Electromagnetic radiation
... of concentration substance. To use such description of spectral line, which straight proportional the concentration of a substance. ...
... of concentration substance. To use such description of spectral line, which straight proportional the concentration of a substance. ...
Linking Asteroids and Meteorites through Reflectance
... What is a galaxy? • Is a massive, gravitationally bound system consisting of stars, gas and dust, and dark matter. Galaxies can contain between ten million and a trillion stars • Dark matter is matter that does not emit or reflect enough radiation to be seen, but whose gravitation effects can be fe ...
... What is a galaxy? • Is a massive, gravitationally bound system consisting of stars, gas and dust, and dark matter. Galaxies can contain between ten million and a trillion stars • Dark matter is matter that does not emit or reflect enough radiation to be seen, but whose gravitation effects can be fe ...
Section 25.1 Properties of Stars
... Binary Stars and Stellar Mass A binary star is one of two stars revolving around a common center of mass under their mutual gravitational attraction. Binary stars are used to determine the star property most difficult to calculate—its mass. Common Center of Mass ...
... Binary Stars and Stellar Mass A binary star is one of two stars revolving around a common center of mass under their mutual gravitational attraction. Binary stars are used to determine the star property most difficult to calculate—its mass. Common Center of Mass ...
4th Six Weeks Review key
... Characteristics of the Sun 31. Fusion occurs when ___hydrogen_ atoms fuse to form __helium____ with the resulting change in mass releases energy. 32. What type of star is our sun? (circle one) MASSIVE or AVERAGE 33. Our sun is a _____main sequence star and is the color ___yellow___. 34. Where is ou ...
... Characteristics of the Sun 31. Fusion occurs when ___hydrogen_ atoms fuse to form __helium____ with the resulting change in mass releases energy. 32. What type of star is our sun? (circle one) MASSIVE or AVERAGE 33. Our sun is a _____main sequence star and is the color ___yellow___. 34. Where is ou ...
Which has a hotter temperature, a red star or a blue star? How do
... temperature. Are yellow socks as hot as the sun? ...
... temperature. Are yellow socks as hot as the sun? ...
THE LIBERAL ARTS AND SCIENCES The liberal arts and sciences
... billions of civilisations out there – or we may be the only one. At the moment, there is no scientific evidence one way or the other. Another very important issue is the possibility of a collision with an asteroid or other space object – as seen in Russia recently. Currently in the news is the come ...
... billions of civilisations out there – or we may be the only one. At the moment, there is no scientific evidence one way or the other. Another very important issue is the possibility of a collision with an asteroid or other space object – as seen in Russia recently. Currently in the news is the come ...
The Earth and BeyondGCSE
... Light from other galaxies has a longer _________ than expected. This shows that these galaxies are moving ____ from us very quickly. This effect is seen to a greater extent in galaxies that are _______ away from us. This indicates that the further away the galaxy is, the ______ it is moving. This ev ...
... Light from other galaxies has a longer _________ than expected. This shows that these galaxies are moving ____ from us very quickly. This effect is seen to a greater extent in galaxies that are _______ away from us. This indicates that the further away the galaxy is, the ______ it is moving. This ev ...
The HR Diagram and Stars Worksheet
... a. Page 622 – Add the Spectral Class below the temperatures. b. Page 626 – Use colored pencils to add and label the band that represents Main Sequence stars. c. Page 626 – Use colored pencils to label the following areas: Blue Giants, Red Super Giants, Red Giants, Red Dwarfs, White Dwarfs d. Page 62 ...
... a. Page 622 – Add the Spectral Class below the temperatures. b. Page 626 – Use colored pencils to add and label the band that represents Main Sequence stars. c. Page 626 – Use colored pencils to label the following areas: Blue Giants, Red Super Giants, Red Giants, Red Dwarfs, White Dwarfs d. Page 62 ...
STUDY GUIDE FOR CHAPTER 1
... 1. Which direction does temperature increase in? Luminosity? 2. What can we plot instead of temperature? Instead of luminosity? B. Different types of stars are in different regions. You should know what types they are and what regions of the H-R diagram they are found in. 1. Where are the supergiant ...
