Science Olympiad - Department of Physics and Astronomy
... Apparent: magnitude of the star determined by how bright it appears from the earth Absolute: magnitude of the star determined by how bright it appears from 10 parsec away ...
... Apparent: magnitude of the star determined by how bright it appears from the earth Absolute: magnitude of the star determined by how bright it appears from 10 parsec away ...
Astronomy
... • research and describe the contributions of scientists to our changing understanding of astronomy, including Ptolemy, Copernicus, Tycho Brahe, Kepler, Galileo, Newton, Einstein, and Hubble, and the contribution of women astronomers, including Maria Mitchell and Henrietta Swan Leavitt.[4B] • describ ...
... • research and describe the contributions of scientists to our changing understanding of astronomy, including Ptolemy, Copernicus, Tycho Brahe, Kepler, Galileo, Newton, Einstein, and Hubble, and the contribution of women astronomers, including Maria Mitchell and Henrietta Swan Leavitt.[4B] • describ ...
Supernova worksheet with solutions ()
... In low-mass stars, the core never gets hot or dense enough to fuse carbon and oxygen into heavier elements. Once the helium is used up, the core is able to stave off gravitational collapse with a new source of pressure: electron degeneracy pressure. This is a quantum mechanical effect similar to the ...
... In low-mass stars, the core never gets hot or dense enough to fuse carbon and oxygen into heavier elements. Once the helium is used up, the core is able to stave off gravitational collapse with a new source of pressure: electron degeneracy pressure. This is a quantum mechanical effect similar to the ...
ASTRONOMY
... 3. These cores typically have masses around 104 solar masses in the form of gas and dust. 4. The cores are denser than the outer cloud, so they collapse first. As the cores collapse they fragment into clumps around 0.1 parsecs in size and 10 to 50 solar masses in mass. 5. These clumps then form into ...
... 3. These cores typically have masses around 104 solar masses in the form of gas and dust. 4. The cores are denser than the outer cloud, so they collapse first. As the cores collapse they fragment into clumps around 0.1 parsecs in size and 10 to 50 solar masses in mass. 5. These clumps then form into ...
The Universe and Galactic Formation
... 3. These cores typically have masses around 104 solar masses in the form of gas and dust. 4. The cores are denser than the outer cloud, so they collapse first. As the cores collapse they fragment into clumps around 0.1 parsecs in size and 10 to 50 solar masses in mass. 5. These clumps then form into ...
... 3. These cores typically have masses around 104 solar masses in the form of gas and dust. 4. The cores are denser than the outer cloud, so they collapse first. As the cores collapse they fragment into clumps around 0.1 parsecs in size and 10 to 50 solar masses in mass. 5. These clumps then form into ...
Lecture 2. Thermal evolution and surface emission of
... Surprisingly, we do not see objects of this type in our vicinity. In the solar neighbourhood we meet a different class of object. ...
... Surprisingly, we do not see objects of this type in our vicinity. In the solar neighbourhood we meet a different class of object. ...
Light, Light Bulbs and the Electromagnetic Spectrum
... incandescent lamps produce a continuous spectrum, which is something like sunlight. Spectral lamps, on the other hand, emit only a few discrete wavelengths. The quality or “whiteness” of their light depends on how we perceive the particular combination of wavelengths emitted. In order to study the s ...
... incandescent lamps produce a continuous spectrum, which is something like sunlight. Spectral lamps, on the other hand, emit only a few discrete wavelengths. The quality or “whiteness” of their light depends on how we perceive the particular combination of wavelengths emitted. In order to study the s ...
The Bohr Theory, Matter Waves, and Quantum Theory
... Here, light impinges on a surface and electrons may be emitted. Classically, the energy of the light is controlled by the intensity of the light. Energy conservation products that there should be no dependence on wavelength of light. If the intensity of the light is increased, the kinetic energy of ...
