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Detection of Planetary Transits Across a Sun
... Cameron et al. (1999) will be dicult, because of the relative faintness of this star. If successful, however, they would yield the planet's albedo directly, since its radius is accurately known. In particular, the ratio of the ux from the planet at opposition to that of the star is 1:7 10;4 p ...
... Cameron et al. (1999) will be dicult, because of the relative faintness of this star. If successful, however, they would yield the planet's albedo directly, since its radius is accurately known. In particular, the ratio of the ux from the planet at opposition to that of the star is 1:7 10;4 p ...
... — planetary nebulae: general — stars: AGB and post-AGB — stars: white dwarfs 1. INTRODUCTION 2014 was an important year for the study of planetary nebulae. The first planetary nebula (PN) was discovered on 12 July, 1764 when Charles Messier stumbled across the Dumbbell Nebula, M27, making 2014 their ...
Review (PPT) - Uplift Summit Intl
... ▪ Star collapses when most of the hydrogen nuclei have fused into helium. ▪ Gravity now outweighs the radiation pressure and the star shrinks in size and heats up. ▪ The hydrogen in the layer surrounding the shrunken core is now able to fuse, raising the temperature of the outer layers which makes t ...
... ▪ Star collapses when most of the hydrogen nuclei have fused into helium. ▪ Gravity now outweighs the radiation pressure and the star shrinks in size and heats up. ▪ The hydrogen in the layer surrounding the shrunken core is now able to fuse, raising the temperature of the outer layers which makes t ...
L and T Dwarfs - Indiana University
... radiation trapped by extra dust-grain opacity • Heating dissociates H2O, giving weaker water bands • Dust settles gravitationally, depleting metals and leaving ...
... radiation trapped by extra dust-grain opacity • Heating dissociates H2O, giving weaker water bands • Dust settles gravitationally, depleting metals and leaving ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv •
... by an immense galaxy collision. When galaxies collide, they pass through each other -- their individual stars rarely come into contact. The ring-like shape is the result of the gravitational disruption caused by an entire small intruder galaxy passing through a large one. When this happens, interste ...
... by an immense galaxy collision. When galaxies collide, they pass through each other -- their individual stars rarely come into contact. The ring-like shape is the result of the gravitational disruption caused by an entire small intruder galaxy passing through a large one. When this happens, interste ...
CoRoT Observations of O Stars: Diverse Origins of Variability
... At the moment we can only speculate about the possible causes of this red noise in O-type stars. One possibility is that it is caused by the sub-surface convection zone found in theoretical modeling (Cantiello et al. 2009). This zone is assumed to be responsible for a number of surface effects, such ...
... At the moment we can only speculate about the possible causes of this red noise in O-type stars. One possibility is that it is caused by the sub-surface convection zone found in theoretical modeling (Cantiello et al. 2009). This zone is assumed to be responsible for a number of surface effects, such ...
The Milky Way Galaxy
... Since the stars in the Large Magellanic Cloud are all at approximately the same distance from us, a relationship between their apparent magnitudes and periods implied a relationship between their intrinsic luminosities (i.e. absolute magnitudes) and periods. Harlow Shapley (1885-1972) noticed that ...
... Since the stars in the Large Magellanic Cloud are all at approximately the same distance from us, a relationship between their apparent magnitudes and periods implied a relationship between their intrinsic luminosities (i.e. absolute magnitudes) and periods. Harlow Shapley (1885-1972) noticed that ...
Document
... where gas pressure balances gravity. • Sometimes, an external disturbance can cause parts of the cloud to move closer together. In this case, the gravitational force may be stronger than the pressure ...
... where gas pressure balances gravity. • Sometimes, an external disturbance can cause parts of the cloud to move closer together. In this case, the gravitational force may be stronger than the pressure ...
Kepler-539: a young extrasolar system with two giant planets on
... orbiting a solar-analogue G2 V star. The mass of Kepler-539 b was accurately derived thanks to a series of precise radial velocity measurements obtained with the CAFE spectrograph mounted on the CAHA 2.2-m telescope. A simultaneous fit of the radial-velocity data and Kepler photometry revealed that ...
... orbiting a solar-analogue G2 V star. The mass of Kepler-539 b was accurately derived thanks to a series of precise radial velocity measurements obtained with the CAFE spectrograph mounted on the CAHA 2.2-m telescope. A simultaneous fit of the radial-velocity data and Kepler photometry revealed that ...
No Slide Title
... with the Sagittarius A* radio source, surrounded by a torus (R=7 pc) of molecular gas, which flows in at a rate of 0.001-0.01 Msun/yr and formed dozens of massive stars within the last 3-7 Myr. Nucleus (right panel, showing gas) is much smaller than the black dot in the background picture. A fairly ...
... with the Sagittarius A* radio source, surrounded by a torus (R=7 pc) of molecular gas, which flows in at a rate of 0.001-0.01 Msun/yr and formed dozens of massive stars within the last 3-7 Myr. Nucleus (right panel, showing gas) is much smaller than the black dot in the background picture. A fairly ...
Lecture 13 Hydrogen Burning on the Main Sequence and Homology
... than linearly with M on the main sequence and it doesn’t) 2. That the actual radius of the star will depend on the form of the energy generation. Until nuclear energy generation is specified, R is undetermined, though L may be. 3. Stars will get hotter in their centers when they use up a given fue ...
