Disk Galaxies: Structural Components
... • Bulges of spiral galaxies are similar to certain elliptical galaxies; formed as a result of monolithic collapse of a cloud of gas and dark matter with very little angular momentum ...
... • Bulges of spiral galaxies are similar to certain elliptical galaxies; formed as a result of monolithic collapse of a cloud of gas and dark matter with very little angular momentum ...
SSS in young stellar populations: progenitors of the
... • Be stars are non-giant B stars which show emission lines in their spectra • Are known to be rapidly rotating, at 70-90% of breakup velocity (Townsend et al., 2004) • Emission lines believed to arise in decretion disk which forms due to massive rotation • Evidence that rapid rotation is due to CBE ...
... • Be stars are non-giant B stars which show emission lines in their spectra • Are known to be rapidly rotating, at 70-90% of breakup velocity (Townsend et al., 2004) • Emission lines believed to arise in decretion disk which forms due to massive rotation • Evidence that rapid rotation is due to CBE ...
The Birth of Stars
... The new young star is exposed, while the accretion disk is still in place. The spectrum of all is seen together (so we don’t have to image disks in order to know they are there). ...
... The new young star is exposed, while the accretion disk is still in place. The spectrum of all is seen together (so we don’t have to image disks in order to know they are there). ...
Problem set 11
... 1. h9i Consider force free motion of a symmetric top with I1 = I2 , as discussed in the lecture. Suppose the axis of the top makes an angle θ , 0 with the fixed direction of L. (a) h6i Find the angle α between the angular velocity vector Ω and angular momentum vector L (α is half the opening angle o ...
... 1. h9i Consider force free motion of a symmetric top with I1 = I2 , as discussed in the lecture. Suppose the axis of the top makes an angle θ , 0 with the fixed direction of L. (a) h6i Find the angle α between the angular velocity vector Ω and angular momentum vector L (α is half the opening angle o ...
The Milky Way Galaxy
... Younger stars and star forming regions near the center, older stars above and below ...
... Younger stars and star forming regions near the center, older stars above and below ...
wilner_alma06
... • precision subarcsec spectral index information – couple with disk structure models to account for opacity and temperature variations, localize grain growth ...
... • precision subarcsec spectral index information – couple with disk structure models to account for opacity and temperature variations, localize grain growth ...
Part 2: Solar System Formation
... • Within the disk, material is constantly colliding with one another. If the collisions are not too violent material may stick together. • In the outer parts of the Solar Nebula the planets become large enough to have a significant gravitational pull and collect gas around them. • Planets in the inn ...
... • Within the disk, material is constantly colliding with one another. If the collisions are not too violent material may stick together. • In the outer parts of the Solar Nebula the planets become large enough to have a significant gravitational pull and collect gas around them. • Planets in the inn ...
投影片 1
... evolution of stars like the Sun Its progenitor had an original mass about seven times the Sun’s From the death of GD362,it passed two to five billion years based on the cooling rate ...
... evolution of stars like the Sun Its progenitor had an original mass about seven times the Sun’s From the death of GD362,it passed two to five billion years based on the cooling rate ...
Some progress in black hole accretion
... lines based on the conservation of energy, angular momentum and magnetic flux as shown in Fig. 7. The emerged Spectra is obtained by using Monte-Carlo Simulation as shown in Fig. 8. ...
... lines based on the conservation of energy, angular momentum and magnetic flux as shown in Fig. 7. The emerged Spectra is obtained by using Monte-Carlo Simulation as shown in Fig. 8. ...
stars
... • Over the course of their lifetimes, hot, luminous, massive (OB-type) stars lose large amount of mass in nearly continuous outflow called stellar winds. • These winds are driven by scattering of the star’s continuum radiation in a large ensemble of spectral lines (Castor, Abbott & ...
... • Over the course of their lifetimes, hot, luminous, massive (OB-type) stars lose large amount of mass in nearly continuous outflow called stellar winds. • These winds are driven by scattering of the star’s continuum radiation in a large ensemble of spectral lines (Castor, Abbott & ...
Placing Our Solar System in Context
... Are planetary systems like our own are common or rare among sun-like stars in the Milky Way galaxy? Primordial Disk Evolution: - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in ...
... Are planetary systems like our own are common or rare among sun-like stars in the Milky Way galaxy? Primordial Disk Evolution: - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in ...
Accretion and radial disk structure
... • Vertical structure models predict SEDs: disks are flared disks possess an inner rim (dust evaporation radius) • Tgas > Tdust in disk surface layers (tross <~ 1.0): gas and dust are not well coupled molecules can form • Disk dispersal can proceed via photoevaporation by the FUV/EUV of the central s ...
... • Vertical structure models predict SEDs: disks are flared disks possess an inner rim (dust evaporation radius) • Tgas > Tdust in disk surface layers (tross <~ 1.0): gas and dust are not well coupled molecules can form • Disk dispersal can proceed via photoevaporation by the FUV/EUV of the central s ...