The Origin of the Elements edited by David L. Alles Western Washington University
... The fuel which supplies the heat is hydrogen. Hydrogen nuclei are converted to helium as heat is released. Five billion years from now the Sun's hydrogen fuel will be depleted. Gravity will then force the spent core, now almost pure helium, to shrink, compress, and become even hotter than at present ...
... The fuel which supplies the heat is hydrogen. Hydrogen nuclei are converted to helium as heat is released. Five billion years from now the Sun's hydrogen fuel will be depleted. Gravity will then force the spent core, now almost pure helium, to shrink, compress, and become even hotter than at present ...
The Formation of the Solar System
... • Angular Momentum and Gravity are clearly understood • Nebula are very real and very common – We can see stars in different phases of development when we observe nebular through a telescope. ...
... • Angular Momentum and Gravity are clearly understood • Nebula are very real and very common – We can see stars in different phases of development when we observe nebular through a telescope. ...
CoRoT: a space project to listen to the songs of the stars
... Payload mass of CoRoT will be about 300 kg and will orbit at an altitude of 896 km (Courtesy of http://corot.oamp.fr/) Stars are balls of gas in equilibrium under the action of gravity. Many stars can vibrate in different modes like a musical instrument. For example, vibrations detected on the surfa ...
... Payload mass of CoRoT will be about 300 kg and will orbit at an altitude of 896 km (Courtesy of http://corot.oamp.fr/) Stars are balls of gas in equilibrium under the action of gravity. Many stars can vibrate in different modes like a musical instrument. For example, vibrations detected on the surfa ...
T3-W10-0501student
... size of the star also determines what path it will take as it goes through its cycle. ...
... size of the star also determines what path it will take as it goes through its cycle. ...
![[OIII ] Electron Temperatures in Planetary Nebulae](http://s1.studyres.com/store/data/022822830_1-24f8fad33a75c04fa6e3c895c876b204-300x300.png)
[OIII ] Electron Temperatures in Planetary Nebulae
... 3. Results and discussion Many authors have determined the R ratios in planetary nebulae (see, for example, Aller & Keyes 1987), although there are relatively few for which electron temperatures have been independently estimated from a number of Te-sensitive ratios in other species. In Table 1 we su ...
... 3. Results and discussion Many authors have determined the R ratios in planetary nebulae (see, for example, Aller & Keyes 1987), although there are relatively few for which electron temperatures have been independently estimated from a number of Te-sensitive ratios in other species. In Table 1 we su ...
The Interstellar Medium (ISM) The Dust The Gas: a. The Hot
... A general view of the nighttime sky and of the Milky Way: Stars and Nebulae The presence of an interstellar medium Dust Gas Cool Hot General properties: Average temperature about 100K and densities about 1–10 atoms/cm3 , typically atomic Hydrogen (HI) and about 1000 dust particles per cubic kilomete ...
... A general view of the nighttime sky and of the Milky Way: Stars and Nebulae The presence of an interstellar medium Dust Gas Cool Hot General properties: Average temperature about 100K and densities about 1–10 atoms/cm3 , typically atomic Hydrogen (HI) and about 1000 dust particles per cubic kilomete ...
sept2302
... HST and planetary transits HD 209458 – discovered by Keck/Geneva RV teams - transit detected by Charbonneau et al (2000) using ground-based photometry ...
... HST and planetary transits HD 209458 – discovered by Keck/Geneva RV teams - transit detected by Charbonneau et al (2000) using ground-based photometry ...
Milky Way Galaxy
... A star is a big ball of gas which gives off both heat and light. So where do stars come from? What happens to them as they grow older? A galaxy contains clouds of dust and gas, as well as stars. It is in the clouds of dust and gas that stars are born. As more and more of the gas (which is mostly hyd ...
... A star is a big ball of gas which gives off both heat and light. So where do stars come from? What happens to them as they grow older? A galaxy contains clouds of dust and gas, as well as stars. It is in the clouds of dust and gas that stars are born. As more and more of the gas (which is mostly hyd ...
PHYS2160 Notes 4
... – Planetary nebulae : compact regions with higher gas densities excited by the UV flux from a very hot white dwarf. Gas in these higher density regions is excited by collisions between electrons, ions and atoms, resulting in substantially different spectra from HII regions. The shells of gas illumi ...
... – Planetary nebulae : compact regions with higher gas densities excited by the UV flux from a very hot white dwarf. Gas in these higher density regions is excited by collisions between electrons, ions and atoms, resulting in substantially different spectra from HII regions. The shells of gas illumi ...
Stars: Part 2
... • This red giant begins to lose some of its layers. • Eventually it enters the Cepheid stage. • This is the final phase of the star's life. • It then becomes a white dwarf. • In a white dwarf, the core of the star is left, some fires still burn, but there is very little fuel left. ...
... • This red giant begins to lose some of its layers. • Eventually it enters the Cepheid stage. • This is the final phase of the star's life. • It then becomes a white dwarf. • In a white dwarf, the core of the star is left, some fires still burn, but there is very little fuel left. ...
the spectrum of a partially ionized jet sodium ionization in t
... We present the results of a study of the sodium ionization and excitation in the winds of low-luminosity, pre-main-sequence stars. Line profiles for the Nal doublet at 5990,5986 Aare discussed and compared with the observations for those T Tauri stars with P-Cygni profiles. We find that the observed ...
