AY 12 Homework #4 Solutions Winter 2016 Longer Problems 1. a
... f) A star cannot become arbitrarily large. At around 150 M , the radiation pressure in the star becomes so great as to overcome gravity and blow the star apart. Thus, a star above 150 M cannot exist. 5. A Type II supernova would occur first in a cluster of stars. This is because Type II supernovae ...
... f) A star cannot become arbitrarily large. At around 150 M , the radiation pressure in the star becomes so great as to overcome gravity and blow the star apart. Thus, a star above 150 M cannot exist. 5. A Type II supernova would occur first in a cluster of stars. This is because Type II supernovae ...
Cutting-edge chemistry
... by Jayne Birkby of Leiden University, Netherlands, may out at us,’ said Birkby, conveying her excitement that this now move on to other atmospheric molecules such as technique could be used ‘to look for Earth-twin planets’. O2, CO2 and CH4. The researchers can now move on to looking for more Old pri ...
... by Jayne Birkby of Leiden University, Netherlands, may out at us,’ said Birkby, conveying her excitement that this now move on to other atmospheric molecules such as technique could be used ‘to look for Earth-twin planets’. O2, CO2 and CH4. The researchers can now move on to looking for more Old pri ...
Powerpoint Slides
... Where d, is the slit separation, is the angle between the maxima and the optical axis, n is the order of intensity (i.e. n = 1, 2 3, ..etc.), and is the wavelength of light. Notice that for small angles, < 5o, sin = tan , and for this situation tan is: ...
... Where d, is the slit separation, is the angle between the maxima and the optical axis, n is the order of intensity (i.e. n = 1, 2 3, ..etc.), and is the wavelength of light. Notice that for small angles, < 5o, sin = tan , and for this situation tan is: ...
Chapter 6: Electronic Structure of Atoms
... explain how Einstein made use of it in his theory of the photoelectric effect. 2. A laser emits a wavelength of 987 nm. In what portion of the spectrum is this found? Its output energy is absorbed in a detector that measures a total energy of 0.52 J over 32 seconds. How many photons per second are b ...
... explain how Einstein made use of it in his theory of the photoelectric effect. 2. A laser emits a wavelength of 987 nm. In what portion of the spectrum is this found? Its output energy is absorbed in a detector that measures a total energy of 0.52 J over 32 seconds. How many photons per second are b ...
Practice questions for Stars File
... 4. Explain how the energy changes are involved in each of their life cycles from birth to death. 5. Explain how the gravity changes are related to the final stages in the life cycle of large and massive stars. ...
... 4. Explain how the energy changes are involved in each of their life cycles from birth to death. 5. Explain how the gravity changes are related to the final stages in the life cycle of large and massive stars. ...
HE and VHE emission from X-ray binaries
... Models predict that radio jets could be natural sites for the production of high energy photons via both Compton scattering and maybe direct synchrotron emission. Leptonic and hadronic processes could be behind TeV emission. Up to now, above ~ 500 keV, a handful of µqs have been detected: Cygn ...
... Models predict that radio jets could be natural sites for the production of high energy photons via both Compton scattering and maybe direct synchrotron emission. Leptonic and hadronic processes could be behind TeV emission. Up to now, above ~ 500 keV, a handful of µqs have been detected: Cygn ...
Lecture 6 - Stars and Distances
... Explained Werthimer, “if we had looked at the sky even a few seconds later we wouldn’t have found a match” for this candidate. A signal that drifts so quickly that it can only be heard for seconds at a time at a given frequency can only be detected by blind luck. Needless to say, such a transmission ...
... Explained Werthimer, “if we had looked at the sky even a few seconds later we wouldn’t have found a match” for this candidate. A signal that drifts so quickly that it can only be heard for seconds at a time at a given frequency can only be detected by blind luck. Needless to say, such a transmission ...
Document
... material are in a perpetual battle between forces pulling in (gravity) and forces pushing out (pressure). • Gravity comes from the mass of the cloud or star. • Pressure comes from the motion of the atoms or molecules. – Think of hot air balloons. – The hotter the air, the bigger the ...
... material are in a perpetual battle between forces pulling in (gravity) and forces pushing out (pressure). • Gravity comes from the mass of the cloud or star. • Pressure comes from the motion of the atoms or molecules. – Think of hot air balloons. – The hotter the air, the bigger the ...
Star formation and lifetimes
... • Very small stars live a long time (100 billions of years) • Our SUN: will live a total of about 10 billion years (half used up) ...
... • Very small stars live a long time (100 billions of years) • Our SUN: will live a total of about 10 billion years (half used up) ...
– 1 – 1. Feedback From The First Stars
... to detect these energetic photons emitted from regions of high dark matter content. These might include the central region of the Milky Way, nearby dwarf spheroidal galaxies, or dark satellites of the Galaxy (small halos that have been accreted to our galaxy, but never formed stars). If annihilation ...
