The
bright flash, fierce and glaring of the shock wave from the explosion
of a star - what astronomers call the rupture shock - was first observed
in the optical wavelength (visible light) telescope space NASA Kepler planet hunting. This
type of exploding stars, or supernovae, are of the most powerful
stellar explosions known, and you can see all the way to the far edge of
the visible universe. When
a massive star dies in a supernova fury unleashed "death", which leaves
behind a sad testimony of his former existence, a very strange, dense
little "weird" called a neutron star or, alternatively, a resident more Cosmos strange - a black hole of stellar mass. In
March 2011, an international team of astronomers led by Dr. Peter
Garnavich, Professor of Astrophysics at the University of Notre Dame in
Indiana announced significant initial observation of this bright flash
of a massive star explodes. This stellar explosion called a collapse or event type II supernova core.
Dr Garnavich and colleagues analyzed the light captured by Kepler every 30 minutes over a period of three years from 500 distant galaxies, examining some 50 billion stars. Astronomers were looking for evidence of supernovae.
In 2011, a massive star duo, known red supergiants was criticized outside while watching the Kepler. The first duo condemned giant star, nicknamed KSN 2011a, is nearly 300 times the size of our Sun, and only about 700 million light years from Earth. The second pair of tragic star named KSN 2011d, is about 500 times the size of our star and about 1.2 million light years.
"To put in perspective the size of the orbit of the Earth around our sun could fit comfortably within these colossal stars," said Dr. Garnavich in March 21, 2016 NASA press release.
Stars beat towards energy following the nuclear fusion process. Unlike our little sunshine, that are not massive enough to fuse elements heavier atomic, the most massive stars may merge atomic elements hydrogen and helium, and then go on through all the elements more heavy atomic - until a core forms of iron and nickel.
As a massive red supergiant age, they produce "onion layers" more and heavier atomic fusion elements on their nuclear-hearts. However, even massive stars can not merge the atomic elements that are heavier than . iron Indeed, no melting iron releases energy therefore, an iron core accumulates in the centers of these massive supergiant star, not nuclear fusion can occur more. - leave the stellar mass inert core nickel-iron. Because there is no longer output power, resulting in the outward pressure to counteract the pressure in the self-gravity of the star, the balance is broken - and the end is near.
Finally, the inevitable end comes when the iron core reaches the so-called Chandrasekhar limit - which is about 1.4 times the mass of our Sun. When something is this extraordinarily solid, nothing, nothing, nothing at all you can hold it against her fatal collapse.
When the core of a massive star collapses, two important things happen:
--Protons And electrons are crushed together to give rise to neutrons and neutrinos. Although not easily neutrinos interact with matter, when densities are so high, they exert enormous pressure outward.
--The Outer layers of the dying star fall inwards when the iron core collapses. When finally just collapsed core - which occurs when the neutrons begin to gather too much, in a process called degeneration of neutrons - the massive star outer gaseous layers accident condemned in the core, to recover again, sending shock wave outwardly.
These two effects - waves burst of neutrinos and clash recbound - make all the material of the star that is outside of his heart to blow in a huge explosion: a core collapse supernova type II!
Supernovae are brilliant - they are about 10 billion times brighter than our sun In fact, supernovae can briefly outshine its entire host galaxy for weeks - only a brief moment in brilliant cosmological timescales. These huge brilliant explosions tend to disappear over months or years.
A huge amount of energy is released during the explosion of a supernova. A percentage of this energy is used to merge atomic elements that are even heavier than iron. All atomic elements that are heavier than helium are called metals in the terminology used by astronomers. The origin of the heaviest atomic elements of everything-- including silver, gold, uranium and zinc - are produced in the supernova explosion itself, rather than in nuclear fusion oven to a massive star still alive.
The dead star material that gets thrown into space following the explosion of the supernova, becomes part of the interstellar medium (ISM). new fire baby stars and their attendant planets intriguing born expelled for these elderly stars in the ISM condemned material. Because the ISM has been "contaminated" by these heavy metals attacked by supernovas, planets are born of the material in the ISM contain some of these heavy atomic elements.
The collapsed stellar core also left behind by a Type II supernova, and these relics telling the tragic story of a star that was - but no more. If the basis weight is less than two or three times that of our sun becomes a neutron star. However, if more than 2 or 3 solar masses persist, nothing can contain - and collapses into a black hole of stellar mass.
There are several types of core supernovae outbursts, depending on the resulting light curve. A light curve is a graph of brightness with time after the deadly period starburst. Type II-L supernovae show a linear decrease of the light curve after the explosion. In contrast, type II-P display a much slower fall period (tea) in its light curve, which is followed by the normal breakdown. Type Ib supernovae and type Ic are the two basic forms involving a massive star supernovae, which was launched into space in its gaseous outer envelope of hydrogen and (type Ic) helium, too. The result of this is that the two types Ib and Ic supernovae appear to lack of hydrogen and helium kind.
Catch a shock Breakout
Capture images of a sudden catastrophic explosion is extremely difficult - but very useful for astronomers to understand the fundamental origin of the explosive event. However, the constant gaze of Kepler has enabled astronomers to observe, finally, a shock wave from the supernova as it reaches the surface of a massive star and sentenced to die. The crash of break lasts only a short 20 minutes, so catching this gossipy flash energy is a challenge - and an important step in the search for the team of astronomers.
