Lightyear? Speed of Light?

Lightspeed

How much is a Lightyear? - One lightyear is about 5.87 trillion miles or 9.46 trillion kilometers.
A lightyear means the distance light travels through space in one year. The speed of Light is Light travels at a constant, finite speed of 186,000 mi/sec. (about 300 thousand kms a second) A traveler, moving at the speed of light, would circum-navigate the equator approximately 7.5 times in one second. By comparison, a traveler in a jet aircraft, moving at a ground speed of 500 mph, would cross the continental U.S. once in 4 hours

Image Source;truewhisper.com

The term speed of light generally refers to a fundamental physical constant of spacetime that limits the rate of transfer of matter or information. The speed of light is the speed of not just visible light, but of all electromagnetic radiation in vacuum (also called free space), and usually is denoted by the symbol c. Speeds faster than that of light are encountered in physics but, in all such cases, no matter or information is transmitted faster than c. The speed of light also plays a role in general relativity, and is believed to be the speed of gravitational waves.

In SI units, the magnitude of the speed of light in vacuum is exactly 299,792,458 metres per second (m/s) because of the way the metre is defined. Said in different words, the exact value, c = 299 792 458 m/s, is an international convention concerning the metre, not a property of light.

For many practical purposes, the speed of light is so great that it can be regarded to travel instantaneously. An exception is where long distances or precise time measurements are involved. For example, in the Global Positioning System (GPS), a GPS receiver measures its distance to satellites based on how long it takes for a radio signal to arrive from the satellite. In astronomy, distances are often measured in light-years, the distance light travels in a year.

The speed of light when it passes through a transparent or translucent material medium, like glass or air, is less than its speed in vacuum. The speed is inversely proportional to the refractive index of the medium. In specially-prepared media, the speed can be tiny, or even zero.

For many years the speed of light was the subject of speculation, some believing it to be infinite. The first effective measurements of the speed of light were made in the seventeenth century, and these were progressively refined until, in 1983, the speed of light in vacuum was fixed by definition.

Demonstration of Lightspeed

Speed of Light Demonstration by the Foucault Method - Kevin McFarland

University of Rochester PARTICLE Summer Workshop

In the mid-19th century, French physicist Leon Foucault made the most accurate measurement to-date of the speed of light using a laboratory-sized apparatus consisting of rotating and fixed mirrors.



This method was subsequently improved upon in technique and scale by Albert Michelson in the 1920s, resulting in the most precise “mechanical” measurement of the speed of light, with an error of only ±4km/sec! An apparatus inspired by Foucault’s original technique is accessible as a classroom demonstration or laboratory, and makes an excellent way to illustrate the finite (but large) speed of light.

The basic technique is to send a beam of on a path so that it bounces between a rotating mirror, a fixed mirror and back to the rotating mirror for a total distance 2D, as shown in the above illustration. The time of flight of the light on this path implies that the rotating mirror will have turned very slightly between the two times of arrival of the light. This small rotation will deflect the beam of light through a small angle θ from its original path, producing a measurable effect proportional to the mirror and inversely proportional to the speed of light.



If the rotational frequency (revolutions per unit time) of the mirror is given by υ, then the deflection angle is given by where the second factor angular frequency of rotation and the last is the time to travel back and forth between the mirrors.

For our demonstration, we used a He-Ne laser as the source (a much better source than Foucault had!). At these distances, the laser acts essentially as a point source of light, so it is necessary to focus the beam so that the points of focus are the fixed mirror (M) and source and observation point (S). Let D’ be the distance between the rotating mirror and the source/observation point, G be the distance between the lens (L) and fixed mirror (M) and G’ be the distance the light travels from the lens to the source point (LR+RS). Then the lens makers’ equation tells us that the focal length, f, of the lens must be:

For our setup, we used a lens with a focal length of 5m, and set G and G’ to be 10m. We set the distance D to be approximately 13m and D’ to be 7m. In order to observe the deflection of the beam, we inserted a thin (to minimize internal reflections) microscope slide beam splitter just before the source. Our rotating mirror is based on a Bosch router motor, with a peak speed of 27000rpm at 120V AC.

