Chapter 12 Quiz, Nov. 28, 2012, Astro 162, Section 4 12-1
... 12-32. Why are the spiral arms of our Galaxy brighter than the regions between them? The O and B stars formed in the spiral arms explode as supernovae before they emerge from the arms. Therefore, these stars are not found between the arms of spiral galaxies. 12-33. Describe the Sun’s motion through ...
... 12-32. Why are the spiral arms of our Galaxy brighter than the regions between them? The O and B stars formed in the spiral arms explode as supernovae before they emerge from the arms. Therefore, these stars are not found between the arms of spiral galaxies. 12-33. Describe the Sun’s motion through ...
Lecture21 - Michigan State University
... measure the spectra from spiral nebula to search for chemical compositions expected for newly forming planets • The spiral nebulae are very dim and exposures of 20 to 40 hours were required • It took 20 years to measure the spectra from 40 nebulae ISP 205 - Astronomy Gary D. Westfall ...
... measure the spectra from spiral nebula to search for chemical compositions expected for newly forming planets • The spiral nebulae are very dim and exposures of 20 to 40 hours were required • It took 20 years to measure the spectra from 40 nebulae ISP 205 - Astronomy Gary D. Westfall ...
PH607lec12-5gal3
... Often low surface brightness, so they are hard to find! Why are dwarf galaxies important?? Majority of galaxies are dwarfs!! There are probably lots of these, in the Local Group there are >30! Dwarf galaxies may be remnants of galaxy formation process: “proto-dwarf” gas clouds came together to form ...
... Often low surface brightness, so they are hard to find! Why are dwarf galaxies important?? Majority of galaxies are dwarfs!! There are probably lots of these, in the Local Group there are >30! Dwarf galaxies may be remnants of galaxy formation process: “proto-dwarf” gas clouds came together to form ...
The Halo of the Milky Way
... the line of sight from the Sun to the Galactic center. This is approximately perpendicular to the Galactic bar. This is surprising since one typically expects bars to have an angular pattern speed larger than could be sustained in the spheroid, but the possible connection should be examined. Signifi ...
... the line of sight from the Sun to the Galactic center. This is approximately perpendicular to the Galactic bar. This is surprising since one typically expects bars to have an angular pattern speed larger than could be sustained in the spheroid, but the possible connection should be examined. Signifi ...
script
... about astronomical objects as disconnected elements, rather than an integrated system. This demonstration takes visitors from our Solar System, the part of the universe with which they are most familiar, outward to our Sun’s stellar neighbors, the other stars in our Milky Way galaxy, and into the un ...
... about astronomical objects as disconnected elements, rather than an integrated system. This demonstration takes visitors from our Solar System, the part of the universe with which they are most familiar, outward to our Sun’s stellar neighbors, the other stars in our Milky Way galaxy, and into the un ...
Measuring distances to the edge of the local group
... Scientific Justification Be sure to include overall significance to astronomy. For standard proposals limit text to one page with figures, captions and references on no more than two additional pages. We propose to measure the distance to the nearby dwarf irregular galaxies Sextans A, B, and NGC 310 ...
... Scientific Justification Be sure to include overall significance to astronomy. For standard proposals limit text to one page with figures, captions and references on no more than two additional pages. We propose to measure the distance to the nearby dwarf irregular galaxies Sextans A, B, and NGC 310 ...
Chapter 25 - Haiku Learning
... Red stars are much cooler, and most of their energy is emitted as longer-wavelength red light. Stars with temperatures between 5000 and 6000 K appear yellow, like the sun. ...
... Red stars are much cooler, and most of their energy is emitted as longer-wavelength red light. Stars with temperatures between 5000 and 6000 K appear yellow, like the sun. ...
Summary Of the Structure of the Milky Way
... has yielded the orbital speed of the Sun as it orbits the galactic center and the age of the Milky Way. • Finally, when knowledge of the orbital speed of Sun is combined with its distance from the galactic center an estimate of the mass of the galaxy can be obtained. ...
... has yielded the orbital speed of the Sun as it orbits the galactic center and the age of the Milky Way. • Finally, when knowledge of the orbital speed of Sun is combined with its distance from the galactic center an estimate of the mass of the galaxy can be obtained. ...
nexstar_gt_60,80114.. - Downloads
... observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully mastered your telescope’s operation. The NexStar hand control has built-in instructions to guide you through all the alignment procedures needed to have the telescope up and running in ...
... observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully mastered your telescope’s operation. The NexStar hand control has built-in instructions to guide you through all the alignment procedures needed to have the telescope up and running in ...
