In expansion to solo stars like the sun, the universe contains binary star systems including two gigantic stars that connect with each other. In numerous binaries, the two stars are sufficiently close to trading matter and may even union, delivering a solitary high-mass star that twists at extraordinary speed. Up to this point, the quantity of known high-mass binaries has been little, fundamentally limited to those distinguished in the galaxy which is the Milky Way.
As written in Phys.org, a research has identified and characterized 82 new high-mass binaries in the binary star systems which are located in the Tarantula Nebula in the Large Magellanic Cloud. Tarantula Nebula is also known as 30 Doradus. The Large Magellanic Cloud is located about 160,000 light years away from earth and is a satellite galaxy of the Milky way.
The research survey for the binary star systems was led by the scientists at the University of Sao Paulo's Institute of Astronomy, Geophysics and Atmospheric Sciences (IAG-USP) located in Brazil. The research paper and the results of the study are published in the journal Astronomy & Astrophysics. The research was supervised by a professor at IAG, who is also the co-author of the article journal, named Augusto Damineli Neto.
Science News Line reported that researchers broke down the information acquired amid the VLT-FLAMES Tarantula Survey and Tarantula Massive Binary Monitoring perception campaigns performed by the European Southern Observatory (ESO) from 2011 for binary star systems. Utilizing FLAMES/GIRAFFE, a spectrograph coupled to ESO's Very Large Telescope (VLT), which has four 8m essential mirrors and works in Chile's Atacama Desert, the perception gathered ghastly information for more than 800 high-mass objects in the area of the Tarantula Nebula.
With the help of the gathered 800 high mass objects, scientists working on the two surveys high mass binary star systems also identified 100 candidate binaries of spectral type O, which is considered to be very hot and huge in size, within a sample of 360 stars. The sample was based on parameters, for example, the amplitude of varieties in their spiral speed (the speed of movement from or toward an observer).
