Astro 27 Solar System Formation and ExoPlanets Slide Show
... • The “Fast” scenario: eddys form, merge. Eddys include not just dust (which is only ~2% of total mass recall), but hydrogen and helium as well (much more mass here). The growth rate would be much faster as gravity would kick in right away for such massive objects. ...
... • The “Fast” scenario: eddys form, merge. Eddys include not just dust (which is only ~2% of total mass recall), but hydrogen and helium as well (much more mass here). The growth rate would be much faster as gravity would kick in right away for such massive objects. ...
Chapter 10: Simple Harmonic Motion
... illuminates a single slit 0.750 mm in width. (a) At what distance from the slit should a screen be located if the first minimum in the diffraction pattern is to be 0.850 mm from the center of the principal maximum? (b) What is the width of the central maximum? ...
... illuminates a single slit 0.750 mm in width. (a) At what distance from the slit should a screen be located if the first minimum in the diffraction pattern is to be 0.850 mm from the center of the principal maximum? (b) What is the width of the central maximum? ...
Cepheus (constellation)
... • NGC 188 is an open cluster that has the distinction of being the closest open cluster to the north celestial pole, as well as one of the oldest known open clusters. • The Fireworks Galaxy (NGC 6946) is a spiral galaxy in which nine supernovae have been observed, more than in any other galaxy. • IC ...
... • NGC 188 is an open cluster that has the distinction of being the closest open cluster to the north celestial pole, as well as one of the oldest known open clusters. • The Fireworks Galaxy (NGC 6946) is a spiral galaxy in which nine supernovae have been observed, more than in any other galaxy. • IC ...
L101 DETECTION OF A LARGE ARC OF IONIZED HYDROGEN
... one of its primary missions, a northern sky Ha survey, consisting of 37,300 spectra on a 0⬚. 85 # 0⬚. 98 grid above ⫺30⬚ declination. Each spectrum was centered near the LSR velocity and had a sensitivity limit of approximately 0.1 R, where 1 R (rayleigh) is 106/4p photons cm⫺2 s⫺1 sr⫺1 or 2.41 # 10 ...
... one of its primary missions, a northern sky Ha survey, consisting of 37,300 spectra on a 0⬚. 85 # 0⬚. 98 grid above ⫺30⬚ declination. Each spectrum was centered near the LSR velocity and had a sensitivity limit of approximately 0.1 R, where 1 R (rayleigh) is 106/4p photons cm⫺2 s⫺1 sr⫺1 or 2.41 # 10 ...
Astronomy 321 --- Homework Exercise: Star Wheel
... in mind that the locations of the constellations will vary depending on the time of night you observe. In the tables below, the first column is the constellation, with its standard 3-letter abbreviation in parentheses. For constellations with bright stars, one or two of these bright stars are listed ...
... in mind that the locations of the constellations will vary depending on the time of night you observe. In the tables below, the first column is the constellation, with its standard 3-letter abbreviation in parentheses. For constellations with bright stars, one or two of these bright stars are listed ...
Starry Dome: Astronomy in Art and the Imagination
... earliest telescopes experimented with the use of mirrors and paralleled major advances in the creation of new and different kinds of lenses. The most common and oldest telescope is the optical telescope. The optical telescope works by gathering and focusing light from the visible light spectrum- the ...
... earliest telescopes experimented with the use of mirrors and paralleled major advances in the creation of new and different kinds of lenses. The most common and oldest telescope is the optical telescope. The optical telescope works by gathering and focusing light from the visible light spectrum- the ...
the K-12 Teacher Resource Packet for
... earliest telescopes experimented with the use of mirrors and paralleled major advances in the creation of new and different kinds of lenses. The most common and oldest telescope is the optical telescope. The optical telescope works by gathering and focusing light from the visible light spectrum- the ...
... earliest telescopes experimented with the use of mirrors and paralleled major advances in the creation of new and different kinds of lenses. The most common and oldest telescope is the optical telescope. The optical telescope works by gathering and focusing light from the visible light spectrum- the ...
Viewing the Sky - Indiana University Astronomy
... 1. Once you have found the North Star, look toward it. South will be behind you, east will be to your right, and west to your left. Match up the stars you see in the northern sky with the constellations shown on the sky chart. Some constellations are faint and hard to see if sky is too bright from n ...
... 1. Once you have found the North Star, look toward it. South will be behind you, east will be to your right, and west to your left. Match up the stars you see in the northern sky with the constellations shown on the sky chart. Some constellations are faint and hard to see if sky is too bright from n ...
