Monday, September 5, 2011

Top 10 quirky science tricks for parties

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Saturday, September 3, 2011

Solar storm a serious threat around 2012


Solar storm is a serious threat around 2012. Both NASA and ESA confirmed the next huge solar storm between September 2012 and May 2013. We all heard about the big one in 1859 and it looks like we are not far away from another one coming our way.

For more info please read the NASA's report from May 2009:
- http://science.nasa.gov/headlines/y2009/29may_noaaprediction.htm

and ESA's March 2008 report :
- http://www.esa.int/esaSC/SEMJSD5QGEF_index_0.html

..from August 2010:
- http://www.news.com.au/technology/sun-storm-to-hit-with-force-of-100-bombs/story-e6frfro0-1225909999465#ixzz0xfyUPTiq

Here are the latest warnings from September 2010:
- http://www.responsesource.com/releases/rel_display.php?relid=59406

- http://www.thesun.co.uk/sol/homepage/news/3145874/Solar-flare-to-paralyse-Earth-in-2013.html

- http://www.mumbaimirror.com/article/7/2010092220100922033433230e17c3bc5/Solar-flare-could-potentially-paralyse-Earth-in-three-years.html

- http://www.telegraph.co.uk/science/space/8014444/Britain-vulnerable-to-space-nuclear-attack-or-solar-flare-storm-conference-told.html

- http://www.dailymail.co.uk/sciencetech/article-1313858/Solar-flare-paralyse-Earth-2013.html?ito=feeds-newsxml

- http://www.southgatearc.org/news/september2010/solar_storm_warning_system.htm
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Friday, September 2, 2011

The Biggest Stars In The Universe


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Star Size Comparison: The biggest/largest known stars in the Universe.

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VY Canis Majoris (VY CMa) is a red hypergiant star located in the constellation Canis Major. With a size of 2600 solar radii, it is the largest known star and also one of the most luminous known. It is located about 1.5 kiloparsecs (4.6×1016 km) or about 4,900 light years away from Earth. Unlike most stars, which occur in either binary or multiple star systems, VY CMa is a single star. It is categorized as a semiregular variable and has an estimated period of 6,275,081 days, or just under 17,200 years.

Antares is a red supergiant star in the Milky Way galaxy and the sixteenth brightest star in the nighttime sky (sometimes listed as fifteenth brightest, if the two brighter components of the Capella quadruple star system are counted as one star). Along with Aldebaran, Spica, and Regulus it is one of the four brightest stars near the ecliptic. Antares is a variable star, whose apparent magnitude varies from +0.9 to +1.8.

The Pistol Star is a blue hypergiant and is one of the most luminous known stars in the Milky Way Galaxy. It is one of many massive young stars in the Quintuplet cluster in the Galactic Center region. The star owes its name to the shape of the Pistol Nebula, which it illuminates. It is located approximately 25,000 light years from Earth in the direction of Sagittarius. It would be visible to the naked eye as a fourth magnitude star, if it were not for the interstellar dust that completely hides it from view in visible light.

Rigel (β Ori / β Orionis / Beta Orionis) is the brightest star in the constellation Orion and the sixth brightest star in the sky, with visual magnitude 0.18. Although it has the Bayer designation "beta", it is almost always brighter than Alpha Orionis (Betelgeuse).

Aldebaran (α Tau, α Tauri, Alpha Tauri) is an orange giant star located about 65 light years away in the zodiac constellation of Taurus. With an average apparent magnitude of 0.87 it is the brightest star in the constellation and is one of the brightest stars in the nighttime sky. The name Aldebaran is Arabic (الدبران al-dabarān) and translates literally as "the follower", presumably because this bright star appears to follow the Pleiades, or Seven Sisters star cluster in the night sky. This star is also called the Bull's Eye because of its striking orange color and its location in the bull's head shaped asterism. NASA's Pioneer 10 spacecraft, which flew by Jupiter in 1973, is currently traveling in the direction and will reach it in about two million years.

