NASAexplores 9-12 Lesson: Classified Stars - Science
... a chart according to their color and brightness. The most amazing thing is that they did not even know one other, and did their experiments completely independent of each other. Therefore, this chart is called the Hertzsprung-Russell (HR) diagram. The diagram shows you how the sizes and colors of st ...
... a chart according to their color and brightness. The most amazing thing is that they did not even know one other, and did their experiments completely independent of each other. Therefore, this chart is called the Hertzsprung-Russell (HR) diagram. The diagram shows you how the sizes and colors of st ...
OBAFGKM(LT) extra credit due today. Mid
... Life and Death as a High-Mass star (>8× the sun) At first, evolution similar to low mass star: core of hydrogen, fusing to helium Red giant phase with H fusing in a shell. Core of helium fusing into Carbon. ...
... Life and Death as a High-Mass star (>8× the sun) At first, evolution similar to low mass star: core of hydrogen, fusing to helium Red giant phase with H fusing in a shell. Core of helium fusing into Carbon. ...
Formation of the Solar System
... Our solar system and the stars visible in our sky comprise an extremely small portion of our galaxy. Our galactic centre cannot be seen in optical light due to heavy obscuration from foreground stars and interstellar matter; we can only see about a tenth of the way toward the centre. In a dark rural ...
... Our solar system and the stars visible in our sky comprise an extremely small portion of our galaxy. Our galactic centre cannot be seen in optical light due to heavy obscuration from foreground stars and interstellar matter; we can only see about a tenth of the way toward the centre. In a dark rural ...
Slides from Lecture04
... through telescopes but were not bright enough to be seen by Greek astronomers). • The Sun can also be put on this “magnitude” system. ...
... through telescopes but were not bright enough to be seen by Greek astronomers). • The Sun can also be put on this “magnitude” system. ...
Our Solar System
... as the sun, still found in the sun’s atmosphere. Rocky planet material formed from clumping together of dust grains in the protostellar cloud. ...
... as the sun, still found in the sun’s atmosphere. Rocky planet material formed from clumping together of dust grains in the protostellar cloud. ...
Astronomy
... The star is now in the “prime of its life”; it is in equilibrium. Over time; temp, luminosity, color change. Our sun is in the main sequence phase It will live for about 10 billion years Our sun is now about 4.6 billion years old – Links: ...
... The star is now in the “prime of its life”; it is in equilibrium. Over time; temp, luminosity, color change. Our sun is in the main sequence phase It will live for about 10 billion years Our sun is now about 4.6 billion years old – Links: ...
part2
... was where most of the silicates in the solar nebula were located. b) silicates could only condense close to the Sun. c) it was too hot for the large protoplanets forming here to capture any significant amounts of hydrogen or helium. d) there was no hydrogen or helium in the inner solar nebula where ...
... was where most of the silicates in the solar nebula were located. b) silicates could only condense close to the Sun. c) it was too hot for the large protoplanets forming here to capture any significant amounts of hydrogen or helium. d) there was no hydrogen or helium in the inner solar nebula where ...
Anomalous diffusion in generalised Ornstein
... 2. The transit of a planet across a star can be detected as a slight reduction in luminosity of the star. 3. Gravitational lensing effects from planets have been observed. With these techniques it is easier to detect large planets with small rotational periods. ...
... 2. The transit of a planet across a star can be detected as a slight reduction in luminosity of the star. 3. Gravitational lensing effects from planets have been observed. With these techniques it is easier to detect large planets with small rotational periods. ...
1 Ay 124 Winter 2016 – HOMEWORK #3
... Due Friday, Feb 5, 2016 by 5pm, in Denise’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about t ...
... Due Friday, Feb 5, 2016 by 5pm, in Denise’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about t ...
Astrophysics Outline—Option E
... Define apparent brightness and state how it is measured. Wien’s law and the Stefan-Boltzmann law E.2.5 Apply the Stefan–Boltzmann law to compare the luminosities of different stars. E.2.6 State Wien’s (displacement) law and apply it to explain the connection between the colour and temperature of sta ...
... Define apparent brightness and state how it is measured. Wien’s law and the Stefan-Boltzmann law E.2.5 Apply the Stefan–Boltzmann law to compare the luminosities of different stars. E.2.6 State Wien’s (displacement) law and apply it to explain the connection between the colour and temperature of sta ...
