Eta Carinae Star:
Eta Carinae Star system does not lack the highest level. It not only contains one of the largest and brightest stars in our galaxy, they occupy at least 90 times the mass of the sun, it is also very volatile, is expected in the future at least one supernova explosion.
As the first object observed by NASA’s Chandra X-ray Observatory after about 15 years of transmission, the binary system continues to reveal new clues about its nature through its resulting X-rays.
Astronomers have reported the extremely destabilizing behavior of the nineteenth century Ita Carina, and for twenty years it has become very bright, surpassing almost every star in the sky. This event is called “big outbreak”. Data from the modern telescope showed that Eta Carinas threw ten times the quality of the sun during that time. Surprisingly, the planet survived this turbulent material expulsion, adding an “extremely strong” list of attributes.
Today, astronomers are trying to learn more about the two stars in the Eta Carinae system and how they interact. The heavier one of the two stars is rapidly losing quality by air flow at speeds of more than one million miles per hour. Although it is not a huge outbreak of the outbreak, this star is still at a very high rate of loss of quality, which will accumulate in the millennium to the quality of the sun. Eta Carinae Star Eta Carinae Star
While smaller than its partner, the companion in Eta Carinae is also huge, weighing about 30 times the weight of the sun. It is losing material at a rate a hundred times faster than his partner, but it is still a huge weight loss compared to most other stars. Accompanied by the stars beat the wind more stars, the wind speed ten times faster.
When these two fast and powerful winds collide, they form a bow impact – similar to the sound of the Sonics’ roar and then heat the gas between the stars. The temperature of the gas reaches about ten million degrees, resulting in X-rays detected by Chandra.
Eta Carinae’s Chandra images show red low-energy X-rays, green X-rays, and blue high-energy X-rays. Most of the emissions come from low energy and high-energy X-rays. The blue dot source is generated by the collision wind, and the diffuse blue emission occurs when the material that is cleared during the eruption reflects these X-rays. The low-energy X-rays further show the wind from two stars or the material from the outburst in the surroundings. This surrounding material may include the gas that was ejected before the outbreak. Eta Carinae Star Eta Carinae Star Eta Carinae Star
An interesting feature of the Eta Carina system is that the two stars travel around each other along a highly elliptical path over a five-and-a-half long orbit. Depending on the position of each star on its oval trajectory, the distance between the two stars changes by 20 times. These oval trajectories give astronomers an opportunity to study what happens when they collide with different distances from each other. Eta Carinae Star
In most of the whole system, the X-ray is stronger at the vertex, that is, the area of wind collision. However, when two stars are closest to their orbital (they are the point where the astronomer calls it “the surrounding stars”), the X-ray emission unexpectedly drops.
To understand this tilting reason, astronomers were observed around the beginning of 2009 with Chandra’s Eta Carinae. These results provide the first detailed picture of the X-ray emission of the collision wind at Eta Carina. Studies have shown that subsidence in the surrounding area is partly due to the fact that the X-rays from the vertices are blocked by dense winds from the larger mass of the Eta Carinae, or may be blocked by the surface of the star itself.
Another factor that causes the X-ray dip is that the shock wave appears to be destroyed at the neighboring circumference, possibly because of the faster cooling of the gas due to the increase in density and/or the intensity of the wind accompanying the star due to the extra ultraviolet radiation from The supernova arrive at it. Researchers hope that Chandra observes the latest peripheral nervous system in August 2014 will help them determine the true explanation.
These results were published in the April 1, 2014, issue of the journal Astrophysics, available online. The first author of this paper is Kenji Hamaguchi of the Goddard Space Center, at Greenbelt, MD, whose collaborators are Michael Kokolen of the Goddard Space Flight Center (GSFC); Christopher of the University of Delaware Russell is a freak from the European Space Agency in Madrid, Spain; Theodore Gore, Marian Teodoro and Thomas I. Madura from the GSFC; Augusto Damineli from the University of Sao Paulo, Sao Paulo, Brazil, and from the University of Leeds Julian Pittard.
Image Source: NASA / CXC / GSFC / K.Hamaguchi, et al.
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