Extra-Solar Life: Habitable Zones
... for life, then there is a limited volume of any stellar system where that might exist – the Habitable Zone • If we assume temperature is dominated by sun/starlight, then the HZ can be calculated for any given star • Likely star types for life are F, G, and K stars (bigger stars die fast; M stars hav ...
... for life, then there is a limited volume of any stellar system where that might exist – the Habitable Zone • If we assume temperature is dominated by sun/starlight, then the HZ can be calculated for any given star • Likely star types for life are F, G, and K stars (bigger stars die fast; M stars hav ...
Test - Scioly.org
... i. Imperfections in the telescopes’ lenses/mirrors and general construction distort data ii. The diffraction of light blurs the observed image iii. Earth’s atmosphere has turbulence and uneven pressures that blur images iv. Photons arrive randomly at the detector, creating noisy data v. Desirabl ...
... i. Imperfections in the telescopes’ lenses/mirrors and general construction distort data ii. The diffraction of light blurs the observed image iii. Earth’s atmosphere has turbulence and uneven pressures that blur images iv. Photons arrive randomly at the detector, creating noisy data v. Desirabl ...
Stars Study Guide KEY
... 10. What is “apparent magnitude” and what does it depend on? It is how bright a star appears to our eyes as seen here on Earth. It depends on how far away the star is and how bright the star actually is (it’s absolute magnitude) 11. What is “absolute magnitude” and what does it depend on? It is how ...
... 10. What is “apparent magnitude” and what does it depend on? It is how bright a star appears to our eyes as seen here on Earth. It depends on how far away the star is and how bright the star actually is (it’s absolute magnitude) 11. What is “absolute magnitude” and what does it depend on? It is how ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean density of PMS stars of ∼750 stars deg−2. Our sensitivity limit ...
... emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean density of PMS stars of ∼750 stars deg−2. Our sensitivity limit ...
Chapter 15 (Star Lives)
... 30. Formed only during seconds of supernova core collapse. 31. Formed by main sequence stars by fusing four protons together. 32. Acts as a catalyst in hydrogen fusion in cores of hotter stars. ESSAYS 1. Explain in terms of its role in stellar evolution why iron is much more common than any other he ...
... 30. Formed only during seconds of supernova core collapse. 31. Formed by main sequence stars by fusing four protons together. 32. Acts as a catalyst in hydrogen fusion in cores of hotter stars. ESSAYS 1. Explain in terms of its role in stellar evolution why iron is much more common than any other he ...
Which Constellation is Which?
... You probably know some constellations. The Big Dipper looks like a giant pot with a long handle. Orion is named after a great hunter. You can see his belt, marked by three bright stars. Constellations are imaginary pictures in the sky. The stars look like they are all the same distance away. That’s ...
... You probably know some constellations. The Big Dipper looks like a giant pot with a long handle. Orion is named after a great hunter. You can see his belt, marked by three bright stars. Constellations are imaginary pictures in the sky. The stars look like they are all the same distance away. That’s ...
Test - Scioly.org
... D. Secondary Minimum E. Orbital Secondary 56. If the entire X-Axis (as strictly measured on the graph) spans 1.641 units, calculate the approximate period and frequency of the described binary system. A. Period: .876; Frequency: 1.14 B. Period: .853; Frequency: 1.17 C. Period: .821; Frequency: 1.21 ...
... D. Secondary Minimum E. Orbital Secondary 56. If the entire X-Axis (as strictly measured on the graph) spans 1.641 units, calculate the approximate period and frequency of the described binary system. A. Period: .876; Frequency: 1.14 B. Period: .853; Frequency: 1.17 C. Period: .821; Frequency: 1.21 ...
Beyond the Solar System By Patti Hutchison ANSWER THE
... the Milky Way, our galaxy. But wait, there's something even bigger than that- the universe! There are billions of galaxies in space. A galaxy is a group of stars, gas, and dust that are bound together by gravity. If you look into the sky on a dark night, you can see our galaxy, the Milky Way. It is ...
... the Milky Way, our galaxy. But wait, there's something even bigger than that- the universe! There are billions of galaxies in space. A galaxy is a group of stars, gas, and dust that are bound together by gravity. If you look into the sky on a dark night, you can see our galaxy, the Milky Way. It is ...
