There are giant clouds of gas and dust calledmolecular clouds. How that happens is explained by the nebular hypothesis. Clouds of hydrogen collapse due to instability according to that hypothesis. The basic idea is what the Nebular Hypothesis is all about.
It doesn't explain how single stars form. Half of the stars are multiple stars. There isn't a clear explanation of how those stars form.
Most stars that are the same size as our Sun are not single stars. The majority of them are members of multiple star systems. There are differing theories on how stars form.
A circumstellar disk is formed after a molecular cloud collapses into a star. A theory says that a pair or more of young stars are fragments of a bigger disk. One theory says that the young stars form independently and one captures the other.
Stars begin with a dense core inside a cloud. A star is formed when enough gas is gathered in one place to make a star. What are the differences between multiple stars and single stars?
Astronomers at Hawaii's James Clerk Maxwell Telescope wanted to know what that was.
There is a radio telescope at the observatory. The telescope can see where stars are born. The closest active stellar nursery to Earth is the OMC, which is 1500 light years away. Observations from ALMA and the Nobeyama Telescope were used.
The team made important discoveries while watching multiple star systems form. They presented their findings in a journal. The paper looks at how dense core properties affect the multiplicity of stars. The author is a student at the observatory.
One or several Protostars can form within a single gas core during the transition phase from a prestellar to a cloud core. The physical processes of this transition are not clear.
The team of researchers collected observations of 43 core in the cloud. They used the ALMA telescope to look at the interior of the core.
The majority of the dense cores form only single stars. The size and mass of the core were estimated by the astronomer. They found that the densities and mass of the multiple cores are the same.
The author said it was understandable. The self-gravity inside the core makes fragmenting easier.
The Nobayama radio telescope is located in Japan. The N2H+ J=1-0 line is found in all the dense cores. One of the first ion found in clouds is N2H+. It is easy to observe this line through the atmosphere. It's used to map the density and velocity of the gas.
The observations show that dense stars are more turbulent than single stars.
The Nobeyama observations can be used to measure turbulence levels. The Nobeyama observations show that stars form in more turbulent cores.
The study findings were summarized by the lead author. We found that stars form in denser and more turbulent core in this study.
The JCMT is a great tool for uncovering stellar nurseries for ALMA follow ups. With ALMA giving unprecedented sensitivity and resolution, we can do similar studies to a much sample of larger dense cores for a more thorough understanding of star formation.
The stars in each arrangement are at different stages in their evolution. Younger protostars are closer to the center of the dense cores than the more evolved ones. As stars evolve, they move out of their core.
There are differences between single stars and multiple stars. There is more to be learned and more questions.
Magnetic fields play a role in the formation of stars. Clouds that are star-forming can be magnets. Astronomers know that magnetic fields can affect the formation of stars. Are they involved in determining if a single star forms or multiple stars?
The lead for the ALMA observations said that they had yet to look at the effect of magnetic fields. The next stage of our research is focused on magnetic field suppression in dense cores, so we are excited to use the jctt.
The low sample size makes it hard for the authors to get the results they want. Forty-three dense cores aren't enough to draw conclusions because they're all from the same cloud The study was limited by the various telescopes used in it.
Their conclusion is that the results could be further tested using future higher spatial andspectral resolution observations towards a more complete dense core sample in different environments.
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