this poster - Astrophysics
... Active Galactic Nuclei The presence of supermassive black holes in the cores of galaxies has been inferred from observations of Active Galactic Nuclei (AGN). These are characterised by enhanced emission at all wavelengths in galaxy nuclei which is fuelled by accretion of matter onto a central compac ...
... Active Galactic Nuclei The presence of supermassive black holes in the cores of galaxies has been inferred from observations of Active Galactic Nuclei (AGN). These are characterised by enhanced emission at all wavelengths in galaxy nuclei which is fuelled by accretion of matter onto a central compac ...
Modeling Time Dependent Winds - Center for Computational Sciences
... • Solar wind originates in open magnetic field lies in coronal holes • Stellar winds from stars rotating near break-up are denser and cooler in the equatorial plane • Winds from accretion disks vary strongly with distance in the disk from the central object • Stellar winds in X-ray binary systems di ...
... • Solar wind originates in open magnetic field lies in coronal holes • Stellar winds from stars rotating near break-up are denser and cooler in the equatorial plane • Winds from accretion disks vary strongly with distance in the disk from the central object • Stellar winds in X-ray binary systems di ...
File1 - School of Astronomy, IPM
... and collapse stop. In order that collapse continues until the star forms, we need energy transport from cloud by radiation to outside. ...
... and collapse stop. In order that collapse continues until the star forms, we need energy transport from cloud by radiation to outside. ...
Discussion Activity #13
... and then blows out in supernovae and then contracts to form stars again and so on. …continued on other side ...
... and then blows out in supernovae and then contracts to form stars again and so on. …continued on other side ...
T3 F2013 9 30
... 3. The uniform solid rectangular block shown below has mass M = 0.25 kg and edge lengths a = 4.0 cm and b = 9.0 cm. Four point masses, m = 0.05 kg are located at the corners. Calculate its rotational inertia about the axis shown, through one corner and perpendicular to the large face. ...
... 3. The uniform solid rectangular block shown below has mass M = 0.25 kg and edge lengths a = 4.0 cm and b = 9.0 cm. Four point masses, m = 0.05 kg are located at the corners. Calculate its rotational inertia about the axis shown, through one corner and perpendicular to the large face. ...
The Merger of Two Disk Galaxies
... the material becomes part of the young Sun, but some debris forms a disk. Within this disk form the planets, moons, comets, asteroids, and meteoroids. Note that this process is repeated on a smaller scale in the outer solar system, where miniature disks form around the Jovian planets. ...
... the material becomes part of the young Sun, but some debris forms a disk. Within this disk form the planets, moons, comets, asteroids, and meteoroids. Note that this process is repeated on a smaller scale in the outer solar system, where miniature disks form around the Jovian planets. ...
Planetary Configurations
... • Recall escape speed: • The Sch. Radius (RS) is the distance at which vesc=c for a BH: ...
... • Recall escape speed: • The Sch. Radius (RS) is the distance at which vesc=c for a BH: ...
Poster
... accretion disk. In sinusoidal perturbation cases,v 0.1Vs 0 sin 2 , where Vs0 is the sound velocity at (r,z)=(r0,0) (see Matsumoto & Shibata 1997; Kato 2002). In random perturbation cases, the sinusoidal function in the abovementioned v is replaced with random numbers between -1 and 1. The cas ...
... accretion disk. In sinusoidal perturbation cases,v 0.1Vs 0 sin 2 , where Vs0 is the sound velocity at (r,z)=(r0,0) (see Matsumoto & Shibata 1997; Kato 2002). In random perturbation cases, the sinusoidal function in the abovementioned v is replaced with random numbers between -1 and 1. The cas ...
Disk Structure
... + OI, water and OH in protoplanetary disks - Oxygen-bearing species (OI, CO, H2O and OH) have a critical role for the disks´ physics, chemistry and dynamics of the warm gas. - ALMA will not be sensitive to the warm gas, will not observe water thermal lines, nor the atomic & ionic fine structure line ...
... + OI, water and OH in protoplanetary disks - Oxygen-bearing species (OI, CO, H2O and OH) have a critical role for the disks´ physics, chemistry and dynamics of the warm gas. - ALMA will not be sensitive to the warm gas, will not observe water thermal lines, nor the atomic & ionic fine structure line ...
The Stromgren sphere around the highest-redshift QSOs
... disks: – Disk winds, infalling material deposited onto the disk, instabilities, self-gravitating disks, star formation … • Binary black holes and coevolution of galaxies and QSOs/AGNs ...
... disks: – Disk winds, infalling material deposited onto the disk, instabilities, self-gravitating disks, star formation … • Binary black holes and coevolution of galaxies and QSOs/AGNs ...
AN INTRODUCTION TO ASTRONOMY Dr. Uri Griv Department of Physics, Ben-Gurion University
... or in q a stellar system PN V = (1/N ) i=1 (vi − v̄)2 where PN v̄ = (1/N ) i=1 vi is the mean velocity and N is the total number of stars • A true MB distribution has a “tail” • Stars will be lost from the cluster • The escape speed ve = 2V ...
... or in q a stellar system PN V = (1/N ) i=1 (vi − v̄)2 where PN v̄ = (1/N ) i=1 vi is the mean velocity and N is the total number of stars • A true MB distribution has a “tail” • Stars will be lost from the cluster • The escape speed ve = 2V ...
The formation of stars and planets
... flux, and sources with strong mid/far-IR flux. One of the ideas is that disk can be self-shadowed to obtain weak mid/far-IR flux. ...
... flux, and sources with strong mid/far-IR flux. One of the ideas is that disk can be self-shadowed to obtain weak mid/far-IR flux. ...
