About Earth Science...?

Question

What is a black hole and how does it work? Explain the concept of spaghettification in black holes. Give the definitions of pulsar, quasar, neutron star, and binary star.

Astronomy is also included in Earth Science. Why? The earth itself is in the cosmos. duh...

This is not earth science. But how do you simplify like terms? Pls. answer this too. tnx. :)

Answer 1

did you say "earth science?"

Answer 2

Black holes are also referred to as singularities. when getting near the event horizon of the black hole, particles of the object will be pulled with different intentisities. Remember newton's gravity: the gravity of two objects is inversely proportional to their distance. So, particles of the object at the end/side near the hole will be pulled apart from particles on the other side/end since they would be under stronger gravitational pull. This would cause the object to get stretched out like a piece of spaghetti.
Pulsar - pulsing star
The matter left after a star goes supernova will coalesce in a fashion that it begins to spin. It will radiate energy from only one point. This energy can be observed when the source points at the observer, so it appears to "pulse". Like an old pilce car light--before strobe I mean. The light wasn't blinking on and off, it's beam was spinning around and from one stationary point away from the light makes it look like it is blinking on and off.
A quasar is a QUASistellar Radio source.
Neutron star is what's left over after certain types of stars go supernova. Our Sun will not go supernova, it is too small. It will turn into a red giant, then a white dawrf after it goes nova.
A binary star is like a binary anything, binary means two. Your computer is a binary device. It deals with only two "digits", 1 and 0. this refers to the two states the transistors in the procesors can be in either on-1 or off-0.

Answer 3

black hole is some part of the space which has the most highest gravitational force.. even light cannot escape from this!!!!
pulsar is a system where 2 stars revolve around a common point or object.
quasar is also a period of a star before dying or destruction.
neutron star is a stage of a star after death in which there r only uncharged or neutral particles.
binary star is a system of 2 stars revolving around a single centre of gravity.

Answer 4

Black Hole>http://en.wikipedia.org/wiki/Black_hole#Fact_and_fiction

Definitions>http://dictionary.reference.com/

Answer 5

pulsar -- a degenerate neutron star; small and extremely dense; rotates very fast and emits regular pulses of polarized radiation
quasar--.An extremely distant, and thus old, celestial object whose power output is several thousand times that of our entire galaxy.
neutron star, extremely small, extremely dense star, about double the sun's mass but only a few kilometers in radius, in the final stage of stellar evolution. Astronomers Baade and Zwicky predicted the existence of neutron stars in 1933. In the central core of a neutron star there are no stable atoms or nuclei; only elementary particles can survive the extreme conditions of pressure and temperature. Surrounding the core is a fluid composed primarily of neutrons squeezed in close contact. The fluid is encased in a rigid crystalline crust a few hundred meters thick. The outer gaseous atmosphere is probably only a few centimeters thick. The neutron star resembles a single giant nucleus because the density everywhere except in the outer shell is as high as the density in the nuclei of ordinary matter. There is observational evidence of the existence of several classes of neutron stars: pulsars are periodic sources of radio frequency, X ray, or gamma ray radiation that fluctuate in intensity and are considered to be rotating neutron stars. A neutron star may also be the smaller of the two components in an X-ray binary star.
binary star or binary system, pair of stars that are held together by their mutual gravitational attraction and revolve about their common center of mass. In 1650 Riccioli made the first binary system discovery, that of the middle star in the Big Dipper's handle, Zeta Urase Majoris. True binary stars are distinct from optical doubles—pairs of stars that lie nearly along the same line of sight from the earth but are not physically associated. Binary stars are grouped into three classes. A visual binary is a pair of stars that can be seen by direct telescopic observation to be a distinct pair with shared motion. A spectroscopic binary cannot be seen as two separate stars, even with the most powerful telescopes, but spectral lines from the pair show a periodic Doppler effect that indicates mutual revolution. Some lines indicate motion toward the earth while others indicate motion away; later, as the stars revolve around in their orbit, this pattern reverses. An eclipsing binary has the plane of its orbit lying near the line of sight, and shows a periodic fluctuation in brightness as one star passes in front of the other. The more massive star (A) of a binary is called the primary, and the less massive (B) is called the secondary; e.g., Sirius A and Sirius B are the primary and secondary components of the Sirius system. It seems likely that more than two-thirds of the stars in our galaxy are binary or multiple (a system of more than two stars moving around their mutual center of mass), since many stars within 30 light-years of the sun are binary or multiple. The masses of the components of a spectroscopic binary can be determined from the observed motions and Newton's law of gravitation; binary stars are the only stars outside the solar system for which masses have been directly determined. Binary stars are thus important indicators from which the masses of all similar stars can be deduced. Measurements of the masses of some of the visual binary stars have been used to verify the mass-luminosity relation. Although most binary stars have distance between them, the components of W Ursae Majoris binaries are actually in contact with each other, their mutual gravity distorting their shapes into teardrops. There are binary systems in which one member is a pulsar: PSR 1913+16, for example, has an orbital period of 7 hr 45 min; in this case the other star is also a neutron star. The orbit period decreases as the system loses energy in the form of gravitational waves; used as a clock to measure the effect of the curvature of space-time on the binary's orbit, such a system confirms Einstein's theory of general relativity