Alignment is slightly tricky. I suggest establishing the beam to the rotating mirror first, and then moving the rotating mirror to point approximately at the desired location of the fixed mirror. The beam should go to the center of the lens and the fixed mirror, and then (harder) the spot returning from the fixed mirror must be aligned on the rotating mirror. At this point, the returned beam should be visible after the beam splitter! Chalk dust and water mist make great diagnostics for finding the beam and small variations in the lens position sometimes can compensate for small mirror misalignments. This takes some patience and good clamps for the lens and fixed mirrors!

One you have established a view of the beam after the beam splitter, I suggest measuring the beam spot position at high and low frequency. The deviation of the beam spot, δx, will be

where δυ is the difference between the high and low frequencies. For our setup, we found deviations of about 2-3mm with δυ of about 300Hz.

A diagram showing a modern approach to measuring the speed of light using Foucault's rotating mirror method.

Sources;
NASA website Wikipedia Rochester University

Terminology Used in Alpha Centauri

Alpha Centauri wishes it's readers to be able to understand the terminology used in this site. For this reason there will be various posts on each term used in the Alpha Centauri blog for you to research the meanings of words used when you need to - this you can do by clicking on the "terminology" label on the navigation bar.

Where is Proxima Centauri?

If you were able to view the galaxy from outside, the Sun and Proxima Centauri would be seemingly lost in the immense cloud of stars which compose this Galaxy.
To make this more understandable for those of you on the surface of Planet Earth, Proxima Centauri is in one way extremely far away according to the terms of measurement you are accustomed to; Approximately 25 trillion miles distance from the Sun.
But in Galactic and Intergalactic terms, you can consider it to be in relative proximity to Earth's Solar System. Among the 100 billion or more stars visible in this Galaxy, The stars Alpha Centauri A, Alpha Centauri B and Proxima Centauri (also called Alpha Centauri C) are the three closest to Planet Earth.
Proxima Centauri is a Red Dwarf star located about 4.2 lightyears away from your Planet. (this means about 5.9 trillion miles).


On Proxima's surface, flares, or explosive outbursts, are occuring almost constantly. This is due to Proxima Centauri's extremely low mass, about one tenth of the mass of your Sun. Inside the cores of low mass stars, nuclear fusion reactions that convert hydrogen to helium proceed, albeit very slowly. These reactions, create a turbulent, convectional motion within the interior core. This convection stores up great magnetic energy forces, which is often released in the form of explosions in the star's upper atmosphere, producing flares in the form of X-rays and other types of light emissions.
This is the very same process that produces X-rays on the surface of your Sun. Except that the magnetic energy of your Sun, is released in a much weaker way and the explosions appear through gas loop heating, which causes occasional flares.



Red dwarfs are the most common type of star known to Humans, with an average mass between about 8% and 50% of the mass of the Sun. They are commonly much less bright than the Sun, but will generally shine for much longer, up to trillions of years in the case of Proxima Centauri, where as the lifetime of the Sun's luminosity is expected to reach a mere 10 billion-year lifetime.


Viewed from afar, what you have come to know as the "Milky Way Galaxy" would look like a whirlwind cloud storm with two arms, a spiral of stars, this cloud of stars is not spherical in shape, rather is flat. 100,000 lightyears in diameter with an ever increasing density of stars the more you move towards the center. The core however, seems to be an empty hole. This is because there is a black hole in the center which prevents light from escaping. The black hole is also the reason why this Galaxy is flat.
You can see Proxima Centauri's sister stars with the naked eye from Earth's surface, but Proxima is not visible without use of some kind of apparatus.

Alpha Centauri A and Alpha Centauri B can be seen as bright stars. these two stars are what you call a "binary" star. This is because they are orbiting each other. Alpha Centauri A and B are located approximately 4.4 lightyears from your Sun (perhaps around 6 Trillion miles or more).
Proxima Centauri, the star nearest to Earth, is so far away it's only a pinpoint of light even when viewed through some of your biggest telescopes when viewed from Earth. Proxima Centauri is extremely close to us in Galactic terms.

Does Proxima have planets? This is something that Earth's People shall have to wait and see when the time is right.
Proxima Centauri is about 6 Billion Earth years old