![January - WVU Planetarium - West Virginia University](http://s1.studyres.com/store/data/017029032_1-25d7601ea076c1d6068cebe8114d0b06-300x300.png)
January - WVU Planetarium - West Virginia University
... Big Dipper (Ursa Major). This is easy to do as all seven stars of the dipper are nice and bright. Once you have found this constellation, find the two stars in the side of the bowl which we will call “pointer stars ” because they point the way to the North Star. Draw an imaginary line as shown in th ...
... Big Dipper (Ursa Major). This is easy to do as all seven stars of the dipper are nice and bright. Once you have found this constellation, find the two stars in the side of the bowl which we will call “pointer stars ” because they point the way to the North Star. Draw an imaginary line as shown in th ...
Star Composition: Flame Testing Lab S-2
... Background Information: Astronomers analyze the white light from stars, which spread out into the colors of a spectrum. Dark bands appear in the spectrum caused by the absorption of the light by certain chemicals in the stars’ atmospheres. Each chemical has its own pattern of lines like a fingerprin ...
... Background Information: Astronomers analyze the white light from stars, which spread out into the colors of a spectrum. Dark bands appear in the spectrum caused by the absorption of the light by certain chemicals in the stars’ atmospheres. Each chemical has its own pattern of lines like a fingerprin ...
Stellar Structure, Polytropes, Standard Stellar Model
... This could apply to a proto-neutron star with relativistic electron gas up to ρt, and relatively stiff matter beyond. The ...
... This could apply to a proto-neutron star with relativistic electron gas up to ρt, and relatively stiff matter beyond. The ...
The Death of Massive Stars
... What happens after all the H is used up in the core? • Very Low-mass stars (0.4 Msun or less): Star cease fusing material in the core after all the Hydrogen is used up • Low-mass stars: Hydrogen shell burning, eventually leads to Helium flash in core, planetary nebula phase, leaving a carbon-oxygen ...
... What happens after all the H is used up in the core? • Very Low-mass stars (0.4 Msun or less): Star cease fusing material in the core after all the Hydrogen is used up • Low-mass stars: Hydrogen shell burning, eventually leads to Helium flash in core, planetary nebula phase, leaving a carbon-oxygen ...
PART II: Life of a Star
... • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be different at Z=0 (spectrographic observations of metal-poor stars can tell us a lot about the mass distribution of Pop III) • Ancient Supernovae Yields: MP stars ...
... • Big Bang Nucleosynthesis (eg. 7Li in Halo stars) • The nature of Population III, the First Stars •The First Mass Function, thought to be different at Z=0 (spectrographic observations of metal-poor stars can tell us a lot about the mass distribution of Pop III) • Ancient Supernovae Yields: MP stars ...
proposed research projects for pparc gemini studentships
... formation of S0 galaxies, and their dependency on galaxy mass. To this end, we propose a spectral study of a large sample of lenticular systems to establish the links between the properties of their stellar populations (ages and chemical abundances) and their kinematic properties (masses and dynamic ...
... formation of S0 galaxies, and their dependency on galaxy mass. To this end, we propose a spectral study of a large sample of lenticular systems to establish the links between the properties of their stellar populations (ages and chemical abundances) and their kinematic properties (masses and dynamic ...
1 - Università degli Studi dell`Insubria
... MBH assemby follow the galaxy evolution starting from seed BHs with mass ~100M⊙ forming in minihalos at z~20 ...
... MBH assemby follow the galaxy evolution starting from seed BHs with mass ~100M⊙ forming in minihalos at z~20 ...
Goal: To understand how stars form.
... • It generates its energy from gravitational collapse and not from nuclear fusion like an adult star. • Eventually, the pressure and density at the core of this protostar increase. This increases the collisions of particles at its core. • This causes the core to heat up quickly. ...
... • It generates its energy from gravitational collapse and not from nuclear fusion like an adult star. • Eventually, the pressure and density at the core of this protostar increase. This increases the collisions of particles at its core. • This causes the core to heat up quickly. ...
Part 1, Some Basics
... • The masses can be computed from measurements of the orbital period and orbital size of the system • The mass ratio of M1 and M2 is inversely proportional to the distance of stars to the center of mass ...
... • The masses can be computed from measurements of the orbital period and orbital size of the system • The mass ratio of M1 and M2 is inversely proportional to the distance of stars to the center of mass ...
Future Directions for Astronomy at MSU The lab The rest
... pressure • P- relation is unknown • Results usually shown assuming P = - energy density ...
... pressure • P- relation is unknown • Results usually shown assuming P = - energy density ...
What is np?
... 4.! Minimum mass of star For low-mass stars, any life bearing planet would have to be closer to the star– and closer to stellar effects (e.g. tidal locking and more flares from low mass stars). That limits us to a minimum of 0.5 solar masses. 25% of all stars are more massive than that. ...
... 4.! Minimum mass of star For low-mass stars, any life bearing planet would have to be closer to the star– and closer to stellar effects (e.g. tidal locking and more flares from low mass stars). That limits us to a minimum of 0.5 solar masses. 25% of all stars are more massive than that. ...
