Sunlight Timeline
... The goal of this activity is to begin understanding the speed of light and how astronomers measure distance, not by miles, but by how far light travels in space in a unit of time. If light can travel 93,000,000 miles in 8 minutes and 20 seconds, imagine how far light can travel in one year, a light ...
... The goal of this activity is to begin understanding the speed of light and how astronomers measure distance, not by miles, but by how far light travels in space in a unit of time. If light can travel 93,000,000 miles in 8 minutes and 20 seconds, imagine how far light can travel in one year, a light ...
Sunlight Timeline
... The goal of this activity is to begin understanding the speed of light and how astronomers measure distance, not by miles, but by how far light travels in space in a unit of time. If light can travel 93,000,000 miles in 8 minutes and 20 seconds, imagine how far light can travel in one year, a light ...
... The goal of this activity is to begin understanding the speed of light and how astronomers measure distance, not by miles, but by how far light travels in space in a unit of time. If light can travel 93,000,000 miles in 8 minutes and 20 seconds, imagine how far light can travel in one year, a light ...
PPT - University of Arizona
... Because light takes time to travel through space, when we look farther away in distance, we look farther back in TIME. The farthest we can see in space is 13.7 billion light years, because we think the Universe is 13.7 billion years old. ...
... Because light takes time to travel through space, when we look farther away in distance, we look farther back in TIME. The farthest we can see in space is 13.7 billion light years, because we think the Universe is 13.7 billion years old. ...
Astronomy 201: Cosmology
... 1 light minute = the distance light travels in one minute 1 light year = the distance light travels in one year = almost 10 trillion kilometers or 6 trillion miles (one trillion = 1012 = 1,000,000,000,000) Because light takes time to travel through space, when we look farther away in distance, we l ...
... 1 light minute = the distance light travels in one minute 1 light year = the distance light travels in one year = almost 10 trillion kilometers or 6 trillion miles (one trillion = 1012 = 1,000,000,000,000) Because light takes time to travel through space, when we look farther away in distance, we l ...
Unit 8 Chapter 30 Stars, Galaxies and the Universe
... Hubble found that the spectra of galaxies, except for the few closest to Earth, were shifted toward the red end of the spectrum. By examining the amount of red shift, he determined the speed at which the galaxies were moving away from Earth. Hubble found that the most distant galaxies showed the gre ...
... Hubble found that the spectra of galaxies, except for the few closest to Earth, were shifted toward the red end of the spectrum. By examining the amount of red shift, he determined the speed at which the galaxies were moving away from Earth. Hubble found that the most distant galaxies showed the gre ...
part 2 - Stardome
... the star can no longer the star This is the point where and d, war out ng iati rad of energy of gravity with the force ire ent the in – the largest explosion explodes in a supernova nts heavier rks the creation of eleme spa on losi exp universe. The supernovae are rs outer layers of these sta than i ...
... the star can no longer the star This is the point where and d, war out ng iati rad of energy of gravity with the force ire ent the in – the largest explosion explodes in a supernova nts heavier rks the creation of eleme spa on losi exp universe. The supernovae are rs outer layers of these sta than i ...
Stellar Populations Science
... The Star Formation Histories of Disk Galaxies •Potential gain of increasing aperture to ~ 40m – Crowding limit deeper by ~0.6 mag compared to 30-m for same observation, reached in same exposure time; incremental progress for most purposes – 30-m class provides a leap in number and diversity of disk ...
... The Star Formation Histories of Disk Galaxies •Potential gain of increasing aperture to ~ 40m – Crowding limit deeper by ~0.6 mag compared to 30-m for same observation, reached in same exposure time; incremental progress for most purposes – 30-m class provides a leap in number and diversity of disk ...
スライド 1 - Astrophyics Lab. in Kagoshima University
... “Nature” and “Science” journals What is currently hot topics in (radio) astronomy? • New type of radio sources (e.g. fast radio bursts) • Newly found phase of star formation and stellar evolution • Newly discovered gas dynamics • New characteristics of a black hole, a high-envergy object, and inter ...
... “Nature” and “Science” journals What is currently hot topics in (radio) astronomy? • New type of radio sources (e.g. fast radio bursts) • Newly found phase of star formation and stellar evolution • Newly discovered gas dynamics • New characteristics of a black hole, a high-envergy object, and inter ...
Extension worksheet – Topic 6 - Cambridge Resources for the IB
... The average apparent magnitude of a Cepheid star is m 5.8 and the period of variation of its luminosity is 12 days. Using the relation M 2.83log10 T 1.81 between period T (in days) and average absolute magnitude M calculate the distance to this star. ...
... The average apparent magnitude of a Cepheid star is m 5.8 and the period of variation of its luminosity is 12 days. Using the relation M 2.83log10 T 1.81 between period T (in days) and average absolute magnitude M calculate the distance to this star. ...
Light and Blackbody radiation
... • Star B is emitting the most light per area. The Stefan-Boltzman law says the Watts/m2 emitted is proportional to the temperature to the fourth power. • We can’t tell which star (A or B) is emitting the most energy in general because that depends on both size and temperature, and we only know the r ...
... • Star B is emitting the most light per area. The Stefan-Boltzman law says the Watts/m2 emitted is proportional to the temperature to the fourth power. • We can’t tell which star (A or B) is emitting the most energy in general because that depends on both size and temperature, and we only know the r ...
Lab 7: Galaxies
... version of an ellipse, it looks like a squashed circle. An elliptical galaxy has an ellisoidal shape, so no matter how it is oriented with respect to the Earth it appears to be an ellipse. Elliptical galaxies are designated by the letter “E” on the tuning fork. The letter is followed by a number 0 t ...