Wien`s Law and Temperature
... 8. A more accurate way to determine the spectral class of a star is by looking at the absorption lines in the star and the general shape of the curve. Don’t panic, this is almost more of an art and it takes practice, so here we go. Open the program Graphical Analysis and then open the file for star ...
... 8. A more accurate way to determine the spectral class of a star is by looking at the absorption lines in the star and the general shape of the curve. Don’t panic, this is almost more of an art and it takes practice, so here we go. Open the program Graphical Analysis and then open the file for star ...
Einstein
... • a white dwarf supernova attains 10,000,000,000 L (10 billion L) – runaway carbon fusion in core – causes explosion – since they all attain the same peak luminosity white dwarf supernovae make good distance indicators – they are more luminous than Cepheid variable stars so they can be used to mea ...
... • a white dwarf supernova attains 10,000,000,000 L (10 billion L) – runaway carbon fusion in core – causes explosion – since they all attain the same peak luminosity white dwarf supernovae make good distance indicators – they are more luminous than Cepheid variable stars so they can be used to mea ...
THE SUN IS NOT AN AVERAGE STAR Sometimes biblical creation
... The other reason is that evolutionism wants to believe that extraterrestrial life exists throughout the universe, but since it is well known that such life would have to be on "earthlike" planets near "sun-like" stars, all other such planets and stars must be like the earth and sun, or to put it dif ...
... The other reason is that evolutionism wants to believe that extraterrestrial life exists throughout the universe, but since it is well known that such life would have to be on "earthlike" planets near "sun-like" stars, all other such planets and stars must be like the earth and sun, or to put it dif ...
Chapter 3 Cosmology 3.1 The Doppler effect
... Astronomers in 1998 studying type Ia supernovae were astounded when they discovered very distant supernovae much further away than expected. To reach such distances, the supernovae must have been accelerating. The astronomers concluded that the expansion of the Universe is accelerating and has been ...
... Astronomers in 1998 studying type Ia supernovae were astounded when they discovered very distant supernovae much further away than expected. To reach such distances, the supernovae must have been accelerating. The astronomers concluded that the expansion of the Universe is accelerating and has been ...
Pre-Lab
... bright lights, the Milky Way, a band of diffuse light stretching across the dark sky, would have been as familiar as the planets and the Moon. This band of stars completely encircles Earth. It is the disk of our Galaxy seen from the inside (but not the center). With unaided eyes one other galaxy can ...
... bright lights, the Milky Way, a band of diffuse light stretching across the dark sky, would have been as familiar as the planets and the Moon. This band of stars completely encircles Earth. It is the disk of our Galaxy seen from the inside (but not the center). With unaided eyes one other galaxy can ...
Research proposal uploaded for ESO fellowship
... How is the star formation history of galaxies affected by supernovae feedback? Is this feedback powerful enough as to drive the global star formation rate decline of the universe? Supernova feedback represents a long standing problem in galaxy formation model. Currently, toy models are used to treat ...
... How is the star formation history of galaxies affected by supernovae feedback? Is this feedback powerful enough as to drive the global star formation rate decline of the universe? Supernova feedback represents a long standing problem in galaxy formation model. Currently, toy models are used to treat ...
