Characterizing Stars - Department of Physics and Astronomy
... By carefully examining a star’s spectral lines, astronomers can determine whether that star is a main-sequence star, giant, supergiant, or white dwarf ...
... By carefully examining a star’s spectral lines, astronomers can determine whether that star is a main-sequence star, giant, supergiant, or white dwarf ...
Hubble`s Law is the relation between the recession velocity of a
... may explain why stars form there. The fact that we see star formation in spiral arms is evidence for the density wave theory, not the other way around. Similarly, the fact that we see star formation implies that elliptical galaxies were once more efficient then spirals, not the other way around. Als ...
... may explain why stars form there. The fact that we see star formation in spiral arms is evidence for the density wave theory, not the other way around. Similarly, the fact that we see star formation implies that elliptical galaxies were once more efficient then spirals, not the other way around. Als ...
File
... •A star is a huge ball of hot glowing gases, called plasma. •Stars twinkle because the light is distorted by Earth’s atmosphere. •All stars have one thing in common, the way they produce energy. •The energy comes from nuclear reactions that change hydrogen into helium. It is as if millions of atomi ...
... •A star is a huge ball of hot glowing gases, called plasma. •Stars twinkle because the light is distorted by Earth’s atmosphere. •All stars have one thing in common, the way they produce energy. •The energy comes from nuclear reactions that change hydrogen into helium. It is as if millions of atomi ...
Today`s Powerpoint
... Some protostars not massive (< 0.08 MSun) enough to begin fusion. These are Brown Dwarfs or failed stars. Very difficult to detect because so faint. First seen in 1994 with Palomar 200”. How many are there? ...
... Some protostars not massive (< 0.08 MSun) enough to begin fusion. These are Brown Dwarfs or failed stars. Very difficult to detect because so faint. First seen in 1994 with Palomar 200”. How many are there? ...
The Life Cycle of Stars
... Nebula and other nebulae (stars in formation) on this page. Continue by reading up on Main Sequence Stars and find out how our sun compares in mass to other stars like Sirius, and Proxima Centauri. Based on its mass, will our sun be around for a while? Approximately how long before our sun consumes ...
... Nebula and other nebulae (stars in formation) on this page. Continue by reading up on Main Sequence Stars and find out how our sun compares in mass to other stars like Sirius, and Proxima Centauri. Based on its mass, will our sun be around for a while? Approximately how long before our sun consumes ...
Expansion of the Universe
... RELATE TO THE UNIVERSE EXPANDING? Stars and galaxies are not getting bigger; rather, the space between all objects is expanding with time The expansion of the universe was discovered in 1929, by American astronomer Edwin Hubble ...
... RELATE TO THE UNIVERSE EXPANDING? Stars and galaxies are not getting bigger; rather, the space between all objects is expanding with time The expansion of the universe was discovered in 1929, by American astronomer Edwin Hubble ...
Stars: Other Suns
... • Apply Kepler’s 3rd law to get sum of masses from orbital period, separation (need distance!) ...
... • Apply Kepler’s 3rd law to get sum of masses from orbital period, separation (need distance!) ...
The Sun Compared to Other Stars
... The Sun Compared to Other Stars • Hertzsprung-Russell (HR) Diagram: A graph plot indicating individual stars as points, with stellar luminosity on the vertical axis & surface temperature (spectral type) on the horizontal axis • We can use spectroscopy to determine the spectral type & luminosity of a ...
... The Sun Compared to Other Stars • Hertzsprung-Russell (HR) Diagram: A graph plot indicating individual stars as points, with stellar luminosity on the vertical axis & surface temperature (spectral type) on the horizontal axis • We can use spectroscopy to determine the spectral type & luminosity of a ...
The life of a Star (pages 468-471)
... 4. What is a supernova? During this stage, what happens to the core of the star? When our Sun eventually swells into a red giant star, its outer layers will grow to be about 100 times its present size swallowing up Mercury, Venus, Earth and maybe even Mars 5. What is a neutron star? 6. What is a p ...
... 4. What is a supernova? During this stage, what happens to the core of the star? When our Sun eventually swells into a red giant star, its outer layers will grow to be about 100 times its present size swallowing up Mercury, Venus, Earth and maybe even Mars 5. What is a neutron star? 6. What is a p ...
Death of Stars
... The PROTON-PROTON reaction and the CNO cycle both involve fusion of four Hydrogen nuclei to form a He nucleus and conversion of mass to energy The energy appears as K.E of the particles formed, high energy gamma rays and neutrinos The temperature of the star’s core determines which process will domi ...
... The PROTON-PROTON reaction and the CNO cycle both involve fusion of four Hydrogen nuclei to form a He nucleus and conversion of mass to energy The energy appears as K.E of the particles formed, high energy gamma rays and neutrinos The temperature of the star’s core determines which process will domi ...
Measuring the Properties of Stars
... being radiated by the surface of a particular star. Astronomers call this power Luminosity, and it has dependancy on two properties of a star; it’s surface size (4R2) and its surface temperature (T). These are direct relationships. An increase in either of the properties, results in an increase in ...
