Study reveals diverse magnetic fields in solar-type star-forming cores


IMAGE: Core-scale magnetic fields (red sectors) presumed utilizing high-resolution and delicate dust emission polarization observations utilizing JCMT. The Solar-type star forming cores fragmented out of B213 filament are revealed….
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Credit: Eswaraiah Chakali, et al. 2021

Magnetic fields are common throughout our Milky Way Galaxy and play an essential function in all characteristics of interstellar medium. However, concerns like how Solar-type stars form out of allured molecular clouds, whether the function of magnetic fields modifications at different scales and densities of molecular clouds, and what aspects can alter the morphology of magnetic fields in low-mass thick cores still stay uncertain.

A brand-new study led by Dr. Eswaraiah Chakali from Prof. LI Di’s research study group at the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC) has actually partly responded to these concerns. The study reveals the diverse magnetic field morphologies in Solar-type star forming cores in the Taurus B213 area.

This study was released in The Astrophysical Journal Letters on May 10.

The scientists utilized high-resolution and delicate 850-micron dust emission polarization information obtained by the James Clerk Maxwell Telescope (JCMT) utilizing the SCUBA-2 video camera in addition to the POL-2 polarimeter.

The observations were carried out as a part of a big global program called B-fields In STar-forming Region Observations (BISTRO).

“Although formed out of the same filamentary cloud, Taurus/B213, among the three dense cores having more polarization measurements, only one remembers the relatively uniform large-scale magnetic field threading the parental cloud,” stated Dr. Eswaraiah Chakali, lead author of the study.

This is in contrast to expectations based upon the theory that magnetic fields control star development. If a massive magnetic field controls throughout cloud build-up, core collapse and star development, the mean position angle of the magnetic field must be comparable throughout different spatial scales.

Further analysis of the gas speed gradient exposed that the kinematics due to gas accretion streams onto the adult filament might have modified the magnetic field setup.

“Even in the presence of substantial magnetic flux, local physical conditions can significantly affect magnetic field morphology and their role in star formation,” stated Prof. LI Di, co-corresponding author of the study.

“Our current observations represent one of the deepest sub-millimeter polarimetry images ever taken using a single dish telescope toward a Galactic region,” stated Prof. QIU Keping of Nanjing University, co-PI of the BISTRO job and a coauthor of the study.

Prof. LI Di likewise highlighted “more comprehensive analyses, in combination with Planck data and stellar polarimetry, may give more insights into the evolution of magnetic fields in this stereotypical low-mass star-forming region.”


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