New insights into the formation of brown dwarfs

Brown dwarfs are strange bodies that are between stars and planets. Failure stars are sometimes called 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 888-353-1299 It is debated if the formation of brown dwarfs is a scaled-down version of the formation of Sun-like stars. Proto-brown dwarfs are the youngest brown dwarfs. They are a few thousand years old and still in the early stages of formation. They want to know if the gas and dust in these dwarfs are similar to the youngest Sun-like stars.

M methane is a stable gas molecule that can only be destroyed by high-energy physical processes. It has been found on a number of planets. Methane has been used in the past to identify and study the properties of the oldest brown dwarfs, which are hundreds of million to billions of years old.

A team led by LMU astrophysicist Basmah Riaz has detected deuterated methane in three brown dwarfs. It is the first time that CH 3 D has been detected outside the solar system. This is not a normal result.

Proto-brown dwarfs are very dense. They are difficult to study for methane signatures. They can be seen in the millimeter wave range. Deuterated methane (CH 3 D) can be observed at millimeter wavelength because of its symmetry.

According to the theories on brown dwarf formation, brown dwarfs are cooler and denser than stars. CH 3 D is preferentially formed when the gas is warm, i.e., around 20 to 30Kelvin. Scientists can use the CH 3 D abundance measurement to estimate methane abundance.

The LMU Team has detected CH 3 D in 3 proto-brown dwarfs, which is surprising since there is only one Sun-like star known to date. The cool compact astrophysical objects may not be simply a scaled-down replica of the stars, because they exhibit a rich warm organic chemistry.

Wing-Fai Thi of the Max Planck Institute for Extraterrestrial Physics says that the methane in the brown dwarfs may or may not survive. Since a warm environment is favorable for forming more complex molecules, brown dwarfs are intriguing objects to look for in the future.

More information: B Riaz et al, First CH₃D detection in Class 0/I proto-brown dwarfs: constraints on CH₄ abundances, Monthly Notices of the Royal Astronomical Society: Letters (2022). DOI: 10.1093/mnrasl/slac007 Citation: New insights into the formation of brown dwarfs (2022, February 18) retrieved 18 February 2022 from https://phys.org/news/2022-02-insights-formation-brown-dwarfs.html This document is subject to copyright. Apart from any fair dealing for the purpose of private study or research, no part may be reproduced without the written permission. The content is provided for information purposes only.