![Rotational spin-up in the 30-Myr](http://s1.studyres.com/store/data/022881932_1-afeb6ba8aafeb5a6953d6da1e8b3dbed-300x300.png)
Rotational spin-up in the 30-Myr
... driver for magnetic activity, from X-ray luminosity to UV flux and surface spots, that is the ultimate source of stellar winds. Studying the initial angular momentum content of stars and its evolution throughout the star’s lifetime brings unique clues to the star formation process, to the accretion/ ...
... driver for magnetic activity, from X-ray luminosity to UV flux and surface spots, that is the ultimate source of stellar winds. Studying the initial angular momentum content of stars and its evolution throughout the star’s lifetime brings unique clues to the star formation process, to the accretion/ ...
WIRO: Spectral Analysis P1
... curve. Photons from star core heat up gas in star’s atmosphere. Electrons in the gas increase energy levels, but eventually decrease energy levels, which in essence changes the direction of the photons from the core. So what we are able to “view” is absorption of photon energy, whereas in reality th ...
... curve. Photons from star core heat up gas in star’s atmosphere. Electrons in the gas increase energy levels, but eventually decrease energy levels, which in essence changes the direction of the photons from the core. So what we are able to “view” is absorption of photon energy, whereas in reality th ...
Spatial Structure Evolution of Star Clusters
... - Full data release expected end of 2002 - Deep IR images to differentiate the MS (IR camera with Nagoya U & PMO) • Stars in an open cluster, regardless of masses, are concentrated progressively toward the center. • The youngest star clusters show evidence of luminosity (mass) segregation - cf. mole ...
... - Full data release expected end of 2002 - Deep IR images to differentiate the MS (IR camera with Nagoya U & PMO) • Stars in an open cluster, regardless of masses, are concentrated progressively toward the center. • The youngest star clusters show evidence of luminosity (mass) segregation - cf. mole ...
The Mass of the Galaxy - University of California, Berkeley
... light of the Galaxy (corrected for interstellar absorption). This comes out substantially lower. There must be some “dark matter”. ...
... light of the Galaxy (corrected for interstellar absorption). This comes out substantially lower. There must be some “dark matter”. ...
Slide 1
... Superbubbles, and the Source of Cosmic Rays” 2005, ApJ, 268, 738 Ikeuchi, S. “Evolution of Evolution of Superbubbles” 1998, LNP, 506, 399 Mac Low, M.M. & McCray, R. “Superbubbles in disk galaxies”, 1988, ApJ, 324, 776 Maiz-Apellaniz, J. “The Origin of the Local Bubble” 2001, ApJ, 560, L86 Oey, M.S. ...
... Superbubbles, and the Source of Cosmic Rays” 2005, ApJ, 268, 738 Ikeuchi, S. “Evolution of Evolution of Superbubbles” 1998, LNP, 506, 399 Mac Low, M.M. & McCray, R. “Superbubbles in disk galaxies”, 1988, ApJ, 324, 776 Maiz-Apellaniz, J. “The Origin of the Local Bubble” 2001, ApJ, 560, L86 Oey, M.S. ...
distances
... • A star’s spectrum typically depicts the energy it emits at each wavelength • A spectrum also can reveal a star’s composition, temperature, luminosity, velocity in space, rotation speed, and it may reveal mass and radius ...
... • A star’s spectrum typically depicts the energy it emits at each wavelength • A spectrum also can reveal a star’s composition, temperature, luminosity, velocity in space, rotation speed, and it may reveal mass and radius ...
Astronomical Observations with the Voyager Spacecraft
... • Atmospheric scale height, temperature – Stellar Occultation's ...
... • Atmospheric scale height, temperature – Stellar Occultation's ...
Nature template
... mark where the nuclearly processed material reaches the surface – filled circles belong to the twice solar metalicity tracks and open to the solar metalicity tracks. The ends of the tracks designate where the outer atmosphere becomes unbound by gravity against radiation pressure. In general, these t ...
