Presentation
... treatments used, the observed spectral features can be reproduced. • Fine-structure dielectronic processes are important in modelling ionic recombination spectra, particularly at low temperatures (comparable to the fine-structure energy separations) • The absence of some two-body terms from the curr ...
... treatments used, the observed spectral features can be reproduced. • Fine-structure dielectronic processes are important in modelling ionic recombination spectra, particularly at low temperatures (comparable to the fine-structure energy separations) • The absence of some two-body terms from the curr ...
Lecture1
... The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit ...
... The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit ...
Astronomy 100 Name(s):
... need information on where to place the stars accurately; you will need a coordinate system to specify the position of an object in space. Astronomers use the right ascension (RA) to determine the position along the celestial equator of an object (think of it as sort of a space longitude). By traditi ...
... need information on where to place the stars accurately; you will need a coordinate system to specify the position of an object in space. Astronomers use the right ascension (RA) to determine the position along the celestial equator of an object (think of it as sort of a space longitude). By traditi ...
How did the solar system form? (reading
... Like most creation stories, this one is dramatic: we began, not as a mere glimmer buried in an obscure cloud, but instead amidst the glare and turmoil of restless giants. Or so says a new theory, supported by stunning astronomical images and hard chemical analysis. For years most astronomers have im ...
... Like most creation stories, this one is dramatic: we began, not as a mere glimmer buried in an obscure cloud, but instead amidst the glare and turmoil of restless giants. Or so says a new theory, supported by stunning astronomical images and hard chemical analysis. For years most astronomers have im ...
Lecture13 - University of Waterloo
... • 23 He is an intermediate species in the pp chain. It is most abundant at the top of the H-burning region, where the temperature is lower. • Abundances are homogeneous within the convective zone, since the plasma is effectively mixed ...
... • 23 He is an intermediate species in the pp chain. It is most abundant at the top of the H-burning region, where the temperature is lower. • Abundances are homogeneous within the convective zone, since the plasma is effectively mixed ...
To the Stars - LBlackwell
... super massive black hole. A black hole is a region of space where gravity is so strong that nothing, not even light, can escape. The Affect of a Black Hole: Stars are pulled into the hole and destroyed. The mass of the star adds to the black holes mass, increasing its size. The black hole in o ...
... super massive black hole. A black hole is a region of space where gravity is so strong that nothing, not even light, can escape. The Affect of a Black Hole: Stars are pulled into the hole and destroyed. The mass of the star adds to the black holes mass, increasing its size. The black hole in o ...
PART 3 Galaxies
... The primary reason that massive O-type stars are not found in the galactic halo is because they are a) too massive to be kicked into the halo from the disk. b) so massive that they settle into the thinner disk. c) too short-lived to have persisted from halo formation until today. d) closer to us in ...
... The primary reason that massive O-type stars are not found in the galactic halo is because they are a) too massive to be kicked into the halo from the disk. b) so massive that they settle into the thinner disk. c) too short-lived to have persisted from halo formation until today. d) closer to us in ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... or in q a stellar system PN V = (1/N ) i=1 (vi − v̄)2 where PN v̄ = (1/N ) i=1 vi is the mean velocity and N is the total number of stars • A true MB distribution has a “tail” • Stars will be lost from the cluster • The escape speed ve = 2V ...
... or in q a stellar system PN V = (1/N ) i=1 (vi − v̄)2 where PN v̄ = (1/N ) i=1 vi is the mean velocity and N is the total number of stars • A true MB distribution has a “tail” • Stars will be lost from the cluster • The escape speed ve = 2V ...
B/W
... 1) mixing of central material to the surface 2) large scale mass loss of outer layers exposing interior (e.g. helium stars) 3) mass transfer in a binary (e.g. barium stars) 4) pollution with supernova material from a binary companion (e.g. Nova Sco) Sub-stellar objects ...
... 1) mixing of central material to the surface 2) large scale mass loss of outer layers exposing interior (e.g. helium stars) 3) mass transfer in a binary (e.g. barium stars) 4) pollution with supernova material from a binary companion (e.g. Nova Sco) Sub-stellar objects ...
Master Page
... Really, really dark. There are no major cities around to pollute the area with light. On a clear night in Sutherland the sky is better than any TV show. You can see thousands of stars, yes, even without a telescope. Constellations that most of us who live in cities never ever see, even though they a ...
... Really, really dark. There are no major cities around to pollute the area with light. On a clear night in Sutherland the sky is better than any TV show. You can see thousands of stars, yes, even without a telescope. Constellations that most of us who live in cities never ever see, even though they a ...
Was our Solar System Born inside a Wolf
... temperature of these hot stars results in a large number of ionizing photons. The combined action of the supersonic winds and ionizing radiation results in the formation of photo-ionized wind-blown bubbles around the stars, consisting of a low-density interior surrounded by a high-density shell (Fig ...
... temperature of these hot stars results in a large number of ionizing photons. The combined action of the supersonic winds and ionizing radiation results in the formation of photo-ionized wind-blown bubbles around the stars, consisting of a low-density interior surrounded by a high-density shell (Fig ...
