ ∇ad . • Because of the extreme temperature sensitivity of CNO burning, nuclear reactions in high mass stars are generally confined to a very small region, much smaller than the siz ...
The H-R Diagram
... The Main Sequence: The main sequence goes from the upper left to the lower right. The stars at the upper left are hotter, larger, and more massive than the Sun. The Sun is near with an absolute magnitude of MV=+5 and a spectral type G2. Like all m.s. stars it is of luminosity class V. Those stars to ...
... The Main Sequence: The main sequence goes from the upper left to the lower right. The stars at the upper left are hotter, larger, and more massive than the Sun. The Sun is near with an absolute magnitude of MV=+5 and a spectral type G2. Like all m.s. stars it is of luminosity class V. Those stars to ...
The Milky Way - Houston Community College System
... measurements of distant celestial objects is especially difficult. To discover the properties of stars, astronomers have used their telescopes and spectrographs in clever ways to learn the secrets hidden in starlight. The result is a family portrait of the stars. In this chapter you will find answer ...
... measurements of distant celestial objects is especially difficult. To discover the properties of stars, astronomers have used their telescopes and spectrographs in clever ways to learn the secrets hidden in starlight. The result is a family portrait of the stars. In this chapter you will find answer ...
Star Track 2 - The Search for a Supermassive Black... Early radio astronomers detected an immensely
... 7. Why do astronomers think this makes SgrA* a black hole, and not some other kind of object? This is about half the mass of the sun per cubic AU – actually much less than the Sun's density. So in principle SgrA* "could" be some other object. However, this density is just a minimum, and we know of m ...
... 7. Why do astronomers think this makes SgrA* a black hole, and not some other kind of object? This is about half the mass of the sun per cubic AU – actually much less than the Sun's density. So in principle SgrA* "could" be some other object. However, this density is just a minimum, and we know of m ...
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. ...
S1-4-03 - Celestial Navigation
... 6. How high is Polaris in the sky? (It depends on where you are.) 7. How many degrees does the earth rotate in one day? (360o) 8. Draw A) the Earth and label the northern and southern hemisphere, the equator and the North Star. B) A star trails diagram. ...
... 6. How high is Polaris in the sky? (It depends on where you are.) 7. How many degrees does the earth rotate in one day? (360o) 8. Draw A) the Earth and label the northern and southern hemisphere, the equator and the North Star. B) A star trails diagram. ...
Slide 1
... system. Both masses equal => center of mass is in the middle, rA = rB. The more unequal the masses are, the more it shifts toward the more massive star. ...
... system. Both masses equal => center of mass is in the middle, rA = rB. The more unequal the masses are, the more it shifts toward the more massive star. ...
Astronomy Library wk 6.cwk (WP)
... We expect that stars of similar temperatures will have similar spectral features. Stars have been classified into 7 major categories based on the relative strength of their spectral lines. ...
... We expect that stars of similar temperatures will have similar spectral features. Stars have been classified into 7 major categories based on the relative strength of their spectral lines. ...
Stars…Giants, Supergiants, Dwarfs….
... atomic energy levels, instead of being crisp and unique, get “fuzzed out”. “Fuzzed out” is technical terminology for a change in the energy which depends on how close the neighbors are, how many of them there are, what direction they are,…… ...
... atomic energy levels, instead of being crisp and unique, get “fuzzed out”. “Fuzzed out” is technical terminology for a change in the energy which depends on how close the neighbors are, how many of them there are, what direction they are,…… ...
12-1 MAIN-SEQUENCE STARS
... system, and mass can flow from one star to the other through the inner Lagrangian point. Close binary stars evolve in complex ways because they can transfer mass from one star to the other. This explains why some binary systems contain a main-sequence star more massive than its giant companion—the A ...
... system, and mass can flow from one star to the other through the inner Lagrangian point. Close binary stars evolve in complex ways because they can transfer mass from one star to the other. This explains why some binary systems contain a main-sequence star more massive than its giant companion—the A ...
Lecture 1
... position of Star A as seen in July and label it “Star A July”. Describe how Star A would appear to move among the distant stars as Earth orbits the Sun counterclockwise from January of one year, through July, to January of the following year. Consider two stars (C and D) that both exhibit parallax. ...
... position of Star A as seen in July and label it “Star A July”. Describe how Star A would appear to move among the distant stars as Earth orbits the Sun counterclockwise from January of one year, through July, to January of the following year. Consider two stars (C and D) that both exhibit parallax. ...
ASTR100 Class 01 - University of Maryland Department of
... the core temperature becomes hot enough for fusion. Star-like objects not massive enough to start fusion are brown dwarfs. ...
... the core temperature becomes hot enough for fusion. Star-like objects not massive enough to start fusion are brown dwarfs. ...
Day-26
... It is very difficult to directly see a faint planet in the bright glow of its star. A few dozen planets have been identified this way so far. ...
... It is very difficult to directly see a faint planet in the bright glow of its star. A few dozen planets have been identified this way so far. ...
The quick brown fox jumps over the lazy dog
... On "the first day of the New Year" sometime "early in the twentieth century", 3 different observatories simultaneously announced having noticed unexplainable perturbations in the motion of planet Neptune. It will be soon be found that this is due to a foreign star - a "strange wanderer ... a great ...
... On "the first day of the New Year" sometime "early in the twentieth century", 3 different observatories simultaneously announced having noticed unexplainable perturbations in the motion of planet Neptune. It will be soon be found that this is due to a foreign star - a "strange wanderer ... a great ...
How big are stars? How do we know?
... b) relatively cool giant stars that are relatively close to the Sun. c) relatively cool main-sequence stars that are relatively far from the Sun. d) relatively cool main-sequence stars that are relatively close to the Sun. e) giant stars and relatively hot main sequence stars. ...
... b) relatively cool giant stars that are relatively close to the Sun. c) relatively cool main-sequence stars that are relatively far from the Sun. d) relatively cool main-sequence stars that are relatively close to the Sun. e) giant stars and relatively hot main sequence stars. ...
Astronomy (C) - North Carolina Science Olympiad
... • Low-mass stars: slowly burn all fuel • Medium mass stars: burn H, become red giant, separate into planetary nebula & white dwarf • Massive stars: burn H all the way to Fe, explode in supernova, leave behind remnant and either neutron star or black hole ...
... • Low-mass stars: slowly burn all fuel • Medium mass stars: burn H, become red giant, separate into planetary nebula & white dwarf • Massive stars: burn H all the way to Fe, explode in supernova, leave behind remnant and either neutron star or black hole ...
The Evening Sky Map
... Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to each other in the sky; either linked by gravity so that they orbit each other (binary star) or lying at different distances from Earth (optical double). Apparent separation of stars is given in ...
... Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to each other in the sky; either linked by gravity so that they orbit each other (binary star) or lying at different distances from Earth (optical double). Apparent separation of stars is given in ...
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 ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.