... version of an ellipse, it looks like a squashed circle. An elliptical galaxy has an ellisoidal shape, so no matter how it is oriented with respect to the Earth it appears to be an ellipse. Elliptical galaxies are designated by the letter “E” on the tuning fork. The letter is followed by a number 0 t ...
2008 - UCL
... List the four fundamental forces of Nature in order of decreasing strength, and name the corresponding carrier particle for each of them, as well as the particles they act upon. ...
... List the four fundamental forces of Nature in order of decreasing strength, and name the corresponding carrier particle for each of them, as well as the particles they act upon. ...
Foundation 1 - Discovering Astronomy
... for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy – occurs rapidly - called the Helium Flash ...
... for helium to begin to fuse into carbon and oxygen – core helium fusion – 3 He C + energy and C + He O + energy – occurs rapidly - called the Helium Flash ...
Topic 2 IB Chemistry Assessment Statements 2009 Revised File
... and recognize that the lines in a line spectrum are directly related to these differences. An understanding of convergence is expected. Series should be considered in the ultraviolet, visible and infrared regions of the spectrum. Calculations, knowledge of quantum numbers and historical references w ...
... and recognize that the lines in a line spectrum are directly related to these differences. An understanding of convergence is expected. Series should be considered in the ultraviolet, visible and infrared regions of the spectrum. Calculations, knowledge of quantum numbers and historical references w ...
Lecture 12
... We can directly observe the orbital motions of these stars. We can only see visual binaries if they are very near Earth. ...
... We can directly observe the orbital motions of these stars. We can only see visual binaries if they are very near Earth. ...
Which object is a meteor?
... • Not Option A (Nebular Star? What the heck is that?) • Not Option C (A Binary Star isn’t formed as a result of a star dying) • Not Option D (A supernova can be created when a star dies, but nothing is left -like with a the other options listed) • CORRECT ANSWER: Option B must be correct. A Black H ...
... • Not Option A (Nebular Star? What the heck is that?) • Not Option C (A Binary Star isn’t formed as a result of a star dying) • Not Option D (A supernova can be created when a star dies, but nothing is left -like with a the other options listed) • CORRECT ANSWER: Option B must be correct. A Black H ...
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... the answers to global warming or our energy crisis. Students must choose the destination that they feel will be most helpful to human-kind. In this MEA, students will: identify and compare characteristics of the electromagnetic spectrum such as wavelength, frequency, and energy. understand the benef ...
... the answers to global warming or our energy crisis. Students must choose the destination that they feel will be most helpful to human-kind. In this MEA, students will: identify and compare characteristics of the electromagnetic spectrum such as wavelength, frequency, and energy. understand the benef ...
Life cycle of a star
... powerful explosions in the universe, as they represent the collapse of the most massive stars. ...
... powerful explosions in the universe, as they represent the collapse of the most massive stars. ...
The Sun . . .
... H-R Diagram: Diagram that classifies stars according to their luminosity/absolute magnitude, and spectral class based on color and surface temperature. Luminosity: The brightness of a star compared to the Sun. Absolute Magnitude: Compares the brightness of stars from a standard distance ...
... H-R Diagram: Diagram that classifies stars according to their luminosity/absolute magnitude, and spectral class based on color and surface temperature. Luminosity: The brightness of a star compared to the Sun. Absolute Magnitude: Compares the brightness of stars from a standard distance ...
Monday, April 15
... Earth = a grain of sand The Earth orbits the Sun at a distance of one meter Proxima Centauri lies 270 kilometers (170 miles) away Barnard’s Star lies 370 kilometers (230 miles) away Less than 100 stars lie within 1000 kilometers (600 miles) ...
... Earth = a grain of sand The Earth orbits the Sun at a distance of one meter Proxima Centauri lies 270 kilometers (170 miles) away Barnard’s Star lies 370 kilometers (230 miles) away Less than 100 stars lie within 1000 kilometers (600 miles) ...
Contributions of astronomy to all of science
... This is a good time to reflect on the contributions that astronomy has made to all of science, and indeed to society at large. But also to reflect on the interconnectedness of science: the gifts that one science gives to another and to society. And to see science as one of the many threads tha ...
... This is a good time to reflect on the contributions that astronomy has made to all of science, and indeed to society at large. But also to reflect on the interconnectedness of science: the gifts that one science gives to another and to society. And to see science as one of the many threads tha ...
Children of the stars, children of the Universe…
... The sky should be uniformly bright, just like the surface of a star, but it is obviously not! The reason why the sky is dark is that the Universe is not infinitely old, or that the look-back time is greater than the age of the observable Universe ...
... The sky should be uniformly bright, just like the surface of a star, but it is obviously not! The reason why the sky is dark is that the Universe is not infinitely old, or that the look-back time is greater than the age of the observable Universe ...
PHYS2160 Notes 4
... is the gas (roughly 99%) and dust (roughly 1% - condensed molecular material containing silicates, graphite, silicon carbide, polycyclic aromatic hydrocarbons, water ice …) in the space between the stars. Typical sizes range from just a few molecules up to ~1µm (much smaller than the dust in your ho ...
... is the gas (roughly 99%) and dust (roughly 1% - condensed molecular material containing silicates, graphite, silicon carbide, polycyclic aromatic hydrocarbons, water ice …) in the space between the stars. Typical sizes range from just a few molecules up to ~1µm (much smaller than the dust in your ho ...
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.