STIS/HST Observations of Large Magellanic Cloud Planetary
... elliptical. In this size regime the nebulae are well resolved (>11 pixels diameter), so the lack of asymmetric nebulae here could indicate an evolutionary effect, in the sense that any initial asymmetry in the gas distribution and velocity field may not have had time to manifest itself in the morpho ...
... elliptical. In this size regime the nebulae are well resolved (>11 pixels diameter), so the lack of asymmetric nebulae here could indicate an evolutionary effect, in the sense that any initial asymmetry in the gas distribution and velocity field may not have had time to manifest itself in the morpho ...
Binary Star Par 1802 Word Document
... (Translated from Sterne und Weltraum 12/08 by G S Kelly) For many years astronomers have assumed that the stars in binary or multiple systems form at the same time. Now, however, a research team headed by Keivan Stassun at the Vanderbilt University in Tennessee, have come across a binary star system ...
... (Translated from Sterne und Weltraum 12/08 by G S Kelly) For many years astronomers have assumed that the stars in binary or multiple systems form at the same time. Now, however, a research team headed by Keivan Stassun at the Vanderbilt University in Tennessee, have come across a binary star system ...
1. The distances to the most remote galaxies can be
... the disc of gas and dust surrounding a young star that will soon form a solar system. the ejected envelope of a red giant star surrounding a stellar core remnant. a type of young, medium mass star. a planet surrounded by a cool shell of molecular gas. ...
... the disc of gas and dust surrounding a young star that will soon form a solar system. the ejected envelope of a red giant star surrounding a stellar core remnant. a type of young, medium mass star. a planet surrounded by a cool shell of molecular gas. ...
The central star of the planetary nebula PB 8: a Wolf-Rayet
... The typical emission-line spectra of Wolf-Rayet stars are predominantly formed by recombination processes in their dense stellar winds. Therefore the continuum-normalized spectrum shows a useful scale-invariance: for a given stellar temperature T ∗ and chemical composition, the equivalent widths of ...
... The typical emission-line spectra of Wolf-Rayet stars are predominantly formed by recombination processes in their dense stellar winds. Therefore the continuum-normalized spectrum shows a useful scale-invariance: for a given stellar temperature T ∗ and chemical composition, the equivalent widths of ...
The Star–Gas–Star Cycle
... Regions of the Milky Way Galaxy diameter of disk = 100,000 l.y. (30,000 pc) thickness of disk = 1,000 l.y. (300 pc) number of stars = 200 billion ...
... Regions of the Milky Way Galaxy diameter of disk = 100,000 l.y. (30,000 pc) thickness of disk = 1,000 l.y. (300 pc) number of stars = 200 billion ...
Stellar evolution - Chandra X
... about them. X-ray data reveal extreme or violent conditions where gas has been heated to very high temperatures or particles have been accelerated to extremely high energies. These conditions can exist near collapsed objects such as white dwarfs, neutron stars, and black holes; in giant bubbles of h ...
... about them. X-ray data reveal extreme or violent conditions where gas has been heated to very high temperatures or particles have been accelerated to extremely high energies. These conditions can exist near collapsed objects such as white dwarfs, neutron stars, and black holes; in giant bubbles of h ...
As a pure solid, elemental carbon occurs in two distinct chemical forms
... accumulate and interact with the dust particles, forming larger particles. As these particles grow larger, they start producing a gravitational pull that attracts even more particles, creating big clumps of matter. As the cloud is rotating while all this is happening, it collapses inward, going from ...
... accumulate and interact with the dust particles, forming larger particles. As these particles grow larger, they start producing a gravitational pull that attracts even more particles, creating big clumps of matter. As the cloud is rotating while all this is happening, it collapses inward, going from ...
Stellar Evolution
... • What are the evolutionary stages of a one solar mass star? • How does the evolution of a high mass star differ from that of a low mass star? • How can the age of a cluster of stars, all formed at the same time, be determined? • Why does fusion stop at Iron? ...
... • What are the evolutionary stages of a one solar mass star? • How does the evolution of a high mass star differ from that of a low mass star? • How can the age of a cluster of stars, all formed at the same time, be determined? • Why does fusion stop at Iron? ...
The big bang left the universe with its first atoms
... made of super-dense matter. Most of their hydrogen and helium are lost to the stellar wind. These stars are so dense that they form a new type of “degenerate” or nuclear matter. ...
... made of super-dense matter. Most of their hydrogen and helium are lost to the stellar wind. These stars are so dense that they form a new type of “degenerate” or nuclear matter. ...
Where Did All The Elements Come From??
... made of super-dense matter. Most of their hydrogen and helium are lost to the stellar wind. These stars are so dense that they form a new type of “degenerate” or nuclear matter. ...
... made of super-dense matter. Most of their hydrogen and helium are lost to the stellar wind. These stars are so dense that they form a new type of “degenerate” or nuclear matter. ...
Saloni
... of hydrogen and that helium starts imploding further becomes even denser. It nucleus becomes so dense duewith to its and a tail of dust gas.escape Many comets beenhole discovered using powerful telescopes a small percentage of heavy metals. It is have then presence ofathese metals that give the grav ...
... of hydrogen and that helium starts imploding further becomes even denser. It nucleus becomes so dense duewith to its and a tail of dust gas.escape Many comets beenhole discovered using powerful telescopes a small percentage of heavy metals. It is have then presence ofathese metals that give the grav ...