... being radiated by the surface of a particular star. Astronomers call this power Luminosity, and it has dependancy on two properties of a star; it’s surface size (4R2) and its surface temperature (T). These are direct relationships. An increase in either of the properties, results in an increase in ...
Stellar Physics Lecture 1
... The H-R Diagram – Other regions to note are stars of high luminosity but low temperature (indicating they are large – hence the term red giant) and stars of high temperature but low luminosity (indicating small diameters, hence white dwarf ) – As we shall see, the H-R diagram is extremely useful in ...
... The H-R Diagram – Other regions to note are stars of high luminosity but low temperature (indicating they are large – hence the term red giant) and stars of high temperature but low luminosity (indicating small diameters, hence white dwarf ) – As we shall see, the H-R diagram is extremely useful in ...
Note
... • You want to detect the faint star of an unresolved binary system comprising a B5V star and an M0V companion. What wavelength regime would you choose to try to detect the M0V star? What is the ratio of the flux from the B star to the flux from the M star at that wavelength? • You want to detect the ...
... • You want to detect the faint star of an unresolved binary system comprising a B5V star and an M0V companion. What wavelength regime would you choose to try to detect the M0V star? What is the ratio of the flux from the B star to the flux from the M star at that wavelength? • You want to detect the ...
PHYS 175 (2014) Final Examination Name: ___SOLUTION_____
... Massive objects warp spacetime. If a massive object is aligned between an observer and a light source, some rays of light from the source, which would not normally be directed toward the observer, can be deflected toward the observer. The effect may ma ...
... Massive objects warp spacetime. If a massive object is aligned between an observer and a light source, some rays of light from the source, which would not normally be directed toward the observer, can be deflected toward the observer. The effect may ma ...
Stars and the Main Sequence
... Temperature,Luminosity, Mass relation during core H-burning: It turns out that as a function of mass there is a rather unique relationship between • surface temperature (can be measured from contineous spectrum) • luminosity (can be measured if distance is known) ...
... Temperature,Luminosity, Mass relation during core H-burning: It turns out that as a function of mass there is a rather unique relationship between • surface temperature (can be measured from contineous spectrum) • luminosity (can be measured if distance is known) ...
Astronomy practice questions for 3-6 test
... 4. Is the Andromeda galaxy red or blue shifted? __________________________________________________________ 5. According to Hubble’s law, which galaxy or planet is moving fastest away from the nearby star? __________________________________________________________ 6. Which galaxy or planet is moving ...
... 4. Is the Andromeda galaxy red or blue shifted? __________________________________________________________ 5. According to Hubble’s law, which galaxy or planet is moving fastest away from the nearby star? __________________________________________________________ 6. Which galaxy or planet is moving ...
Stars, Galaxies and the Universe FORM A
... 19. Why can’t an astronomer observe most of the infrared spectrum from the ground? (a) the ozone and oxygen in the Earth’s atmosphere absorb infrared radiation (b) water vapor in the Earth’s atmosphere absorbs infrared radiation (c) it is cheaper to put a telescope in space rather than on Earth (d) ...
... 19. Why can’t an astronomer observe most of the infrared spectrum from the ground? (a) the ozone and oxygen in the Earth’s atmosphere absorb infrared radiation (b) water vapor in the Earth’s atmosphere absorbs infrared radiation (c) it is cheaper to put a telescope in space rather than on Earth (d) ...
Chapter 16 - "The Universe"
... – Each magnitude is approximately 2.51 times fainter than the next higher magnitude number. – The absolute magnitude of a stars brightness is the brightness it would have if it were measured at 10 ...
... – Each magnitude is approximately 2.51 times fainter than the next higher magnitude number. – The absolute magnitude of a stars brightness is the brightness it would have if it were measured at 10 ...
7a Properties of Stars.pptx
... • Astronomical unit (AU) – 1 AU is the distance between the Sun and Earth • Our closest star (other than the sun) is 4.3 light-‐ years away. ...
... • Astronomical unit (AU) – 1 AU is the distance between the Sun and Earth • Our closest star (other than the sun) is 4.3 light-‐ years away. ...
1. Neutron stars 2. Black holes
... Type 1 supernovae and white dwarfs When an accreting white dwarf exceeds a maximum value of 1.4 solar masses (Chandresekhar mass), electrons inside cannot provide the pressure needed to support the star. Star begins to collapse, temperature rises to the point where carbon fusion takes place. Fu ...
... Type 1 supernovae and white dwarfs When an accreting white dwarf exceeds a maximum value of 1.4 solar masses (Chandresekhar mass), electrons inside cannot provide the pressure needed to support the star. Star begins to collapse, temperature rises to the point where carbon fusion takes place. Fu ...
Chapter19
... Because the stars in a cluster have nearly the same age, they fall on an isochrone in an H-R diagram. Cluster 2 is younger because its less massive stars (which will become K and M main sequence stars) have not yet had time to reach the main sequence. Cluster 1 is older because its K stars have had ...
... Because the stars in a cluster have nearly the same age, they fall on an isochrone in an H-R diagram. Cluster 2 is younger because its less massive stars (which will become K and M main sequence stars) have not yet had time to reach the main sequence. Cluster 1 is older because its K stars have had ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.