White Paper on the Revival of Stellar Intensity Interferometry E. Ribak S. LeBohec
... path lengths to each receiver are much less stringent than in amplitude interferometry (AI). In particular, SII eliminates the need for adaptive optics and optical delay lines and is essentially insensitive to atmospheric turbulence and seeing conditions. As a consequence, baselines can virtually be ...
... path lengths to each receiver are much less stringent than in amplitude interferometry (AI). In particular, SII eliminates the need for adaptive optics and optical delay lines and is essentially insensitive to atmospheric turbulence and seeing conditions. As a consequence, baselines can virtually be ...
Comments
... fact that massive spheroidal galaxies appear to have formed much earlier and faster than predicted by previous semi-analytical models. After having assessed the values of the two parameters that control the effect of the complex radiative transfer processes on the time-dependent SEDs we have compare ...
... fact that massive spheroidal galaxies appear to have formed much earlier and faster than predicted by previous semi-analytical models. After having assessed the values of the two parameters that control the effect of the complex radiative transfer processes on the time-dependent SEDs we have compare ...
fifth midterm -- review problems
... Find the internal kinetic energy of the system in part (c) before and after the collision, k i and k f, respectively. If you have not solved part 9c), use v for the final velocity. A particle in space of mass m = 2.00 kg is moving with velocity v = 8 m/s î. The particle breaks up into two particles ...
... Find the internal kinetic energy of the system in part (c) before and after the collision, k i and k f, respectively. If you have not solved part 9c), use v for the final velocity. A particle in space of mass m = 2.00 kg is moving with velocity v = 8 m/s î. The particle breaks up into two particles ...
Meade Wireless Telescope Server Setup Guide - Meade
... 1.0 is, as far as we know, the first product worldwide that can be used as an astronomical device server for amateur astronomers, universities, schools and astronomical observatories. It supports Wireless LAN, IP-connections and Ethernet. This is the first step MEADE Europe is taking in terms of dev ...
... 1.0 is, as far as we know, the first product worldwide that can be used as an astronomical device server for amateur astronomers, universities, schools and astronomical observatories. It supports Wireless LAN, IP-connections and Ethernet. This is the first step MEADE Europe is taking in terms of dev ...
Cataclysmic Cosmic Events and How to Observe Them www.springer.com/series/5338
... brighter variable stars were monitored, but photography was in its infancy and digital imaging lay a century in the future. Today, at the start of the twenty-first century, amateurs are better equipped than any professionals of the mid-twentieth century, let alone the nineteenth. An amateur equipped ...
... brighter variable stars were monitored, but photography was in its infancy and digital imaging lay a century in the future. Today, at the start of the twenty-first century, amateurs are better equipped than any professionals of the mid-twentieth century, let alone the nineteenth. An amateur equipped ...
latest Edition - ExoPlanet News
... Context. Tentative correlations between the presence of dusty circumstellar debris discs and low-mass planets have been recently presented. In parallel, detailed chemical abundance studies have reported different trends between samples of planet and non-planet hosts. Whether these chemical differenc ...
... Context. Tentative correlations between the presence of dusty circumstellar debris discs and low-mass planets have been recently presented. In parallel, detailed chemical abundance studies have reported different trends between samples of planet and non-planet hosts. Whether these chemical differenc ...
The Hertzsprung-Russell Diagramm
... luminosity classes range from I for supergiant stars to VI for subdwarfs (table 5). By a detailed analysis of a stars spectra and it’s absorption lines, it is possible to classify it in this M-K system. Our sun is a G2 V, Betelgeuse a M2 Ia star. In figure 9 are shown A-class stars of different lumi ...
... luminosity classes range from I for supergiant stars to VI for subdwarfs (table 5). By a detailed analysis of a stars spectra and it’s absorption lines, it is possible to classify it in this M-K system. Our sun is a G2 V, Betelgeuse a M2 Ia star. In figure 9 are shown A-class stars of different lumi ...
Databases Meet Astronomy a db view of astronomy
... which satisfy a certain color cut, like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form adequate for visualization. Q14: Find stars with multiple measurements and have magnitude variations >0.1. Scan for stars that have a secondary object (observed at a different time) and compare their magnitud ...
... which satisfy a certain color cut, like 0.7u-0.5g-0.2i<1.25 && r<21.75, output it in a form adequate for visualization. Q14: Find stars with multiple measurements and have magnitude variations >0.1. Scan for stars that have a secondary object (observed at a different time) and compare their magnitud ...