... mark where the nuclearly processed material reaches the surface – filled circles belong to the twice solar metalicity tracks and open to the solar metalicity tracks. The ends of the tracks designate where the outer atmosphere becomes unbound by gravity against radiation pressure. In general, these t ...
Characteristics of Stars PLATO
... Milky Way Galaxy Our Solar System is located in the far reaches of a spiral galaxy that we call the Milky Way Galaxy. Almost all of the stars that we see in the night sky are also members of the Milky Way Galaxy. The Milky Way Galaxy contains roughly 200 billion stars, one of which is our Sun. ...
... Milky Way Galaxy Our Solar System is located in the far reaches of a spiral galaxy that we call the Milky Way Galaxy. Almost all of the stars that we see in the night sky are also members of the Milky Way Galaxy. The Milky Way Galaxy contains roughly 200 billion stars, one of which is our Sun. ...
Stars and The Universe
... If the material remaining in the core is greater than 3 solar masses, its gravitational force is strong enough to cause the collapse of neutrons. The mass compresses itself into an infinitely small point whose gravity is so intense that not even light can escape from it. ...
... If the material remaining in the core is greater than 3 solar masses, its gravitational force is strong enough to cause the collapse of neutrons. The mass compresses itself into an infinitely small point whose gravity is so intense that not even light can escape from it. ...
CoRoT-2a magnetic activity: hints for possible star
... nature of SPI appears to be strongly affected by both the stellar and planetary magnetic fields. Shkolnik et al. (2009) and Schmitt (2009) show that for extrasolar planets around young stars conditions similar to those observed for the Jupiter-Io system are met and consequently similar processes ar ...
... nature of SPI appears to be strongly affected by both the stellar and planetary magnetic fields. Shkolnik et al. (2009) and Schmitt (2009) show that for extrasolar planets around young stars conditions similar to those observed for the Jupiter-Io system are met and consequently similar processes ar ...
The Habitable Zone Gallery
... The philosophy of the HZG design is accuracy and sustainability such that it can continue to provide useful results which keep pace with the current rate of exoplanet detection. The optimal path to reach this goal is to avoid data entry which dramatically increases maintenance and the introduction o ...
... The philosophy of the HZG design is accuracy and sustainability such that it can continue to provide useful results which keep pace with the current rate of exoplanet detection. The optimal path to reach this goal is to avoid data entry which dramatically increases maintenance and the introduction o ...
BAS - Monthly Sky Guide
... A couple of constellations in the sky along the meridian at about 9 PM during the New Moon period are the constellations Ara and Ophiuchus. Ara is a small constellation in the southern sky located near the curly tail of Scorpius. It is not always easy to identify but it does have a bent rectangle s ...
... A couple of constellations in the sky along the meridian at about 9 PM during the New Moon period are the constellations Ara and Ophiuchus. Ara is a small constellation in the southern sky located near the curly tail of Scorpius. It is not always easy to identify but it does have a bent rectangle s ...
STUDY GUIDE FOR CHAPTER 1
... 3. The main sequence is where most of the stars are. a. What does it look like? b. For stars on the main sequence only, what is the relationship between mass and luminosity? C. Spectroscopic parallax 1. This is not given in the book. 2. By measuring the spectral type and luminosity class of a star y ...
... 3. The main sequence is where most of the stars are. a. What does it look like? b. For stars on the main sequence only, what is the relationship between mass and luminosity? C. Spectroscopic parallax 1. This is not given in the book. 2. By measuring the spectral type and luminosity class of a star y ...
Balloon Model of the Life Cycle of Stars
... shine orange, even larger ones are hotter and shine yellow, and the largest and hottest ones shine blue. Eventually the star fuses all of its hydrogen. The hot blue stars do this first, in some millions of years. Yellow and orange stars take billions of years, and the universe is not yet old enough ...