Observational astronomy
Observational astronomy is a division of the astronomical science that is concerned with recording data, in contrast with theoretical astrophysics, which is mainly concerned with finding out the measurable implications of physical models. It is the practice of observing celestial objects by using telescopes and other astronomical apparatus.As a science, the study of astronomy is somewhat hindered in that direct experiments with the properties of the distant universe are not possible. However, this is partly compensated by the fact that astronomers have a vast number of visible examples of stellar phenomena that can be examined. This allows for observational data to be plotted on graphs, and general trends recorded. Nearby examples of specific phenomena, such as variable stars, can then be used to infer the behavior of more distant representatives. Those distant yardsticks can then be employed to measure other phenomena in that neighborhood, including the distance to a galaxy.Galileo Galilei turned a telescope to the heavens and recorded what he saw. Since that time, observational astronomy has made steady advances with each improvement in telescope technology.A traditional division of observational astronomy is given by the region of the electromagnetic spectrum observed: Optical astronomy is the part of astronomy that uses optical components (mirrors, lenses and solid-state detectors) to observe light from near infrared to near ultraviolet wavelengths. Visible-light astronomy (using wavelengths that can be detected with the eyes, about 400 - 700 nm) falls in the middle of this range. Infrared astronomy deals with the detection and analysis of infrared radiation (this typically refers to wavelengths longer than the detection limit of silicon solid-state detectors, about 1 μm wavelength). The most common tool is the reflecting telescope but with a detector sensitive to infrared wavelengths. Space telescopes are used at certain wavelengths where the atmosphere is opaque, or to eliminate noise (thermal radiation from the atmosphere). Radio astronomy detects radiation of millimetre to dekametre wavelength. The receivers are similar to those used in radio broadcast transmission but much more sensitive. See also Radio telescopes. High-energy astronomy includes X-ray astronomy, gamma-ray astronomy, and extreme UV astronomy, as well as studies of neutrinos and cosmic rays.Optical and radio astronomy can be performed with ground-based observatories, because the atmosphere is relatively transparent at the wavelengths being detected. Observatories are usually located at high altitudes so as to minimise the absorption and distortion caused by the Earth's atmosphere. Some wavelengths of infrared light are heavily absorbed by water vapor, so many infrared observatories are located in dry places at high altitude, or in space.The atmosphere is opaque at the wavelengths used by X-ray astronomy, gamma-ray astronomy, UV astronomy and (except for a few wavelength ""windows"") far infrared astronomy, so observations must be carried out mostly from balloons or space observatories. Powerful gamma rays can, however be detected by the large air showers they produce, and the study of cosmic rays is a rapidly expanding branch of astronomy.For much of the history of observational astronomy, almost all observation was performed in the visual spectrum with optical telescopes. While the Earth's atmosphere is relatively transparent in this portion of the electromagnetic spectrum, most telescope work is still dependent on seeing conditions and air transparency, and is generally restricted to the night time. The seeing conditions depend on the turbulence and thermal variations in the air. Locations that are frequently cloudy or suffer from atmospheric turbulence limit the resolution of observations. Likewise the presence of the full Moon can brighten up the sky with scattered light, hindering observation of faint objects.For observation purposes, the optimal location for an optical telescope is undoubtedly in outer space. There the telescope can make observations without being affected by the atmosphere. However, at present it remains costly to lift telescopes into orbit. Thus the next best locations are certain mountain peaks that have a high number of cloudless days and generally possess good atmospheric conditions (with good seeing conditions). The peaks of the islands of Mauna Kea, Hawaii and La Palma possess these properties, as to a lesser extent do inland sites such as Llano de Chajnantor, Paranal, Cerro Tololo and La Silla in Chile. These observatory locations have attracted an assemblage of powerful telescopes, totalling many billion US dollars of investment.The darkness of the night sky is an important factor in optical astronomy. With the size of cities and human populated areas ever expanding, the amount of artificial light at night has also increased. These artificial lights produce a diffuse background illumination that makes observation of faint astronomical features very difficult without special filters. In a few locations such as the state of Arizona and in the United Kingdom, this has led to campaigns for the reduction of light pollution. The use of hoods around street lights not only improves the amount of light directed toward the ground, but also helps reduce the light directed toward the sky.Atmospheric effects (astronomical seeing) can severely hinder the resolution of a telescope. Without some means of correcting for the blurring effect of the shifting atmosphere, telescopes larger than about 15–20 cm in aperture can not achieve their theoretical resolution at visible wavelengths. As a result, the primary benefit of using very large telescopes has been the improved light-gathering capability, allowing very faint magnitudes to be observed. However the resolution handicap has begun to be overcome by adaptive optics, speckle imaging and interferometric imaging, as well as the use of space telescopes.Astronomers have a number of observational tools that they can use to make measurements of the heavens. For objects that are relatively close to the Sun and Earth, direct and very precise position measurements can be made against a more distant (and thereby nearly stationary) background. Early observations of this nature were used to develop very precise orbital models of the various planets, and to determine their respective masses and gravitational perturbations. Such measurements led to the discovery of the planets Uranus, Neptune, and (indirectly) Pluto. They also resulted in an erroneous assumption of a fictional planet Vulcan within the orbit of Mercury (but the explanation of the precession of Mercury's orbit by Einstein is considered one of the triumphs of his general relativity theory).