A black hole is what remains when a massive star dies.
History
The concept of an object from which light could not escape (e.g., black hole) was originally proposed by Pierre Simon Laplace in 1795. Using Newton's Theory of Gravity, Laplace calculated that if an object were compressed into a small enough radius, then the escape velocity of that object would be faster than the speed of light.

If you have read How Stars Work, then you know that a star is a huge, amazing fusion reactor. Because stars are so massive and made out of gas, there is an intense gravitational field that is always trying to collapse the star. The fusion reactions happening in the core are like a giant fusion bomb that is trying to explode the star. The balance between the gravitational forces and the explosive forces is what defines the size of the star.

As the star dies, the nuclear fusion reactions stop because the fuel for these reactions gets burned up. At the same time, the star's gravity pulls material inward and compresses the core. As the core compresses, it heats up and eventually creates a supernova explosion in which the material and radiation blasts out into space. What remains is the highly compressed, and extremely massive,
core. The core's gravity is so strong that even light cannot escape.

This object is now a black hole and literally disappears from view. Because the core's gravity is so strong, the core sinks through the fabric of space-time, creating a hole in space-time -- this is why the object is called a black hole. The core becomes the central part of the black hole called the singularity. The opening of the hole is called the event horizon.

You can think of the event horizon as the mouth of the black hole. Once something passes the event horizon, it is gone for good. Once inside the event horizon, all "events" (points in space-time) stop, and nothing (even light) can escape. The radius of the event horizon is called the Schwarzschild radius, named after astronomer Karl Schwarzschild, whose work led to the theory of black holes. Types of Black Holes
There are two types of black holes:
Schwarzschild - Non-rotating black hole
Kerr - Rotating black hole
The Schwarzschild black hole is the simplest black hole, in which the core does not rotate. This type of black hole only has a singularity and an event horizon.
The Kerr black hole, which is probably the most common form in nature, rotates because the star from which it was formed was rotating. When the rotating star collapses, the core continues to rotate, and this carried over to the black hole (conservation of angular momentum). The Kerr black hole has the following parts:

Singularity - The collapsed core
Event horizon - The opening of the hole
Ergosphere - An egg-shaped region of distorted space around the event horizon (The distortion is caused by the spinning of the black hole, which "drags" the space around it.)
Static limit - The boundary between the ergosphere and normal space

Photo courtesy NASA
Artist concept of a black hole and its surroundings: The blackened circle is the event horizon and the egg-shaped region is the ergosphere.

If an object passes into the ergosphere it can still be ejected from the black hole by gaining energy from the hole's rotation.
However, if an object crosses the event horizon, it will be sucked into the black hole and never escape. What happens inside the black hole is unknown; even our current theories of physics do not apply in the vicinity of a singularity.

Even though we cannot see a black hole, it does have three properties that can or could be measured:

Mass
Electric charge
Rate of rotation (angular momentum)
As of now, we can only measure the mass of the black hole reliably by the movement of other objects around it. If a black hole has a companion (another star or disk of material), it is possible to measure the radius of rotation or speed of orbit of the material around the unseen black hole.