School of Physics Multiwavelength Observations of Evolved Stars Research project in Astrophysics
... systems containing evolved giant stars with masses similar to that of our own Sun. Although supernovae are showy objects, stars with mass similar to our Sun are much more plentiful and when they evolve to the red giant stage they begin to lose processed material in the form of a cool wind. These sta ...
... systems containing evolved giant stars with masses similar to that of our own Sun. Although supernovae are showy objects, stars with mass similar to our Sun are much more plentiful and when they evolve to the red giant stage they begin to lose processed material in the form of a cool wind. These sta ...
Solar System Essays, Symeonides Answers
... The typical gas giant planet is many times larger than the Earth. Gas giants have very small metal or rocky cores, since most of these materials stayed near the center of the solar nebula as the solar system formed. Then there is a thick layer of liquid or frozen gasses. This would be the planet’s s ...
... The typical gas giant planet is many times larger than the Earth. Gas giants have very small metal or rocky cores, since most of these materials stayed near the center of the solar nebula as the solar system formed. Then there is a thick layer of liquid or frozen gasses. This would be the planet’s s ...
Star Formation in Lynds Dark Nebulae
... beginning of time (Yan, 05). Dust found in molecular clouds is crucial to the star formation process, as it allows gas to condense into pre-stellar cores and evolve into YSOs, or young stellar objects (Greene, 01). Research by Carballo (1992) identified new candidate YSOs in Scorpio-Centaurus Lupus, ...
... beginning of time (Yan, 05). Dust found in molecular clouds is crucial to the star formation process, as it allows gas to condense into pre-stellar cores and evolve into YSOs, or young stellar objects (Greene, 01). Research by Carballo (1992) identified new candidate YSOs in Scorpio-Centaurus Lupus, ...
What is a Star? - Lisle CUSD 202
... The pressure exerted on the core by the outer layers does not produce enough energy to start carbon fusion. The core is now very dense and very hot. (A tablespoon full would weigh 5 tons!) The stars outer layers drift away and become a planetary nebula. A white dwarf is about 8,000 miles in diameter ...
... The pressure exerted on the core by the outer layers does not produce enough energy to start carbon fusion. The core is now very dense and very hot. (A tablespoon full would weigh 5 tons!) The stars outer layers drift away and become a planetary nebula. A white dwarf is about 8,000 miles in diameter ...
Reprint
... The origin of carbon lies in nucleosynthesis in stars. There are two main contributors to carbon, supernovae (12 C) and evolved stars (12 C and 13 C), including red giants, supergiants, and asymptotic giant branch (AGB) stars. Stellar yields from such objects result in an average galactic C/O ratio ...
... The origin of carbon lies in nucleosynthesis in stars. There are two main contributors to carbon, supernovae (12 C) and evolved stars (12 C and 13 C), including red giants, supergiants, and asymptotic giant branch (AGB) stars. Stellar yields from such objects result in an average galactic C/O ratio ...
Astronomy lab: Planets
... A view of the solar system as seen FROM ABOVE THE NORTH ECLIPTIC POLE with the sun in the center is shown below. The line from the Earth ( ) to the sun () represents the planetary longitude of the sun. For each of the five visible planets, 1) Center a protractor on the Earth, measure the elongation ...
... A view of the solar system as seen FROM ABOVE THE NORTH ECLIPTIC POLE with the sun in the center is shown below. The line from the Earth ( ) to the sun () represents the planetary longitude of the sun. For each of the five visible planets, 1) Center a protractor on the Earth, measure the elongation ...
COSMOLOGY 1 An Introduction to the Universe
... continues in a shell around the core and the star evolves into a red giant. When the Sun becomes a red giant, its atmosphere will envelope the Earth and our planet will be consumed in a fiery death. Meanwhile, the core of the star collapses under gravity's pull until it reaches a high enough density ...
... continues in a shell around the core and the star evolves into a red giant. When the Sun becomes a red giant, its atmosphere will envelope the Earth and our planet will be consumed in a fiery death. Meanwhile, the core of the star collapses under gravity's pull until it reaches a high enough density ...
Life Cycle of a Star
... When the core is trying to fuse Fe No more energy can be gained Fusion stops, no more outward pressure Gravity Wins … the collapse starts After the collapse … rebound … material explodes out Heavy elements formed during these final stages ...
... When the core is trying to fuse Fe No more energy can be gained Fusion stops, no more outward pressure Gravity Wins … the collapse starts After the collapse … rebound … material explodes out Heavy elements formed during these final stages ...
Open clusters
... there are many more low-luminosity stars than highluminosity stars there are many more low-mass stars than highmass stars ...
... there are many more low-luminosity stars than highluminosity stars there are many more low-mass stars than highmass stars ...