Neon abundances - UCL Astrophysics Group
... elements in 26 HgMn, four superficially normal and 10 normal stars. We observed definite detections or determined upper limits for Ne i in 21 of the HgMn stars in the Smith & Dworetsky (1993) sample, and in 11 of the normal and superficially normal group. Some of the other stars in the two samples w ...
... elements in 26 HgMn, four superficially normal and 10 normal stars. We observed definite detections or determined upper limits for Ne i in 21 of the HgMn stars in the Smith & Dworetsky (1993) sample, and in 11 of the normal and superficially normal group. Some of the other stars in the two samples w ...
VLT/FORS Surveys of Wolf-Rayet Stars beyond the
... mass up to perhaps 20–30 MA. Observationally, there is an absence of luminous RSGs, known as the Humphreys-Davidson limit, such that initially more massive stars circumvent the RSG phase, pass through a Luminous Blue Variable stage, before ending their life as Wolf-Rayet (WR) stars, exhibiting eithe ...
... mass up to perhaps 20–30 MA. Observationally, there is an absence of luminous RSGs, known as the Humphreys-Davidson limit, such that initially more massive stars circumvent the RSG phase, pass through a Luminous Blue Variable stage, before ending their life as Wolf-Rayet (WR) stars, exhibiting eithe ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... Natural guide star AO system on Subaru telescope with IRCS. 154 hours of observation in total. 13 FoVs with 36 LBGs , 1 RadioG., and 7 DRGs are observed. Typical on-source effective integration is 5 hours. Typical PSF size at the target position is FWHM=0.2” (~1.5kpc@z=3) ...
... Natural guide star AO system on Subaru telescope with IRCS. 154 hours of observation in total. 13 FoVs with 36 LBGs , 1 RadioG., and 7 DRGs are observed. Typical on-source effective integration is 5 hours. Typical PSF size at the target position is FWHM=0.2” (~1.5kpc@z=3) ...
Chapter 1: The Sun - New Hampshire Public Television
... For 21st century cosmologists, the most important problems are to determine the rate at which the Universe is expanding and how it has expanded in the past. And most fascinating of all, will the Universe continue to expand forever? Or, depending on its total amount of matter and energy, will it coll ...
... For 21st century cosmologists, the most important problems are to determine the rate at which the Universe is expanding and how it has expanded in the past. And most fascinating of all, will the Universe continue to expand forever? Or, depending on its total amount of matter and energy, will it coll ...
Determination of accurate stellar radial
... 2002) indicates that similar or even stronger blueshifts can be expected for other spectral types. Hydrodynamic 3D simulations by Dravins & Nordlund (1990) suggest that the convective shift could be '−1.0 km s−1 for F stars to '−0.2 km s−1 for K dwarfs. Taking into consideration that the gravitation ...
... 2002) indicates that similar or even stronger blueshifts can be expected for other spectral types. Hydrodynamic 3D simulations by Dravins & Nordlund (1990) suggest that the convective shift could be '−1.0 km s−1 for F stars to '−0.2 km s−1 for K dwarfs. Taking into consideration that the gravitation ...
LT telescope proposal (2011a)
... as ‘seen’ by CoRoT; the wide span will amplify differences between these colors both form activity features as well as from the significantly different limb-darkening of the star; and z’ on its own should provide a light-curve with a diminished signal of the activity signatures. For the interpretati ...
... as ‘seen’ by CoRoT; the wide span will amplify differences between these colors both form activity features as well as from the significantly different limb-darkening of the star; and z’ on its own should provide a light-curve with a diminished signal of the activity signatures. For the interpretati ...
International Ultraviolet Explorer
The International Ultraviolet Explorer (IUE) was an astronomical observatory satellite primarily designed to take ultraviolet spectra. The satellite was a collaborative project between NASA, the UK Science Research Council and the European Space Agency (ESA). The mission was first proposed in early 1964, by a group of scientists in the United Kingdom, and was launched on January 26, 1978 aboard a NASA Delta rocket. The mission lifetime was initially set for 3 years, but in the end it lasted almost 18 years, with the satellite being shut down in 1996. The switch-off occurred for financial reasons, while the telescope was still functioning at near original efficiency.It was the first space observatory to be operated in real time by astronomers who visited the groundstations in the United States and Europe. Astronomers made over 104,000 observations using the IUE, of objects ranging from solar system bodies to distant quasars. Among the significant scientific results from IUE data were the first large scale studies of stellar winds, accurate measurements of the way interstellar dust absorbs light, and measurements of the supernova SN1987A which showed that it defied stellar evolution theories as they then stood. When the mission ended, it was considered the most successful astronomical satellite ever.