Our Universe
... – There no center of the universe because there is no edge of the universe – In a finite universe, space is curved so that if you could travel billions of light years in a straight line you would finish back where you started. – It is also possible that our universe is infinite. In both examples, gr ...
... – There no center of the universe because there is no edge of the universe – In a finite universe, space is curved so that if you could travel billions of light years in a straight line you would finish back where you started. – It is also possible that our universe is infinite. In both examples, gr ...
Handout from Allaire Star Party
... We inhabit a speck of dust in a huge cosmos. To get a sense of scale for our universe, imagine that the Sun is the size of a beach ball. On this scale, the entire Earth would be about the size of a pea. If you placed the beach ball on one goal line of a football field, the Earth would be at about th ...
... We inhabit a speck of dust in a huge cosmos. To get a sense of scale for our universe, imagine that the Sun is the size of a beach ball. On this scale, the entire Earth would be about the size of a pea. If you placed the beach ball on one goal line of a football field, the Earth would be at about th ...
1 Ay 124 Winter 2014 – HOMEWORK #3
... Due Friday, Feb 14, 2014 by 5pm, in Steidel’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about ...
... Due Friday, Feb 14, 2014 by 5pm, in Steidel’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about ...
Star Life Cycle – Web Activity
... 8. What type of system is a brown dwarf usually found in? 9. Click on “protostar” and find out how long it takes for a protostar to turn into a star. Stars 10. Stars spend the majority of their lives fusing ____________ into ______________, and then fusing Helium into ________________. 11. Click on ...
... 8. What type of system is a brown dwarf usually found in? 9. Click on “protostar” and find out how long it takes for a protostar to turn into a star. Stars 10. Stars spend the majority of their lives fusing ____________ into ______________, and then fusing Helium into ________________. 11. Click on ...
Diapositiva 1
... Side View of the Milky Way The “halo” is really the “stellar halo” – turns out there’s actually a larger halo we can’t even see! ...
... Side View of the Milky Way The “halo” is really the “stellar halo” – turns out there’s actually a larger halo we can’t even see! ...
Topic Outline - Physics Rocks!
... E.6.1 Describe the distribution of galaxies in the universe E.6.2 Explain the red-shift of light from distant galaxies E.6.3 Solve problems involving red-shift and the recession speed of galaxies ...
... E.6.1 Describe the distribution of galaxies in the universe E.6.2 Explain the red-shift of light from distant galaxies E.6.3 Solve problems involving red-shift and the recession speed of galaxies ...
Measuring Distance with Spectroscopic Parallax
... 2. There are 9.46!1015 meters in one light-year. Convert your distances to lightyears by dividing the distance in meters by this number. 3. Recall that our Milky Way galaxy is 100,000 light-years across. For each of your stars, use the space below to explain whether it is most likely inside our gala ...
... 2. There are 9.46!1015 meters in one light-year. Convert your distances to lightyears by dividing the distance in meters by this number. 3. Recall that our Milky Way galaxy is 100,000 light-years across. For each of your stars, use the space below to explain whether it is most likely inside our gala ...
Lecture 9/10 Stellar evolution Ulf Torkelsson 1 Main sequence stars
... There is a gradual increase in the helium abundance during the main-sequence phase. The increase in molecular weight results in that the core is contracting and heating up in order to provide a sufficient pressure to balance the gravity. As a consequence of this the surface layers are gradually expa ...
... There is a gradual increase in the helium abundance during the main-sequence phase. The increase in molecular weight results in that the core is contracting and heating up in order to provide a sufficient pressure to balance the gravity. As a consequence of this the surface layers are gradually expa ...
*Studying Complex Star-Forming Fields: Rosette Nebula and Monoceros Loop by Chris Hathaway and Anthony Kuchera
... located near one end of a giant molecular cloud (Rosette Molecular Cloud)—a place of ongoing star formation. The Monoceros Loop (a circular optical nebulosity /in the vicinity of the Rosette Nebula) is thought to be a supernova remnant (the final product of the evolution of a very massive star). Ros ...
... located near one end of a giant molecular cloud (Rosette Molecular Cloud)—a place of ongoing star formation. The Monoceros Loop (a circular optical nebulosity /in the vicinity of the Rosette Nebula) is thought to be a supernova remnant (the final product of the evolution of a very massive star). Ros ...