... than linearly with M on the main sequence and it doesn’t) 2. That the actual radius of the star will depend on the form of the energy generation. Until nuclear energy generation is specified, R is undetermined, though L may be. 3. Stars will get hotter in their centers when they use up a given fue ...
Star formation Stars form out of dense, cold, often dusty, molecular
... …on large scales, down to: Molecular cloud cores M ~ few Solar masses R ~ 0.1 pc one or a few stars ASTR 3730: Fall 2003 ...
... …on large scales, down to: Molecular cloud cores M ~ few Solar masses R ~ 0.1 pc one or a few stars ASTR 3730: Fall 2003 ...
JP 2.1: Geodetic Planetology (JP-GP)
... SELENE/Kaguya, Lunar Reconnaissance Orbiter), Mars (Mars Global Surveyor, Mars Odyssey, Mars Reconnaissance Orbiter), Venus (Magellan), and Mercury (Messenger) revealed increasingly detailed structures of the gravity field, shape, surface and atmosphere of these celestial bodies. Forthcoming mission ...
... SELENE/Kaguya, Lunar Reconnaissance Orbiter), Mars (Mars Global Surveyor, Mars Odyssey, Mars Reconnaissance Orbiter), Venus (Magellan), and Mercury (Messenger) revealed increasingly detailed structures of the gravity field, shape, surface and atmosphere of these celestial bodies. Forthcoming mission ...
21. The Milky Way Galaxy
... Also, squeezing of clouds initiates collapse within them => star formation. Bright young massive stars live and die in spiral arms. Emission nebulae mostly in spiral arms. So arms always contain same types of objects, but individual objects come and go. ...
... Also, squeezing of clouds initiates collapse within them => star formation. Bright young massive stars live and die in spiral arms. Emission nebulae mostly in spiral arms. So arms always contain same types of objects, but individual objects come and go. ...
Lesson Plan: Supernova`s
... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
poll_questions
... • The mass is lost when two protons are converted to two neutrons • It takes energy to pull a helium nucleus apart • Helium atoms move so fast that they have a lower apparent mass ...
... • The mass is lost when two protons are converted to two neutrons • It takes energy to pull a helium nucleus apart • Helium atoms move so fast that they have a lower apparent mass ...
ppt - CIERA-Northwestern
... We study the evolution of binary stars in globular clusters using a new Monte Carlo approach combining a population synthesis code (STARTRACK) and a simple treatment of dynamical interactions in the dense cluster core using a new tool for computing three- and four-body interactions (FEWBODY). We fin ...
... We study the evolution of binary stars in globular clusters using a new Monte Carlo approach combining a population synthesis code (STARTRACK) and a simple treatment of dynamical interactions in the dense cluster core using a new tool for computing three- and four-body interactions (FEWBODY). We fin ...
Stellar Evolution
... surface. By the time you get to stars that have masses similar to that of the Sun, the mass fraction that is involved in convection is a very small part of the star at the surface (as is shown in the graph). As you go to higher masses, convection is seen in the cores of many stars, and the fraction ...
... surface. By the time you get to stars that have masses similar to that of the Sun, the mass fraction that is involved in convection is a very small part of the star at the surface (as is shown in the graph). As you go to higher masses, convection is seen in the cores of many stars, and the fraction ...
The Most Massive LMC Star Sk
... and bluest of the three components, The members of the cluster probably R 136 a, might be a star of mass formed together. The fainter components (c-f) are probably early-type 0 250-1,000 MG' Cassinelli et al. (1981) stars, as the formation of low mass stars from the IUE data concluded that R 136 a i ...
... and bluest of the three components, The members of the cluster probably R 136 a, might be a star of mass formed together. The fainter components (c-f) are probably early-type 0 250-1,000 MG' Cassinelli et al. (1981) stars, as the formation of low mass stars from the IUE data concluded that R 136 a i ...
astronomy - Scioly.org
... -At a density of around 10-13 grams per cubic centimeter, the center of the cloud becomes optically opaque. When collapse is essentially halted, a core region called the First Hydrostatic Core forms. Meanwhile, gas falling inwards collides with this region, creating more heat to heat the core via sh ...
... -At a density of around 10-13 grams per cubic centimeter, the center of the cloud becomes optically opaque. When collapse is essentially halted, a core region called the First Hydrostatic Core forms. Meanwhile, gas falling inwards collides with this region, creating more heat to heat the core via sh ...
Spectroscopy - Mr. Borchik
... • Spectroscopy- the study of the light from an object. • Spectrometer- an instrument which spreads out light making a spectra. • Spectra- range of electromagnetic energy separated by wavelength. ...
... • Spectroscopy- the study of the light from an object. • Spectrometer- an instrument which spreads out light making a spectra. • Spectra- range of electromagnetic energy separated by wavelength. ...
The Spectra of Stars
... The Spectral Sequence is a Temperature Sequence • Gross differences among the spectral types are due to differences in Temperature are due to differences in Temperature. • Composition differences are minor at best. – Demonstrated by Cecilia Payne‐Gaposhkin in 1920’s ...
... The Spectral Sequence is a Temperature Sequence • Gross differences among the spectral types are due to differences in Temperature are due to differences in Temperature. • Composition differences are minor at best. – Demonstrated by Cecilia Payne‐Gaposhkin in 1920’s ...
Testing - Elon University
... The older the star, the more negative the value of [Fe/H]. The younger the star, the more positive the value of [Fe/H]. ...
... The older the star, the more negative the value of [Fe/H]. The younger the star, the more positive the value of [Fe/H]. ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
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.