"To see something that occurs on time scales of minutes, as a break from shock, you want to have a continuous sky surveillance camera. You do not know when a supernova is shutting down, and the followed Kepler has enabled us to be a witness who started the blast, "said Dr. Garnavich March 21, 2016 press release NASA.
The duo observed supernovae corresponded very well with the mathematical models Fireworks Type II supernovae - the strengthening of existing theories. However, the two explosions also unveiled what may be an unexpected variety in the individual details of the ferocious and brilliant stellar explosions.
While both explosions delivered similar energy shock, offend no leaks were detected in the smallest of the red supergiant duo. Astronomers think that is probably due to the star sentenced smaller still surrounded by gas, can be plentiful enough to wrap the shock wave when it reaches the surface of the star.
"That's the enigma of these results. Miras two supernovas and see two different things," Dr. Garnavich told the press.
Understanding the physics involved in these stellar explosions, very violent catastrophic sheds new light on how the seeds of chemical complexity and life itself were scattered through space and time in our large galaxy spiral.
"All the heavy elements in the universe come from supernova explosions. For example, all the silver, nickel and copper on Earth and even our bodies came from the explosive death throes of stars. Life exists because of the supernovae, "said Dr. Steve Howell, March 21, 2016 press release NASA. Dr. Howell's Project Scientist for the mission Kepler K2 and NASA Ames Research Center of NASA in Silicon Valley, California. K2's mission is a continuation of the original Kepler mission.
Dr. Garnavich is part of a research team known as Kepler Survey extragalactic (KITE). The team is almost complete mining information derived from the main Kepler mission, which ended in 2013 following the failure of the reaction wheels, which helped keep constant spaceship. However, with the recovery of the spacecraft called Kepler K2 NASA mission, the spacecraft had a second chance to shine. Astronomers are now sift through more data on the hunt for even supernova explosions galaxies far, far away!
"These results are a prelude to what is enticing to come from K2," said Dr. Tom Barclay published March 21, 2016 release NASA press. Dr. Barclay's principal investigator and director of the office watching invited Kepler and K2 in Ames.
In addition to Notre Dame, the team also includes BARRILETES astronomers from the University of Maryland at College Park, the Australian National University in Canberra, Australia; the Science Institute of the Space Telescope Baltimore, Maryland; and the University of California, Berkeley.
The research is scheduled for publication in The Astrophysical Journal.
Judith E. Braffman-Miller is a writer and astronomer whose articles have been published since 1981 in various magazines, newspapers and magazines. Although he writes on a variety of topics, particularly enjoys writing about astronomy because it gives you the ability to communicate to others the many wonders of their field. His first book, "Destroyed, ash and smoke," will be published soon.
http://www.annonces.immo-reve.com/
https://www.facebook.com/immo.reve.tn
Dr Garnavich and colleagues analyzed the light captured by Kepler every 30 minutes over a period of three years from 500 distant galaxies, examining some 50 billion stars. Astronomers were looking for evidence of supernovae.
In 2011, a massive star duo, known red supergiants was criticized outside while watching the Kepler. The first duo condemned giant star, nicknamed KSN 2011a, is nearly 300 times the size of our Sun, and only about 700 million light years from Earth. The second pair of tragic star named KSN 2011d, is about 500 times the size of our star and about 1.2 million light years.
"To put in perspective the size of the orbit of the Earth around our sun could fit comfortably within these colossal stars," said Dr. Garnavich in March 21, 2016 NASA press release.
Stars beat towards energy following the nuclear fusion process. Unlike our little sunshine, that are not massive enough to fuse elements heavier atomic, the most massive stars may merge atomic elements hydrogen and helium, and then go on through all the elements more heavy atomic - until a core forms of iron and nickel.
As a massive red supergiant age, they produce "onion layers" more and heavier atomic fusion elements on their nuclear-hearts. However, even massive stars can not merge the atomic elements that are heavier than . iron Indeed, no melting iron releases energy therefore, an iron core accumulates in the centers of these massive supergiant star, not nuclear fusion can occur more. - leave the stellar mass inert core nickel-iron. Because there is no longer output power, resulting in the outward pressure to counteract the pressure in the self-gravity of the star, the balance is broken - and the end is near.
Finally, the inevitable end comes when the iron core reaches the so-called Chandrasekhar limit - which is about 1.4 times the mass of our Sun. When something is this extraordinarily solid, nothing, nothing, nothing at all you can hold it against her fatal collapse.
When the core of a massive star collapses, two important things happen:
--Protons And electrons are crushed together to give rise to neutrons and neutrinos. Although not easily neutrinos interact with matter, when densities are so high, they exert enormous pressure outward.
--The Outer layers of the dying star fall inwards when the iron core collapses. When finally just collapsed core - which occurs when the neutrons begin to gather too much, in a process called degeneration of neutrons - the massive star outer gaseous layers accident condemned in the core, to recover again, sending shock wave outwardly.