Lect12-3-10-10
... Behind the visible nebula is a dense cloud of molecular hydrogen gas, from which infrared observations show that many more stars have recently formed. In time, these newest stars will also expel the bulk of the gas in the cloud which now obscures them from view in visible light. Thus the process of ...
... Behind the visible nebula is a dense cloud of molecular hydrogen gas, from which infrared observations show that many more stars have recently formed. In time, these newest stars will also expel the bulk of the gas in the cloud which now obscures them from view in visible light. Thus the process of ...
Discussion Activity #13
... than it is today? A. The total amount of gas will be about the same, but it will contain a much higher percentage of elements heavier than hydrogen and helium. B. Thanks to the recycling of the star-gas-star cycle, the interstellar medium should look about the same in 50 billion years as it does tod ...
... than it is today? A. The total amount of gas will be about the same, but it will contain a much higher percentage of elements heavier than hydrogen and helium. B. Thanks to the recycling of the star-gas-star cycle, the interstellar medium should look about the same in 50 billion years as it does tod ...
Radio Microwave Infrared Visible Speed in Vacuum 3.00 x 108 m s
... Warm Objects Terrain Clouds Meteorology Communication GPS Cell Phones Microwaves ...
... Warm Objects Terrain Clouds Meteorology Communication GPS Cell Phones Microwaves ...
Life and Death of a Star The Universe Season 1 Episode 10
... Life on the main sequence can only last as long as there is _____________________ When fuel runs out, gravity __________________ and star will start to________________________________. Larger stars = ___________________________________ ...
... Life on the main sequence can only last as long as there is _____________________ When fuel runs out, gravity __________________ and star will start to________________________________. Larger stars = ___________________________________ ...
To understand the deaths of stars and how it
... Stars 8-20 times the mass of the sun. • The start is the same as the sun. • However, once Helium gets fused into carbon the core is able to ready 600 million degrees. • At 600 million degrees Carbon fuses with Carbon to form an array of heavier elements. • At a billion degrees Oxygen can fuse with ...
... Stars 8-20 times the mass of the sun. • The start is the same as the sun. • However, once Helium gets fused into carbon the core is able to ready 600 million degrees. • At 600 million degrees Carbon fuses with Carbon to form an array of heavier elements. • At a billion degrees Oxygen can fuse with ...
Stars, The Sun, and Star Constellation
... The suns pressure is 340 billion times of earths air pressure at sea level A nuclear reaction can occur with protons and hydrogen nuclei to fuse together Its mass is expelled as energy because of convection Every second 700 million tons of hydrogen is converted to helium ash The corona is the outer ...
... The suns pressure is 340 billion times of earths air pressure at sea level A nuclear reaction can occur with protons and hydrogen nuclei to fuse together Its mass is expelled as energy because of convection Every second 700 million tons of hydrogen is converted to helium ash The corona is the outer ...
ASTRONOMY 1 ... You may use this only this study guide for reference... No electronic devises: I pads, lap tops, phones, etc.
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
Big Bang, 429
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
... 38. Where are elements heavier than iron can only be created ? 39. When the mass of a star's core becomes greater than 1.4 times the mass of the Sun, degenerate electrons can no longer keep it as a white dwarf. Instead, what does it become? 40. To predict whether a star will ultimately become a blac ...
Stars presentation by lauren
... brighter than our sun! It is over 45,000 light years away from Earth, and is at least 150 times bigger than the sun! ...
... brighter than our sun! It is over 45,000 light years away from Earth, and is at least 150 times bigger than the sun! ...
From studying our solar system to searching for worlds beyond and
... characterizing exoplanetary atmospheres, specifically around a class of short-period gas giant worlds known as hot Jupiters. “Much of our understanding of planetary atmospheres is based on models developed to describe the solar system planets,” she explains. “By studying the properties of planets th ...
... characterizing exoplanetary atmospheres, specifically around a class of short-period gas giant worlds known as hot Jupiters. “Much of our understanding of planetary atmospheres is based on models developed to describe the solar system planets,” she explains. “By studying the properties of planets th ...
Cosmic Collisions
... scattered in random directions, but gravity acts so gradually that planetary orbits are not disturbed. A collision takes about a billion years; during the last billion years, life on Earth evolved from single-celled organisms to amazingly primative apes who still think digital watches are pretty nea ...
... scattered in random directions, but gravity acts so gradually that planetary orbits are not disturbed. A collision takes about a billion years; during the last billion years, life on Earth evolved from single-celled organisms to amazingly primative apes who still think digital watches are pretty nea ...
01-Introduction
... Even recently, little was known about how stars presently form and the birth itself remained an absolute mystery. There was a mute gap left exclusively to hand-waving gestures. Even in the best circumstances, we were restricted to weak evidence which often led to indecisive or contradictory conclusi ...
... Even recently, little was known about how stars presently form and the birth itself remained an absolute mystery. There was a mute gap left exclusively to hand-waving gestures. Even in the best circumstances, we were restricted to weak evidence which often led to indecisive or contradictory conclusi ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.