Rotational Dynamics PowerPoint
... angular acceleration have the same form as those for linear motion with constant acceleration. • Torque is the product of force and lever arm. • The rotational inertia depends not only on the mass of an object but also on the way its mass is distributed around the axis of rotation. • The angular acc ...
... angular acceleration have the same form as those for linear motion with constant acceleration. • Torque is the product of force and lever arm. • The rotational inertia depends not only on the mass of an object but also on the way its mass is distributed around the axis of rotation. • The angular acc ...
Order-of-Magnitude Astrophysics
... starts with no metals) and that both the Pop II and Pop III stars generate most of their energy by the CNO cycle, whose efficiency is approximately proportional to T12 in the relevant temperature range. (See Tumlinson & Shull 2000, ApJ 528, L65.) 55. A black hole of mass M accretes gas at a rate Md ...
... starts with no metals) and that both the Pop II and Pop III stars generate most of their energy by the CNO cycle, whose efficiency is approximately proportional to T12 in the relevant temperature range. (See Tumlinson & Shull 2000, ApJ 528, L65.) 55. A black hole of mass M accretes gas at a rate Md ...
File
... Impulse • During a collision the force on an object usually jumps from 0 to very high in a very short amount of time and then abruptly returns to 0. • Let’s start with ΣF = Δp/Δt • And solve it for Δp, • Δp = FΔt = impulse ...
... Impulse • During a collision the force on an object usually jumps from 0 to very high in a very short amount of time and then abruptly returns to 0. • Let’s start with ΣF = Δp/Δt • And solve it for Δp, • Δp = FΔt = impulse ...
Lecture 12
... Their masses have been measured in X-ray emitting binary systems NS masses are clustered around 1.4 M The maximum limit for a stable neutron star is 3-5M Hard lower limits for masses of compact objects have been determined which have values much greater than this limit These are the best stellar ...
... Their masses have been measured in X-ray emitting binary systems NS masses are clustered around 1.4 M The maximum limit for a stable neutron star is 3-5M Hard lower limits for masses of compact objects have been determined which have values much greater than this limit These are the best stellar ...
Ch_07
... 7-6 Inelastic Collisions With inelastic collisions, some of the initial kinetic energy is lost to thermal or potential energy. It may also be gained during explosions, as there is the addition of chemical or nuclear energy. A completely inelastic collision is one where the objects stick together af ...
... 7-6 Inelastic Collisions With inelastic collisions, some of the initial kinetic energy is lost to thermal or potential energy. It may also be gained during explosions, as there is the addition of chemical or nuclear energy. A completely inelastic collision is one where the objects stick together af ...
Towards Planetesimals in the Disk around TW Hya: 3.5 centimeter
... al. 2000; Weinberger et al. 2002) and in thermal emission from dust and trace molecules (Weintraub, Sandell, & Duncan 1989; Kastner et al. 1997; Qi et al. 2004). The dust in the TW Hya disk, like the dust in disks around many younger stars, has long been known to show evidence for size evolution fro ...
... al. 2000; Weinberger et al. 2002) and in thermal emission from dust and trace molecules (Weintraub, Sandell, & Duncan 1989; Kastner et al. 1997; Qi et al. 2004). The dust in the TW Hya disk, like the dust in disks around many younger stars, has long been known to show evidence for size evolution fro ...
Physics 106P: Lecture 1 Notes
... In any natural process, total energy is always “conserved”, i.e. energy can not be created nor destroyed. Can be transformed from one form to another. Can be transferred from one system to ...
... In any natural process, total energy is always “conserved”, i.e. energy can not be created nor destroyed. Can be transformed from one form to another. Can be transferred from one system to ...
Math Notes - UNC Physics and Astronomy
... M = mass of object R = radius of object Rs = Schwarzschild radius of object G = Newton’s gravitational constant c = speed of light Recall the escape speed equation from Lesson 2: vesc = (2GM / R)1/2 Solving for R yields: R = 2GM / vesc2 Setting vesc = c yields the Schwazschild ra ...
... M = mass of object R = radius of object Rs = Schwarzschild radius of object G = Newton’s gravitational constant c = speed of light Recall the escape speed equation from Lesson 2: vesc = (2GM / R)1/2 Solving for R yields: R = 2GM / vesc2 Setting vesc = c yields the Schwazschild ra ...
jan0605
... 7. Continued accretion of small satellite galaxies as Milky Way builds its outer halo Total mass ~ few x 1011 solar masses: <1% halo+bulge; 10% disk; ~90% dark matter ...
... 7. Continued accretion of small satellite galaxies as Milky Way builds its outer halo Total mass ~ few x 1011 solar masses: <1% halo+bulge; 10% disk; ~90% dark matter ...