... We present the results of a study of the sodium ionization and excitation in the winds of low-luminosity, pre-main-sequence stars. Line profiles for the Nal doublet at 5990,5986 Aare discussed and compared with the observations for those T Tauri stars with P-Cygni profiles. We find that the observed ...
potters powerpoint
... Why do stars shine ? • Stars shine because of the heat they make. The heat of a star reaches about 16million degrees Celsius. A grain of sand that hot could kill someone 150km away. ...
... Why do stars shine ? • Stars shine because of the heat they make. The heat of a star reaches about 16million degrees Celsius. A grain of sand that hot could kill someone 150km away. ...
The Life Cycle of a Star
... Because of the expansion, the outer layers are much cooler than when the star was in the main sequence. It therefore appears as a red giant. Our Sun is considered an intermediate mass star and will evolve to this phase in about 5 billion years, its diameter expanding beyond what is now the size ...
... Because of the expansion, the outer layers are much cooler than when the star was in the main sequence. It therefore appears as a red giant. Our Sun is considered an intermediate mass star and will evolve to this phase in about 5 billion years, its diameter expanding beyond what is now the size ...
(the factor f star in the Drake equation. Recall it
... electrically charge neutral atoms of helium and hydrogen as well as electromagnetic radiation. ...
... electrically charge neutral atoms of helium and hydrogen as well as electromagnetic radiation. ...
File
... point of zero-age main sequence stars Larger, hotter main sequence stars, operating at higher core temperatures, can fuse hydrogen via the CNO cycle where carbon, nitrogen and oxygen act as catalysts in the reaction steps to produce helium. Process is cyclical Red-Giants (Post-main sequence) fuse he ...
... point of zero-age main sequence stars Larger, hotter main sequence stars, operating at higher core temperatures, can fuse hydrogen via the CNO cycle where carbon, nitrogen and oxygen act as catalysts in the reaction steps to produce helium. Process is cyclical Red-Giants (Post-main sequence) fuse he ...
jan0605
... 7. Continued accretion of small satellite galaxies as Milky Way builds its outer halo Total mass ~ few x 1011 solar masses: <1% halo+bulge; 10% disk; ~90% dark matter ...
... 7. Continued accretion of small satellite galaxies as Milky Way builds its outer halo Total mass ~ few x 1011 solar masses: <1% halo+bulge; 10% disk; ~90% dark matter ...
I have heard people call Jupiter a "failed star" that just did not get big
... Stars form directly from the collapse of dense clouds of interstellar gas and dust. Because of rotation, these clouds form flattened disks that surround the central, growing stars. After the star has nearly reached its final mass, by accreting gas from the disk, the leftover matter in the disk is fr ...
... Stars form directly from the collapse of dense clouds of interstellar gas and dust. Because of rotation, these clouds form flattened disks that surround the central, growing stars. After the star has nearly reached its final mass, by accreting gas from the disk, the leftover matter in the disk is fr ...
Astronomy The Night Sky. Vocabulary Terms to know for the
... 1. Most ___________________ is in the form of stars or star dust. (You and I are star dust!!) 2. On the ________________________, stars are classified according to their _______________________________ and ____________________ (how bright the star REALLY is). See page 15 of ESRT. 3. All stars begin ...
... 1. Most ___________________ is in the form of stars or star dust. (You and I are star dust!!) 2. On the ________________________, stars are classified according to their _______________________________ and ____________________ (how bright the star REALLY is). See page 15 of ESRT. 3. All stars begin ...
Document
... • Kant figured it out (1754) • Herschel (William) and his son John, both lords, tried to prove Kant right (1785, 1850) • 1850, Sir John admitted that his father’s great quest had failed. • By 1900, virtually all astronomers agreed that the extent of the Universe was the edge of the Milky Way (~100 k ...
... • Kant figured it out (1754) • Herschel (William) and his son John, both lords, tried to prove Kant right (1785, 1850) • 1850, Sir John admitted that his father’s great quest had failed. • By 1900, virtually all astronomers agreed that the extent of the Universe was the edge of the Milky Way (~100 k ...
Astrobiology 101
... 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. ...
OVERVIEW ABSTRACT HST/COS chemical abundance analysis of
... We present new Near-UltraViolet (NUV) elemental abundance analysis, for the hyper metal-poor star HE1327-2326 ([Fe/H] = -5.2) using COS/HST data. We detect for the first time 4 Fe II lines, in addition to Zn I and Ni II absorption lines. Fitting the abundances to SNe yield models, lead to Pop III pr ...
... We present new Near-UltraViolet (NUV) elemental abundance analysis, for the hyper metal-poor star HE1327-2326 ([Fe/H] = -5.2) using COS/HST data. We detect for the first time 4 Fe II lines, in addition to Zn I and Ni II absorption lines. Fitting the abundances to SNe yield models, lead to Pop III pr ...
The life cycle of stars
... Lecture Tutorial: Using “Astronomy Picture of the Day” to learn about the life cycle of stars For this exercise, you will need an ipad or computer and access to the internet. We will be using the website “Astronomy Picture of the Day” (APOD, for short) to learn more about the life cycle of stars. 1. ...
... Lecture Tutorial: Using “Astronomy Picture of the Day” to learn about the life cycle of stars For this exercise, you will need an ipad or computer and access to the internet. We will be using the website “Astronomy Picture of the Day” (APOD, for short) to learn more about the life cycle of stars. 1. ...
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.