... shine orange, even larger ones are hotter and shine yellow, and the largest and hottest ones shine blue. Eventually the star fuses all of its hydrogen. The hot blue stars do this first, in some millions of years. Yellow and orange stars take billions of years, and the universe is not yet old enough ...
Targets for Small Telescopes
... The primary itself was found to be a close binary pair in 1977 using speckle interferometry. It has a separation of .39” and the magnitude difference is 1.5. It was observed visually in 1979 by C. E. Worley using a 26” refractor. The pair should be observable in amateur telescopes over 25” aperture, ...
... The primary itself was found to be a close binary pair in 1977 using speckle interferometry. It has a separation of .39” and the magnitude difference is 1.5. It was observed visually in 1979 by C. E. Worley using a 26” refractor. The pair should be observable in amateur telescopes over 25” aperture, ...
NEBULAR HYPOTHESIS OF LAPLACE
... Laplace maintained that there was a hot an rotating huge gaseous nebula in the space. There was gradual loss of heat from the outer surface of the nebula through radiation due to circular motion or rotation of the nebula. Thus, gradual loss of heat resulted into the cooling of the outer surface of ...
... Laplace maintained that there was a hot an rotating huge gaseous nebula in the space. There was gradual loss of heat from the outer surface of the nebula through radiation due to circular motion or rotation of the nebula. Thus, gradual loss of heat resulted into the cooling of the outer surface of ...
ASTR 1020 FINAL EXAM STUDY GUIDE
... 8) Observationally, how can we tell the difference between a white dwarf supernova and a massive-star supernova? 9) How does the gravity of an object affect the light emitted from that object? ...
... 8) Observationally, how can we tell the difference between a white dwarf supernova and a massive-star supernova? 9) How does the gravity of an object affect the light emitted from that object? ...
1. a. Collisionless Boltzmann—particles moving in smooth potential
... Key point is that low velocity interactions are very disruptive and as several pointed out, mergers of disks can lead to E galaxies. c. E and S0 galaxies: the E is on average denser in its central region but as both galaxies have roughly the same number of stars and these are spread over a larger vo ...
... Key point is that low velocity interactions are very disruptive and as several pointed out, mergers of disks can lead to E galaxies. c. E and S0 galaxies: the E is on average denser in its central region but as both galaxies have roughly the same number of stars and these are spread over a larger vo ...
Abundances - Michigan State University
... to best reproduce all spectral features, incl. all absorption lines (can be 100’s or more) . Example for a r-process star (Sneden et al. ApJ 572 (2002) 861) ...
... to best reproduce all spectral features, incl. all absorption lines (can be 100’s or more) . Example for a r-process star (Sneden et al. ApJ 572 (2002) 861) ...
Stars, Galaxies, and the Universe
... Telescopes: Collect and focus different types of electromagnetic radiation including visible light. Convex lens: A piece of transparent glass, curved so that the middle is thicker than the edges. Refracting telescopes: use convex lens to gather a large amount of light and focus it into a small area. ...
... Telescopes: Collect and focus different types of electromagnetic radiation including visible light. Convex lens: A piece of transparent glass, curved so that the middle is thicker than the edges. Refracting telescopes: use convex lens to gather a large amount of light and focus it into a small area. ...
What Is a Star
... billions of years. Our sun was born about 4.6 billion years ago. It is in the middle of its life cycle. It will live for at least another five billion years. ...
... billions of years. Our sun was born about 4.6 billion years ago. It is in the middle of its life cycle. It will live for at least another five billion years. ...
Life Cycle of Stars Powerpoint
... but is the size of Earth, it is one million times as dense as the sun. When a white dwarf runs out of fuel and energy it becomes a black dwarf. • A black dwarf has stopped glowing because fusion has stopped. It is a “dead” star, not the Death Star that is ...
... but is the size of Earth, it is one million times as dense as the sun. When a white dwarf runs out of fuel and energy it becomes a black dwarf. • A black dwarf has stopped glowing because fusion has stopped. It is a “dead” star, not the Death Star that is ...
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.