... to detect these energetic photons emitted from regions of high dark matter content. These might include the central region of the Milky Way, nearby dwarf spheroidal galaxies, or dark satellites of the Galaxy (small halos that have been accreted to our galaxy, but never formed stars). If annihilation ...
powerpoint - Physics @ IUPUI
... • Instead of galaxies flying away from us they now come towards us. • All the galaxies would meet in 1 region of space (all the ones we can see anyway). • As that happens the temperature of the gas would be higher (simple gas law). • If the gas gets too hot the atom becomes ionized. • What that mean ...
... • Instead of galaxies flying away from us they now come towards us. • All the galaxies would meet in 1 region of space (all the ones we can see anyway). • As that happens the temperature of the gas would be higher (simple gas law). • If the gas gets too hot the atom becomes ionized. • What that mean ...
For stars
... • Rigel (m = 0.12) • Spica (m = +1.0) • Which looks brighter? Rigel BUT... It turns out that Spica actually gives off 1000 times more light than Rigel!! SO..If Spica is giving off more light, why would it appear dimmer in the sky here at Earth? ...
... • Rigel (m = 0.12) • Spica (m = +1.0) • Which looks brighter? Rigel BUT... It turns out that Spica actually gives off 1000 times more light than Rigel!! SO..If Spica is giving off more light, why would it appear dimmer in the sky here at Earth? ...
What powers luminous infrared galaxies?
... Abstract. Based on the initial data sets taken with the ISO short wavelength spectrometer (SWS) we present a first discussion of the source of luminosity of (ultra-)luminous infrared galaxies (ULIRGs). By comparison of observations of 2.5-45m lines to classical starbursts and active galactic nuclei ...
... Abstract. Based on the initial data sets taken with the ISO short wavelength spectrometer (SWS) we present a first discussion of the source of luminosity of (ultra-)luminous infrared galaxies (ULIRGs). By comparison of observations of 2.5-45m lines to classical starbursts and active galactic nuclei ...
A Summary of Stages
... The "flash" results in two things : #1 - a hot carbon core begins to form inside the helium core, and #2 - the star physically changes, moving to the hotter, but somewhat dimmer, horizontal branch of the H-R Diagram, where it stays for many years, at a precise place determined by its mass (sort of a ...
... The "flash" results in two things : #1 - a hot carbon core begins to form inside the helium core, and #2 - the star physically changes, moving to the hotter, but somewhat dimmer, horizontal branch of the H-R Diagram, where it stays for many years, at a precise place determined by its mass (sort of a ...
Stars are made of very hot gas. This gas is mostly hydrogen and
... part of the fire at the top of the flame glows red, the hotter part in the middle glows yellow, and the hottest part near the fuel glows blue. Stars work the same way. Their temperature determine what color they will be. Thus we can determine how hot a star is just by looking at its color. ...
... part of the fire at the top of the flame glows red, the hotter part in the middle glows yellow, and the hottest part near the fuel glows blue. Stars work the same way. Their temperature determine what color they will be. Thus we can determine how hot a star is just by looking at its color. ...
The stellar populations in the low-luminosity, early
... which are much fainter than our original sample of LLEs, and have stellar masses of only a few × 107 M or less (
... which are much fainter than our original sample of LLEs, and have stellar masses of only a few × 107 M or less (
Chapter 2 Waves and Particles De Broglie wavelength: λ=h/p, where
... Eg. An UV light of wavelength 350nm and intensity 1W/m2 is incident at the potassium surface. (a) Find the maximum kinetic energy of photoelectrons. (b) If 0.5 percentages of the incident photons produce photoelectrons, how many photoelectrons/sec are emitted if potassium surface has an area of 1cm2 ...
... Eg. An UV light of wavelength 350nm and intensity 1W/m2 is incident at the potassium surface. (a) Find the maximum kinetic energy of photoelectrons. (b) If 0.5 percentages of the incident photons produce photoelectrons, how many photoelectrons/sec are emitted if potassium surface has an area of 1cm2 ...
Life and Death of a Star The Universe Season 1 Episode 10
... into such density that the gravity field is enormous. Light can’t leave because the gravity is so strong. There is limit to where you will get pulled into a black hole. ...
... into such density that the gravity field is enormous. Light can’t leave because the gravity is so strong. There is limit to where you will get pulled into a black hole. ...
Basic Properties of the Stars
... If two stars have the same temperature, each square meter gives off the same amount of light (E = σ T4). If one of the two stars has 100 times the luminosity of the other, it must have 100 times the surface area, or 10 times the diameter. Hertzsprung and Russell realized that the stars at the ...
... If two stars have the same temperature, each square meter gives off the same amount of light (E = σ T4). If one of the two stars has 100 times the luminosity of the other, it must have 100 times the surface area, or 10 times the diameter. Hertzsprung and Russell realized that the stars at the ...
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.