File - Prairie Science
... cosmic "big bang" that began the universe some 10 billion to 20 billion years ago. In the milliseconds following this explosion, clouds of gases began to coalesce, collapse, and compress under gravity to form the building blocks of galaxies. ...
... cosmic "big bang" that began the universe some 10 billion to 20 billion years ago. In the milliseconds following this explosion, clouds of gases began to coalesce, collapse, and compress under gravity to form the building blocks of galaxies. ...
File - Physical Science
... There are billions of solar systems in our galaxy and billions of galaxies in the known universe! ...
... There are billions of solar systems in our galaxy and billions of galaxies in the known universe! ...
Lecture110402
... security number Chapters 1-16 It will concentrate on Chapters 4, 12-16 (about 3/4 of exam) Some questions are directly from the homework and quizzes ...
... security number Chapters 1-16 It will concentrate on Chapters 4, 12-16 (about 3/4 of exam) Some questions are directly from the homework and quizzes ...
ppt - Slides by Prof Christian
... WDs with more than ~ 1.4 solar masses can not exist! Chandrasekhar Limit = 1.4 Msun ...
... WDs with more than ~ 1.4 solar masses can not exist! Chandrasekhar Limit = 1.4 Msun ...
THE ORIGIN AND EVOLUTION OF PLANETARY NEBULAE
... Herschel (1791). However, no further progress was made for another century. Hubble (1922), using data obtained with the Mount Wilson 60- and 100-in. telescopes, found a correlation between the magnitude of the central star and the size of the nebula. He therefore argued that the emission-line spectr ...
... Herschel (1791). However, no further progress was made for another century. Hubble (1922), using data obtained with the Mount Wilson 60- and 100-in. telescopes, found a correlation between the magnitude of the central star and the size of the nebula. He therefore argued that the emission-line spectr ...
The Change in Gravitational Potential Energy of Objects
... subtracting for loss due to the atmosphere causing friction, has a GPE of 9,800 J. For the same height, the GPE for 1kg object dropped on the Sun, (275m/s2 acceleration of free fall) subtracting for loss due to the atmosphere causing friction and other factors, is 275,000 Joules. What this means is ...
... subtracting for loss due to the atmosphere causing friction, has a GPE of 9,800 J. For the same height, the GPE for 1kg object dropped on the Sun, (275m/s2 acceleration of free fall) subtracting for loss due to the atmosphere causing friction and other factors, is 275,000 Joules. What this means is ...
Search for Planetary Candidates within the OGLE Stars
... fusion of hydrogen (>0.075 Msun); Brown dwarf: capable of deuterium burning (0.013
... fusion of hydrogen (>0.075 Msun); Brown dwarf: capable of deuterium burning (0.013
supplemental materials.
... opacity depends on wavelength, temperature, and composition. While the wavelength dependence of hydrogen’s opacity is relatively simple and wellstudied, some atoms, iron for instance, absorb light at millions of discrete wavelengths, many of which are still unknown. In practice, computer models for ...
... opacity depends on wavelength, temperature, and composition. While the wavelength dependence of hydrogen’s opacity is relatively simple and wellstudied, some atoms, iron for instance, absorb light at millions of discrete wavelengths, many of which are still unknown. In practice, computer models for ...
Observing the Universe 3
... 11. What have astronomers observed in distant galaxies that have enabled them to work out the distance of the galaxy from Earth? ...
... 11. What have astronomers observed in distant galaxies that have enabled them to work out the distance of the galaxy from Earth? ...
Stars and Galaxies
... Planetary Nebulae You read that lower-mass stars, such as the Sun, become white dwarfs. When a star becomes a white dwarf, it casts off hydrogen and helium gases in its outer layers. The expanding, cast-off matter of a white dwarf is a planetary nebula. Most of the star’s carbon remains locked in t ...
... Planetary Nebulae You read that lower-mass stars, such as the Sun, become white dwarfs. When a star becomes a white dwarf, it casts off hydrogen and helium gases in its outer layers. The expanding, cast-off matter of a white dwarf is a planetary nebula. Most of the star’s carbon remains locked in t ...
RADIUS (6371 KM) - Department of Earth and Planetary Sciences
... elements into heavier elements by fusion, or "nuclear burning" Hydrogen “burning” = fusion of 4 hydrogen nuclei (protons) into helium nucleus (2 protons + 2 neutrons) Forming helium from hydrogen gives off lots of energy (a natural hydrogen bomb). Nucleosynthesis requires very high temperature*. The ...
... elements into heavier elements by fusion, or "nuclear burning" Hydrogen “burning” = fusion of 4 hydrogen nuclei (protons) into helium nucleus (2 protons + 2 neutrons) Forming helium from hydrogen gives off lots of energy (a natural hydrogen bomb). Nucleosynthesis requires very high temperature*. The ...
Chapter12 (with interactive links)
... in the expanding outer layers, causing the planetary nebula that we can observe. Planetary nebulae do not last forever – eventually the gas disperses. ...
... in the expanding outer layers, causing the planetary nebula that we can observe. Planetary nebulae do not last forever – eventually the gas disperses. ...
Module 3: Exploring Other Stars Assignment 5: Estimating
... These represent what color photographs of the stellar spectra would look like, if we had really sensitive photographic material. But we don’t, and in the digital age, astronomers have found it’s much more accurate to represent the spectrum as a plot of intensity versus wavelength. This is what the a ...
... These represent what color photographs of the stellar spectra would look like, if we had really sensitive photographic material. But we don’t, and in the digital age, astronomers have found it’s much more accurate to represent the spectrum as a plot of intensity versus wavelength. This is what the a ...
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.