Arcturus (α Boo / α Boötis / Alpha Boötis) is the brightest star in the constellation Boötes. With a visual magnitude of −0.05, it is also the third brightest star in the night sky, after Sirius and Canopus. It is, however, fainter than the combined light of the two main components of Alpha Centauri, which are too close together for the eye to resolve as separate sources of light, making Arcturus appear to be the fourth brightest. It is the second brightest star visible from northern latitudes and the brightest star in the northern celestial hemisphere. The star is in the Local Interstellar Cloud.

Pollux (β Gem / β Geminorum / Beta Geminorum) is an orange giant star approximately 34 light-years from the Earth in the constellation of Gemini (the Twins). Pollux is the brightest star in the constellation, brighter than Castor (Alpha Geminorum). As of 2006, Pollux was confirmed to have an extrasolar planet orbiting it.

Sirius is the brightest star in the night sky. With a visual apparent magnitude of −1.46, it is almost twice as bright as Canopus, the next brightest star. The name Sirius is derived from the Ancient Greek Σείριος. The star has the Bayer designation α Canis Majoris (α CMa, or Alpha Canis Majoris). What the naked eye perceives as a single star is actually a binary star system, consisting of a white main sequence star of spectral type A1V, termed Sirius A, and a faint white dwarf companion of spectral type DA2, termed Sirius B.

The Sun is the star at the center of the Solar System. The Sun has a diameter of about 1,392,000 kilometres (865,000 mi) (about 109 Earths), and by itself accounts for about 99.86% of the Solar System's mass; the remainder consists of the planets (including Earth), asteroids, meteoroids, comets, and dust in orbit. About three-fourths of the Sun's mass consists of hydrogen, while most of the rest is helium.

http://en.wikipedia.org/wiki/Largest_stars

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CREDITS
Animations: morn1415, NASA, ESO, Hubblecast
Editing: http://www.youtube.com/Best0fScience
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Thursday, September 1, 2011

E = mc² | Einstein's Relativity

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Albert Einstein's Theory of Relativity (Chapter 4): E = mc² (Mass-Energy Equivalence)

In physics, mass-energy equivalence is the concept that the mass of a body is a measure of its energy content. In this concept the total internal energy E of a body at rest is equal to the product of its rest mass m and a suitable conversion factor to transform from units of mass to units of energy. If the body is not stationary relative to the observer then account must be made for relativistic effects where m is given by the relativistic mass and E the relativistic energy of the body.

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Albert Einstein proposed mass-energy equivalence in 1905 in one of his Annus Mirabilis papers entitled "Does the inertia of a body depend upon its energy-content?" The equivalence is described by the famous equation E = mc2, where E is energy, m is mass, and c is the speed of light in a vacuum. The formula is dimensionally consistent and does not depend on any specific system of measurement units. For example, in many systems of natural units, the speed of light is set equal to 1, and the formula becomes the identity E = m; hence the term "mass-energy equivalence".

The equation E = mc2 indicates that energy always exhibits mass in whatever form the energy takes. Mass-energy equivalence also means that mass conservation becomes a restatement, or requirement, of the law of energy conservation, which is the first law of thermodynamics. Mass-energy equivalence does not imply that mass may be 'converted' to energy, and indeed implies the opposite. Modern theory holds that neither mass nor energy may be destroyed, but only moved from one location to another.

In physics, mass must be differentiated from matter, a more poorly defined idea in the physical sciences. Matter, when seen as certain types of particles, can be created and destroyed, but the precursors and products of such reactions retain both the original mass and energy, both of which remain unchanged (conserved) throughout the process. Letting the m in E = mc2 stand for a quantity of "matter" may lead to incorrect results, depending on which of several varying definitions of "matter" are chosen.

E = mc2 has sometimes been used as an explanation for the origin of energy in nuclear processes, but mass-energy equivalence does not explain the origin of such energies. Instead, this relationship merely indicates that the large amounts of energy released in such reactions may exhibit enough mass that the mass-loss may be measured, when the released energy (and its mass) have been removed from the system.

Einstein was not the first to propose a mass-energy relationship. However, Einstein was the first scientist to propose the E = mc2 formula and the first to interpret mass-energy equivalence as a fundamental principle that follows from the relativistic symmetries of space and time.

• http://en.wikipedia.org/wiki/Mass%E2%80%93energy_equivalence
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