Spectral-Type Trends: Absorption
... the Chandra archive, arranged in order of decreasing surface temperature and mass-loss rate. As is evident from the data, the more luminous stars have stronger emission at short wavelengths. One possible explanation for this trend is that we are seeing the effects of absorption on the spectra. Since ...
... the Chandra archive, arranged in order of decreasing surface temperature and mass-loss rate. As is evident from the data, the more luminous stars have stronger emission at short wavelengths. One possible explanation for this trend is that we are seeing the effects of absorption on the spectra. Since ...
Slide 1
... The mass of the first planet is > 5 mass of Jupiter, the orbital period is 430 days, the closest distance between the planet and the host star can be as small as 1.3 astronomical units or 13 radiuses of the host star. The possibility of accretion is higher in planetary system. The relative underabun ...
... The mass of the first planet is > 5 mass of Jupiter, the orbital period is 430 days, the closest distance between the planet and the host star can be as small as 1.3 astronomical units or 13 radiuses of the host star. The possibility of accretion is higher in planetary system. The relative underabun ...
Pre-Main Sequence Evolution
... go into heating the gas, but disassociating the hydrogen. This means that the specific heat of the protostar is γ < 4/3, and, through the virial theorem, the star must collapse on a dynamical timescale. This collapse releases energy, which goes into further H2 disassociation (rather than heating the ...
... go into heating the gas, but disassociating the hydrogen. This means that the specific heat of the protostar is γ < 4/3, and, through the virial theorem, the star must collapse on a dynamical timescale. This collapse releases energy, which goes into further H2 disassociation (rather than heating the ...
type II supernova
... neutrinos, whereas only 1% is converted into the kinetic and heat energy of the ejecta (i.e., outer gas layers). Yet enough light is emitted by a supernova to make it as bright as a billion Suns. The most famous historical Type II SN became visible on July 4, 1054 and was noted by astronomers in Imp ...
... neutrinos, whereas only 1% is converted into the kinetic and heat energy of the ejecta (i.e., outer gas layers). Yet enough light is emitted by a supernova to make it as bright as a billion Suns. The most famous historical Type II SN became visible on July 4, 1054 and was noted by astronomers in Imp ...
The Milky Way Galaxy
... Discovering The Galaxy In the early part of the century Harlow Shapley found the distance to globular clusters using ...
... Discovering The Galaxy In the early part of the century Harlow Shapley found the distance to globular clusters using ...
Spot detection on solar like stars
... starspots, similar to solar active regions). – temperatures of 4900 - 5500 K, being hotter than regular sunspots (3800-4400K), however the surface temperature of HD 209458, 6000K, is also hotter than that of the Sun (5780K). Nevertheless, the sunspots seen in the white light image are also about 0.4 ...
... starspots, similar to solar active regions). – temperatures of 4900 - 5500 K, being hotter than regular sunspots (3800-4400K), however the surface temperature of HD 209458, 6000K, is also hotter than that of the Sun (5780K). Nevertheless, the sunspots seen in the white light image are also about 0.4 ...
giants1
... The well known age-metallicity degeneracy requires determination of [Fe/H] to derive more precise stellar characteristics FEROS and TLS spectra (templates) for analysis; S/N= >150, R=50000-67000, large spectral coverage Initial Teff from Photometry, log(g) assuming M=1M Spectroscopic determination: ...
... The well known age-metallicity degeneracy requires determination of [Fe/H] to derive more precise stellar characteristics FEROS and TLS spectra (templates) for analysis; S/N= >150, R=50000-67000, large spectral coverage Initial Teff from Photometry, log(g) assuming M=1M Spectroscopic determination: ...
Ch. 21
... has accumulated too much mass from binary companion If the white dwarf’s mass exceeds 1.4 solar masses, electron degeneracy can no longer keep the core from collapsing. Carbon fusion begins throughout the star almost simultaneously, resulting in a carbon explosion. ...
... has accumulated too much mass from binary companion If the white dwarf’s mass exceeds 1.4 solar masses, electron degeneracy can no longer keep the core from collapsing. Carbon fusion begins throughout the star almost simultaneously, resulting in a carbon explosion. ...
The Milky Way
... • Old, metal-poor stars in the spherical parts of the Galaxy (Bulge and disk) are called Pop. II • Formed by collapse of ...
... • Old, metal-poor stars in the spherical parts of the Galaxy (Bulge and disk) are called Pop. II • Formed by collapse of ...
THE NAMING OF STARS AND THE STUDY OF PROTOSTARS D. R.
... description of the formation of stars is rather less successful. An understanding of this may be the real solution to the problem of how to understand and to classify stars. It is considered that stars are formed from protostars which are large clouds of material which mainly under gravity, coalesce ...
... description of the formation of stars is rather less successful. An understanding of this may be the real solution to the problem of how to understand and to classify stars. It is considered that stars are formed from protostars which are large clouds of material which mainly under gravity, coalesce ...
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.