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Protoplanetary disk formation in rotating, magnetized and turbulent … The rotation, magnetic field and turbulence of the central protostar is triggering the growth of the surrounding disk mass and angular momentum of the protoplanetary disk. Though, if magnetic field of the protoplanetary disk is getting stronger, it will hinder the disk mass growth through stopping (reducing) the infalling of matter from the envelop to the protoplanetary disk.
URL: [Springer Link](https://link.springer.com/article/10.1007/s12036-023-09960-w)
Formation and evolution of a protoplanetary disk: Combining … The small disk sizes, detections of magnetic fields at all scales in protostellar cores (Galametz et al. 2018; Huang et al. 2024), and comparison of disk observations to predictions from magnetized models (Maury et al. 2018; Lebreuilly et al. 2024; Yen et al. 2024) all suggest a disk formation scenario where magnetic fields in protostellar cores regulate the early evolution of the disk sizes.
URL: [A&A](https://www.aanda.org/articles/aa/full_html/2024/11/aa51388-24/aa51388-24.html)
Magnetic fields in protoplanetary disks | Astrophysics and … – Springer Magnetic fields likely play a key role in the dynamics and evolution of protoplanetary disks. They have the potential to efficiently transport angular momentum by MHD turbulence or via the magnetocentrifugal acceleration of …xt”>
Planets form in turbulent disks of gas and dust called protoplanetary disks around young stars. It is thought that the first step in planet formation is dust grains colliding and sticking together. The movement of the dust grains is influenced by many forces, including magnetism. thus, understanding the magnetic fields is important for understanding planet formation, but so far it has not been possible to measure the magnetic fields in a protoplanetary disk.
In this research, an international team of astronomers led by Satoshi Ohashi at the National Astronomical observatory of Japan used the Atacama Large Millimeter/submillimeter Array (ALMA) to observe the protoplanetary disk around a young star known as HD 142527. This star is located 512 light-years away in the direction of the constellation Lupus. The team found that the dust grains aligned with the magnetic field lines.This allowed the team to detect and measure the unseen magnetic field lines, much the same way iron filings can reveal the magnetic field around a magnet. The team thinks that the measured three-dimensional structure might create strong turbulence withing the protoplanetary disk.
Now that this method of dusting for a young star’s magnetic fingerprint has been proven to work, the team wants to apply it to more stars, and measure the magnetic field closer to the star to better understand the magnetic conditions where planets are forming.
interview with Astrophysicist on Protoplanetary Disk Formation
Editor: Can you elaborate on how rotational and magnetic forces influence the formation of protoplanetary discs? Is this something that has been recently studied?
Astrophysicist: Indeed, the interplay between rotation, magnetic fields, and turbulence is crucial in the formation of protoplanetary discs. Recent studies, such as those published in journal articles, suggest that the rotation of the central protostar triggers the growth of the surrounding disc by transferring mass and angular momentum to the disc. However, if the magnetic field of the protoplanetary disc strengthens excessively, it can hinder this process by reducing the infall of matter from the enveloping material. So,magnetic fields play a dual role—facilitating and obstructing disc formation depending on their intensity.
Editor: Could you clarify what happens during the early stages of the disk’s evolution, especially regarding the influence of magnetic fields?
Astrophysicist: During the early evolution of protoplanetary discs, magnetic fields in protostellar cores regulate the sizes of these discs. Observations and comparisons to magnetized models suggest that magnetic fields at various scales in protostellar cores significantly impact the disk formation process. By managing the early evolution,magnetic fields ensure that the disc sizes align with theoretical predictions,providing a framework for subsequent planetary formation.
editor: What is the meaning of detecting magnetic fields in protoplanetary discs, especially in young stellar environments like Lupus?
Astrophysicist: Detecting magnetic fields in protoplanetary discs is critical because these fields influence the dynamics and evolution of the discs. Research indicates that magnetic fields can efficiently transport angular momentum, thereby influencing the overall stability and structure of the disc. In the Lupus region, research teams have used aligned dust grains to detect and measure magnetic field lines. This method allows us to visualize the magnetic field,somewhat akin to using iron filings to reveal magnetic lines around a magnet. This detection can indicate strong turbulence within the disc, affecting where and how planetary bodies form.
Editor: How does understanding the magnetic fields near young stars improve our knowledge of planet formation?
Astrophysicist: By measuring the magnetic fields closer to young stars, we gain insight into the magnetic conditions prevalent during planet formation. These conditions influence the distribution and motion of dust and gas, which are the initial building blocks of planets. Understanding these magnetic environments helps us refine theories on planetary formation and the subsequent evolution of solar systems.
Concluding Remarks
The interviews and research highlight the pivotal role magnetic fields play in both facilitating and constraining the formation and evolution of protoplanetary discs. By managing the infall of material and transporting angular momentum, magnetic fields shape the early stages of disc formation. Recent advancements in detecting and measuring these fields provide valuable insights into the turbulence and conditions where planets begin to take shape. This line of research is crucial for a thorough understanding of planet formation and the overall evolution of solar systems.