High-Mass Star Formation
... CAVEAT: may be contribution from compact components (UCHIIs or disks) within central beam W3(OH) UCHII may contribute as much as 25% of the central flux assuming optically thick free-free scaled from 3mm flux (Wilner, Welch, & Forster 1995) ...
... CAVEAT: may be contribution from compact components (UCHIIs or disks) within central beam W3(OH) UCHII may contribute as much as 25% of the central flux assuming optically thick free-free scaled from 3mm flux (Wilner, Welch, & Forster 1995) ...
JSK_PPV_poster - The Formation & Evolution of Planetary
... 2. As seen in Figure 1 & 2, the improved sensitivity of Spitzer allows us to detect debris disk systems that are much fainter than those detected by IRAS and ISO. The overall impression is that Kuiper-Belt (KB)-like systems detectable by Spitzer and considered in this paper are less massive and more ...
... 2. As seen in Figure 1 & 2, the improved sensitivity of Spitzer allows us to detect debris disk systems that are much fainter than those detected by IRAS and ISO. The overall impression is that Kuiper-Belt (KB)-like systems detectable by Spitzer and considered in this paper are less massive and more ...
The Naked Eye Stars as Data Supporting Galileo`s
... FIGURE 5: Simulated field of stars of magnitudes 1 through 6 (larger circles representing brighter stars). Top left -- numbers of each magnitude in proportions found in Bright Star Catalog (i.e. real sky). Top right -numbers calculated via equation 3. Bottom left, equal numbers of each magnitude. B ...
... FIGURE 5: Simulated field of stars of magnitudes 1 through 6 (larger circles representing brighter stars). Top left -- numbers of each magnitude in proportions found in Bright Star Catalog (i.e. real sky). Top right -numbers calculated via equation 3. Bottom left, equal numbers of each magnitude. B ...
Colorimeters
... absorb light for a variety of reasons. Pigments absorb light at different wavelengths. A cloudy solution will simply scatter/block the passage of light (sometimes a colorimeter is used to monitor the growth of a bacterial or yeast culture). The % transmission or the % absorbance is recorded (you c ...
... absorb light for a variety of reasons. Pigments absorb light at different wavelengths. A cloudy solution will simply scatter/block the passage of light (sometimes a colorimeter is used to monitor the growth of a bacterial or yeast culture). The % transmission or the % absorbance is recorded (you c ...
Accretion
... AGNs and QUASARS like powered by supermassive black holes (SMBHs). These were probably born in the early Universe from collapse of Supermassive Stars (> 100 Mo) and then accrete gas from the galaxy in which they were born: connection between galaxy formation and supermassive black holes, hot topic o ...
... AGNs and QUASARS like powered by supermassive black holes (SMBHs). These were probably born in the early Universe from collapse of Supermassive Stars (> 100 Mo) and then accrete gas from the galaxy in which they were born: connection between galaxy formation and supermassive black holes, hot topic o ...
Lawrence Livermore National Laboratory Radiation
... How do we use a particle based simulation to capture short distance QM effects and long distance classical effects? Weapons and Complex Integration ...
... How do we use a particle based simulation to capture short distance QM effects and long distance classical effects? Weapons and Complex Integration ...
Observational Confirmation of a Link Between Common Envelope
... and low measured expansion velocities for the bright ring. The color image of NGC 6337 from Hillwig et al. (2010) is shown in Figure 7. We find from our images that the ring is not sharply delineated. Thus, assuming the equatorial ring is uniform in radius, inclinations as high as ∼ 20◦ still produc ...
... and low measured expansion velocities for the bright ring. The color image of NGC 6337 from Hillwig et al. (2010) is shown in Figure 7. We find from our images that the ring is not sharply delineated. Thus, assuming the equatorial ring is uniform in radius, inclinations as high as ∼ 20◦ still produc ...
Can we determine the grain composition of the Interstellar Medium with
... Bound-free case for isolated atoms X-ray absorption through the photoelectric process ...
... Bound-free case for isolated atoms X-ray absorption through the photoelectric process ...
Document
... 1. Why is it important that telescopes be large? 2. Why do most modern telescopes use a large mirror rather than a large lens? 3. Why are observatories in such remote locations? 4. Do astronomers use ordinary photographic film to take pictures of the sky? Do they actually look through large telescop ...
... 1. Why is it important that telescopes be large? 2. Why do most modern telescopes use a large mirror rather than a large lens? 3. Why are observatories in such remote locations? 4. Do astronomers use ordinary photographic film to take pictures of the sky? Do they actually look through large telescop ...
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.