These two effects - waves burst of neutrinos and clash recbound - make all the material of the star that is outside of his heart to blow in a huge explosion: a core collapse supernova type II!
Supernovae are brilliant - they are about 10 billion times brighter than our sun In fact, supernovae can briefly outshine its entire host galaxy for weeks - only a brief moment in brilliant cosmological timescales. These huge brilliant explosions tend to disappear over months or years.
A huge amount of energy is released during the explosion of a supernova. A percentage of this energy is used to merge atomic elements that are even heavier than iron. All atomic elements that are heavier than helium are called metals in the terminology used by astronomers. The origin of the heaviest atomic elements of everything-- including silver, gold, uranium and zinc - are produced in the supernova explosion itself, rather than in nuclear fusion oven to a massive star still alive.
The dead star material that gets thrown into space following the explosion of the supernova, becomes part of the interstellar medium (ISM). new fire baby stars and their attendant planets intriguing born expelled for these elderly stars in the ISM condemned material. Because the ISM has been "contaminated" by these heavy metals attacked by supernovas, planets are born of the material in the ISM contain some of these heavy atomic elements.
The collapsed stellar core also left behind by a Type II supernova, and these relics telling the tragic story of a star that was - but no more. If the basis weight is less than two or three times that of our sun becomes a neutron star. However, if more than 2 or 3 solar masses persist, nothing can contain - and collapses into a black hole of stellar mass.
There are several types of core supernovae outbursts, depending on the resulting light curve. A light curve is a graph of brightness with time after the deadly period starburst. Type II-L supernovae show a linear decrease of the light curve after the explosion. In contrast, type II-P display a much slower fall period (tea) in its light curve, which is followed by the normal breakdown. Type Ib supernovae and type Ic are the two basic forms involving a massive star supernovae, which was launched into space in its gaseous outer envelope of hydrogen and (type Ic) helium, too. The result of this is that the two types Ib and Ic supernovae appear to lack of hydrogen and helium kind.
Catch a shock Breakout
Capture images of a sudden catastrophic explosion is extremely difficult - but very useful for astronomers to understand the fundamental origin of the explosive event. However, the constant gaze of Kepler has enabled astronomers to observe, finally, a shock wave from the supernova as it reaches the surface of a massive star and sentenced to die. The crash of break lasts only a short 20 minutes, so catching this gossipy flash energy is a challenge - and an important step in the search for the team of astronomers.
"To see something that occurs on time scales of minutes, as a break from shock, you want to have a continuous sky surveillance camera. You do not know when a supernova is shutting down, and the followed Kepler has enabled us to be a witness who started the blast, "said Dr. Garnavich March 21, 2016 press release NASA.
The duo observed supernovae corresponded very well with the mathematical models Fireworks Type II supernovae - the strengthening of existing theories. However, the two explosions also unveiled what may be an unexpected variety in the individual details of the ferocious and brilliant stellar explosions.
While both explosions delivered similar energy shock, offend no leaks were detected in the smallest of the red supergiant duo. Astronomers think that is probably due to the star sentenced smaller still surrounded by gas, can be plentiful enough to wrap the shock wave when it reaches the surface of the star.
"That's the enigma of these results. Miras two supernovas and see two different things," Dr. Garnavich told the press.
Understanding the physics involved in these stellar explosions, very violent catastrophic sheds new light on how the seeds of chemical complexity and life itself were scattered through space and time in our large galaxy spiral.
"All the heavy elements in the universe come from supernova explosions. For example, all the silver, nickel and copper on Earth and even our bodies came from the explosive death throes of stars. Life exists because of the supernovae, "said Dr. Steve Howell, March 21, 2016 press release NASA. Dr. Howell's Project Scientist for the mission Kepler K2 and NASA Ames Research Center of NASA in Silicon Valley, California. K2's mission is a continuation of the original Kepler mission.
Dr. Garnavich is part of a research team known as Kepler Survey extragalactic (KITE). The team is almost complete mining information derived from the main Kepler mission, which ended in 2013 following the failure of the reaction wheels, which helped keep constant spaceship. However, with the recovery of the spacecraft called Kepler K2 NASA mission, the spacecraft had a second chance to shine. Astronomers are now sift through more data on the hunt for even supernova explosions galaxies far, far away!
"These results are a prelude to what is enticing to come from K2," said Dr. Tom Barclay published March 21, 2016 release NASA press. Dr. Barclay's principal investigator and director of the office watching invited Kepler and K2 in Ames.
In addition to Notre Dame, the team also includes BARRILETES astronomers from the University of Maryland at College Park, the Australian National University in Canberra, Australia; the Science Institute of the Space Telescope Baltimore, Maryland; and the University of California, Berkeley.
The research is scheduled for publication in The Astrophysical Journal.
Judith E. Braffman-Miller is a writer and astronomer whose articles have been published since 1981 in various magazines, newspapers and magazines. Although he writes on a variety of topics, particularly enjoys writing about astronomy because it gives you the ability to communicate to others the many wonders of their field. His first book, "Destroyed, ash and smoke," will be published soon.
http://www.annonces.immo-reve.com/
https://www.facebook.com/immo.reve.tn
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