... Here, light impinges on a surface and electrons may be emitted. Classically, the energy of the light is controlled by the intensity of the light. Energy conservation products that there should be no dependence on wavelength of light. If the intensity of the light is increased, the kinetic energy of ...
Astrophysics for the next decade
... How did stars and planets form? • Star formation shrouded in dust – Transition from absorbing cloud to self-luminous object ...
... How did stars and planets form? • Star formation shrouded in dust – Transition from absorbing cloud to self-luminous object ...
name - New York Science Teacher
... 1. Name the brightest star in the known universe. _____________________________ 2. What is its magnitude? ________________________ 3. Are the brightest stars low magnitude or high magnitude? ______________________________ 4. Make a top 10 list of the names of the 10 brightest stars in the known univ ...
... 1. Name the brightest star in the known universe. _____________________________ 2. What is its magnitude? ________________________ 3. Are the brightest stars low magnitude or high magnitude? ______________________________ 4. Make a top 10 list of the names of the 10 brightest stars in the known univ ...
Stellar Dynamics
... of the Milky Way appear to lie in a flattened disk-like distribution. The mid-plane of this distribution is called the “supergalactic plane”, which is nearly perpendicular to the disk of the Milky Way. In Groups, the dominant species of galaxies tend to be spirals (there are Groups known to consist ...
... of the Milky Way appear to lie in a flattened disk-like distribution. The mid-plane of this distribution is called the “supergalactic plane”, which is nearly perpendicular to the disk of the Milky Way. In Groups, the dominant species of galaxies tend to be spirals (there are Groups known to consist ...
Astro 13 Galaxies & Cosmology LECTURE 1 28 Mar 2001 D. Koo
... the ordinary star to form accretion disk around the black hole. The gas in the accretion disk is compressed and heated to such high temperatures that it becomes an intense source of X rays. ...
... the ordinary star to form accretion disk around the black hole. The gas in the accretion disk is compressed and heated to such high temperatures that it becomes an intense source of X rays. ...
How Stars Form Powerpoint
... Individual cloud fragments begin to collapse. Once the density is high enough, there is no ...
... Individual cloud fragments begin to collapse. Once the density is high enough, there is no ...
Standard
... Point-source of light and sun/earth/moon models: reasons for the seasons and lunar phases ...
... Point-source of light and sun/earth/moon models: reasons for the seasons and lunar phases ...
Overall Architecture - National Radio Astronomy Observatory
... “common” distance measurements) These must be dealt with. ...
... “common” distance measurements) These must be dealt with. ...
The Sun: Not An Average Yellow Star
... colors of the rainbow in roughly equal amounts, which is white light. If the Sun were yellow, then white T-shirts would look yellow in the mid-day sunshine. When you observe the Sun safely, by projecting its image through a pinhole camera or a telescope, you see that it is white. Don’t stare directl ...
... colors of the rainbow in roughly equal amounts, which is white light. If the Sun were yellow, then white T-shirts would look yellow in the mid-day sunshine. When you observe the Sun safely, by projecting its image through a pinhole camera or a telescope, you see that it is white. Don’t stare directl ...
File
... CLASS COPY!!! CLASS COPY!!! CLASS COPY!!! CLASS COPY!!! HR STAR DIAGRAM OBJECTIVE: Compare a stars color, temperature, brightness, and size to its spectral class. PURPOSE: Plot stars according to brightness and temperature to create an HR diagram. PROCEDURES: 1. Study the star data table on the back ...
... CLASS COPY!!! CLASS COPY!!! CLASS COPY!!! CLASS COPY!!! HR STAR DIAGRAM OBJECTIVE: Compare a stars color, temperature, brightness, and size to its spectral class. PURPOSE: Plot stars according to brightness and temperature to create an HR diagram. PROCEDURES: 1. Study the star data table on the back ...
dual nature of light
... of secondary wavelets that spread out in all directions with a speed equal to the speed of propagation of waves. ...
... of secondary wavelets that spread out in all directions with a speed equal to the speed of propagation of waves. ...
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.