NORTH STAR PEOPLE
... arrow, is the spot that marks the center of our own galaxy, the Milky Way. The view towards the south is the most dazzling, interesting and inspiring view. If you turn around and face the north you will see a relatively dark sky. No really bright stars shine there, few interesting nebulae or galaxie ...
... arrow, is the spot that marks the center of our own galaxy, the Milky Way. The view towards the south is the most dazzling, interesting and inspiring view. If you turn around and face the north you will see a relatively dark sky. No really bright stars shine there, few interesting nebulae or galaxie ...
Stellar evolution
... They are on the order of 10 km in diameter. One teaspoon weighs 1 billion tons. Some rotate at very high speeds, and are called pulsars. Pulsars have extreme magnetic fields. ...
... They are on the order of 10 km in diameter. One teaspoon weighs 1 billion tons. Some rotate at very high speeds, and are called pulsars. Pulsars have extreme magnetic fields. ...
Yes - Wichita State University
... •Measure the oxygen gradient in the ISM of the Milky Way disk •Employ planetary nebulae as abundance probes •Perform detailed statistical treatment of data ...
... •Measure the oxygen gradient in the ISM of the Milky Way disk •Employ planetary nebulae as abundance probes •Perform detailed statistical treatment of data ...
CBradleyLoutl
... Stars start from these larger, denser clouds of gas. Any small deviation in density will break the whole cloud into a number of condensed groups, if a group has over a certain mass, gravity will be strong enough to condense it into a star. First, a high mass cloud will contract, then begin breaking ...
... Stars start from these larger, denser clouds of gas. Any small deviation in density will break the whole cloud into a number of condensed groups, if a group has over a certain mass, gravity will be strong enough to condense it into a star. First, a high mass cloud will contract, then begin breaking ...
Die Sonne im Röntgenlicht - ST-ECF
... • Only observable from the space • Excellent imaging stability • Little background due to the Earth’s warm atmosphere Wang et al. 2009 ...
... • Only observable from the space • Excellent imaging stability • Little background due to the Earth’s warm atmosphere Wang et al. 2009 ...
Stellar Evolution
... in their outer layers. The outward thermal pressure increases enough to expand the outer layers of the star. The trapped energy is able to escape when the outer layers are expanded and the thermal pressure drops. Gravity takes over and the star shrinks, but it shrinks beyond the equilibrium point. T ...
... in their outer layers. The outward thermal pressure increases enough to expand the outer layers of the star. The trapped energy is able to escape when the outer layers are expanded and the thermal pressure drops. Gravity takes over and the star shrinks, but it shrinks beyond the equilibrium point. T ...
The universe - Villanova University
... Stuff like iron, nickel, uranium comes from the destruction (explosion) of stars. ...
... Stuff like iron, nickel, uranium comes from the destruction (explosion) of stars. ...
Stellar Evolution: The Live and Death of a Star
... When burning starts and temperature increases, there is no corresponding rise in pressure, no expansion of gas & no stabilization of core The rapid temperature rise results in runaway explosion called the helium flash The helium burns ferociously for a few hours, then equilibrium is eventually re ...
... When burning starts and temperature increases, there is no corresponding rise in pressure, no expansion of gas & no stabilization of core The rapid temperature rise results in runaway explosion called the helium flash The helium burns ferociously for a few hours, then equilibrium is eventually re ...
Chapter 18 Life in the Universe
... Most planetary systems like our own have not been detected yet, but we would expect to be able to detect them using current methods. ...
... Most planetary systems like our own have not been detected yet, but we would expect to be able to detect them using current methods. ...
spiral nebulae
... across. The path followed by an object travelling around and around the centre must be tens or hundreds of thousands of light years in length.` To give rise to the ‘observed’ rotational motions, over a period of just a decade or two, the stars within them would need to be moving very much faster tha ...
... across. The path followed by an object travelling around and around the centre must be tens or hundreds of thousands of light years in length.` To give rise to the ‘observed’ rotational motions, over a period of just a decade or two, the stars within them would need to be moving very much faster tha ...
universe_pp_4 - Cobb Learning
... universe were moving away from us…which would mean at one time they were all together at one point •The Hubble Telescope was named in his honor ...
... universe were moving away from us…which would mean at one time they were all together at one point •The Hubble Telescope was named in his honor ...
A SOLAR SYSTEM IS BORN
... temperature increases and stars begin to form. • This is a solar nebula. • Our sun formed like this. ...
... temperature increases and stars begin to form. • This is a solar nebula. • Our sun formed like this. ...
The Birth of Stars
... The nearest great stellar nursery to us is the great Orion molecular cloud which is about 1000 light years away, and manufacturing thousands of stars. This is probably how the typical star is made. ...
... The nearest great stellar nursery to us is the great Orion molecular cloud which is about 1000 light years away, and manufacturing thousands of stars. This is probably how the typical star is made. ...
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.