... 1. Which direction does temperature increase in? Luminosity? 2. What can we plot instead of temperature? Instead of luminosity? B. Different types of stars are in different regions. You should know what types they are and what regions of the H-R diagram they are found in. 1. Where are the supergiant ...
lecture 27 nuclar fusion in stars
... Neutron stars are incredibly dense – a neutron star with the mass of the sun would be about 10 km in diameter! The star’s rotation also speeds up as it collapses. Neutron stars typically rotate between 1 and 1000 times per second. ...
... Neutron stars are incredibly dense – a neutron star with the mass of the sun would be about 10 km in diameter! The star’s rotation also speeds up as it collapses. Neutron stars typically rotate between 1 and 1000 times per second. ...
Quasars and Active Galaxies
... • “Steady State”: As galaxies move apart from each other, new atoms are spontaneously created in empty space. These atoms coalesce to form new galaxies. The average density of the universe doesn’t change over time. There was no hot early universe. Quasars were the first evidence that the universe wa ...
... • “Steady State”: As galaxies move apart from each other, new atoms are spontaneously created in empty space. These atoms coalesce to form new galaxies. The average density of the universe doesn’t change over time. There was no hot early universe. Quasars were the first evidence that the universe wa ...
Astroparticle physics 1. stellar astrophysics and solar neutrinos
... Astrophysics oriented course. Astrophysical information. Stellar physics (solar neutrinos). Interstellar medium (cosmic-rays). Supernovae and degenerate stars (cosmic-rays, neutrinos). • Beyond our galaxy (high energy cosmicrays, (relic neutrinos), dark matter). ...
... Astrophysics oriented course. Astrophysical information. Stellar physics (solar neutrinos). Interstellar medium (cosmic-rays). Supernovae and degenerate stars (cosmic-rays, neutrinos). • Beyond our galaxy (high energy cosmicrays, (relic neutrinos), dark matter). ...
4.5.5. Black Holes
... solution, which is the analogue of the Schwarzschild solution for the non-rotating case. A black hole by itself is obviously difficult to detect. However, if large amounts of matter, such as another star or nabulae, are present nearby, they can be drawn to it. The extreme acceleration experienced by ...
... solution, which is the analogue of the Schwarzschild solution for the non-rotating case. A black hole by itself is obviously difficult to detect. However, if large amounts of matter, such as another star or nabulae, are present nearby, they can be drawn to it. The extreme acceleration experienced by ...
declarative interrogative imperative
... Astronomers can determine the age of a star by observing it closely. ...
... Astronomers can determine the age of a star by observing it closely. ...
Lifetimes of stars
... • The Sun (and all stars) will eventually run out of fuel (hydrogen in regions where it is hot enough for fusion). • If all the hydrogen in the Sun could fuse to helium, the Sun’s lifetime would be 100 billion years. • But, by the time about 10% of the Sun’s H has been converted into He the solar st ...
... • The Sun (and all stars) will eventually run out of fuel (hydrogen in regions where it is hot enough for fusion). • If all the hydrogen in the Sun could fuse to helium, the Sun’s lifetime would be 100 billion years. • But, by the time about 10% of the Sun’s H has been converted into He the solar st ...
PowerPoint Presentation - Planetary Configurations
... How does this energy propagate through space? And how does that relate to the apparent brightness of a source? “Flux” describes how light spreads out in space: with L=luminosity (or power), and d = distance, flux is Watts/square meter = J/s/m2 ...
... How does this energy propagate through space? And how does that relate to the apparent brightness of a source? “Flux” describes how light spreads out in space: with L=luminosity (or power), and d = distance, flux is Watts/square meter = J/s/m2 ...
1 The Milky Way
... At 21cm radio wavelength, we see emission from cold hydrogen gas. This is the raw material for making new stars. At somewhat higher radio frequency, we see radiation from many different molecules. These molecules exist in the the dense inner parts of gas clouds, and indicate where the next stars are ...
... At 21cm radio wavelength, we see emission from cold hydrogen gas. This is the raw material for making new stars. At somewhat higher radio frequency, we see radiation from many different molecules. These molecules exist in the the dense inner parts of gas clouds, and indicate where the next stars are ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.