Astronomy
Chapter 21 Homework
Homework
Scholars Online Astronomy - Chapter 21: Neutron Stars and Black Holes
Homework
- Reading Preparation
- Key Formulae to Know
- WebLecture
- Study Activity
- Chat Preparation Activities
- Chapter Quiz
- Lab Work
Reading Preparation
Reading: Astronomy, Chapter 21: Stellar Remnants: Neutron Stars and Black Holes
Study Guide
- Section 1: When a star is dense enough at its cores, even electron degeneracy will not withstand the pressure. The atomic structure collapses, forcing protons and electrons to combine to form neutrons, creating a neutron star rotating at high velocity and generating a magnetic field that focuses particles into radiation beams from the poles (pulsars). Gas falling onto the surface of such stars heats up and explodes in a superficial thermonuclear reaction, bursting and cooling.
- Section 2: Relativity - Einstein's special theory of relativity predicts length contraction, time dilation, and mass increases for objects in motion, and explains why two observers with different motions experience time and distance differently.
- Section 3: Equivalence - The general theory of relativity explains why it is impossible to distinguish between force due to gravity and force due to acceleration. the general theory of relativity is supported by observations of light "bending" as it travels through space around massive objects such as galaxies. Because light has a finite velocity, it is possible for massive objects with escape velocities greater than the speed of light to "trap light" so that it cannot escape.
- Section 4: LIGO technology is used to detect gravitational waves from high-mass events such as the merger of two neutron stars or two black holes.
- Section 5: Binary star systems such as Cygnus X-1 may contain a black hole, when one of the stars which is red giant phase, and contracts, draining mass from its companion until it reaches the limit where v = √(2GM/R) > c. Other possible black hole locations are the cores of galaxies.
- Section 6: Gamma-ray bursters may be the result of jets from black hole accretion disks that form temporarily as massive stars (collapsars) contract during a supernova explosion.
- Section 7: Gravitational models based on the revolution of stars around galactic centers indicate the existence of massive cores that exceed the limits required to form black holes.
- Section 8: Because nothing can escape from a black hole, the only observable characteristics are its mass, radius, and location or center. Distinctions between types of atoms are obliterated by destruction of all atomic structures under the pressure of the hole. The point at which light "falls back" to the material surface of the black hole is its event horizon, and the distance to this point from the center of mass is the Schwarzschild radius.
- Section 9: Black holes have mass, rotation, and (sometimes) electrical charge. Rotating black holes may interact with the magnetic fields of their accretion disks, even transferring energy from the black hole's rotational momentum to objects outside the hole. Masses drag spacetime as they rotate, so near the surface of a black hole in the ergoregion, an object cannot be at rest.
- Section 10: An object falling into a black hole experiences time contraction and length dilation, as seen by an outside observer.
- Section 11: The Heisenberg uncertainty principle requires that we cannot determine both position and speed of a subatomic particle. This is a fundamental principle, not a limitation of observation technology that could at some point be overcome. A collateral effect of this principle is the spontaneous creation and annihilation of virtual particles and their antiparticles. When this happens near the surface of a black hole and one member of the pair falls into the black hole, the other gains energy, converts to real mass, and becomes a real particle. This event is Hawking radiation, which drains energy over time. Evaporation of matter from already low-mass black holes may cause the black hole to vanish.
Key Formulae to Know
| Escape Velocity | G: Gravitational Constant M: Mass of primary body R: Starting point distance to center of mass M | |
| Lorentz transformation for time | T: time measured by moving observer T0: time measured by non-moving observer v: speed of moving observer c: speed of light |
|
| Lorentz transformation for length | L: Length measured for moving object along direction of motion L0: Length of object when not moving v: speed of moving observer c: speed of light |
Web Lecture
Read the following weblecture before chat: Black Holes
Study Activity
Study the visualization of a black hole at the ESA site. [Note that this site takes a while to load. Be patient.] What features do you notice? What happens to the background if you rotate your view of the hole (view it from above and below)? Would a black hole be invisible in space? How would you detect its presence and be able to identify it?
Website of the Week: Explore the Black Hole: Gravity's Relentless Pull -- the introductory animation is only the beginning. The site contains both an interactive animation and an in-depth presentation of topics in encyclopaedia form.
Chapter Quiz
- Required: Complete the Mastery exercise with a passing score of 85% or better.
- Go to the Moodle and take the quiz for this chat session to see how much you already know about astronomy!
Lab Work
Read through the lab for this week; bring questions to chat on any aspect of the lab, whether you intend not perform it or not. If you decide to perform the lab, be sure to submit your report by the posted due date.
- Lab instructions: Binary Stars
© 2005 - 2024 This course is offered through Scholars Online, a non-profit organization supporting classical Christian education through online courses. Permission to copy course content (lessons and labs) for personal study is granted to students currently or formerly enrolled in the course through Scholars Online. Reproduction for any other purpose, without the express written consent of the author, is prohibited.