Because stars and planets consist of clouds of decaying gas and dust in space, ISM that spreads can be considered a starting point for chemical processes that will ultimately lead to the formation of planets and life, Martin Koningar of Washington Catholic University said.
Full identification of content so as to provide information about available stars and planets. The coordinator, at the Nadal Space Flight Center in Greenbelt, Maryland, is the lead author of this research report, published on April 22 in the astrophysics journal.
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The molecule identified by Cordiner and his team is a carbon form known as buckminsterfullerene, also known as buckyballs, which consists of 60 carbon atoms, C60, which are arranged in hollow balls. C60 is found in rocks and minerals in some cases that are rare on earth and can also occur at high combustion temperatures
C60 has been seen in space. However, this is the first time that it has been confirmed that there is a diffuse (ionized) version of electrically charged ISM. C60 is ionized when ultraviolet light, which from the stars of an electron from a molecule breaks down the positive charge C60 (C60 +).
The diffuse ISM in the past is considered too rough and too weak to produce large numbers of large molecules, Cordiner said. “Before the discovery of C60, the largest known molecule in the space size was only 12 atoms. Confirmation of our C60 + showed how the astrohimiya complex itself could be in UV protection in the galaxy.
Life, as we know, is based on carbon molecules, and these findings show that complex carbon molecules can form and survive in interstellar harsh environments. “On the one hand, life can be considered the highest in chemical complexity,” Cornir said. “The presence of C60 clearly shows the high level of chemical complexity involved in the space environment, and shows the possibility that even more complex carbon molecules that naturally occur in space.
Most ISMs are made of hydrogen and helium, but there are many compounds that cannot be identified. With so far interstellar space, scientists learned how to manipulate distant starlight to identify its contents.
When starlight falls through space, elements and compounds in ISM absorb and block certain colors wavelengths of light. When scientists analyze starlight by dividing it into composite colors spectrum the absorbed color seems unclear or absent. Each element or compound has a unique absorption pattern that acts as a fingerprint and allows identification.
However, some models of ISM absorption cover a wider range of colors than atoms or molecules known on earth. This absorption pattern is referred to as Diffuse Interstitial Strips DIBs. Their identity remained a mystery when they were discovered by Mary Li Heger, who published observations from the first two DIBs in 1922.
DIB can be assigned to find the right match with traces of absorption of a particular substance in the laboratory. However, there are millions of different molecular structures so it will require a lot of life to test everything.