Three-dimensional Magnetic field in a protoplanetary disk

Three-dimensional Magnetic field in a protoplanetary disk | Research Square window.SnipcartSettings = { analytics: { enabled: false } }; (function() { var accessVector = localStorage.getItem('access_vector') || ''; window.dataLayer = window.dataLayer || []; if (accessVector) { window.dataLayer.push({ user: { profile: { profileInfo: { snid: accessVector } } } }); } })(); (function(w,d,s,l,i){w[l]=w[l]||[];w[l].push({'gtm.start':new Date().getTime(),event:'gtm.js'});var f=d.getElementsByTagName(s)[0],j=d.createElement(s),dl=l!='dataLayer'?'&l='+l:'';j.async=true;j.src='https://www.googletagmanager.com/gtm.js?id='+i+dl;f.parentNode.insertBefore(j,f);})(window,document,'script','dataLayer','GTM-K279D39R'); Browse Preprints In Review Journals COVID-19 Preprints AJE Video Bytes Research Tools Research Promotion AJE Professional Editing AJE Rubriq About Preprint Platform In Review Editorial Policies Our Team Advisory Board Help Center Sign In Submit a Preprint Cite Share Download PDF Article Three-dimensional Magnetic field in a protoplanetary disk Satoshi Ohashi, Takayuki Muto, Yusuke Tsukamoto, Akimasa Kataoka, and 4 more This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-4303060/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 05 Feb, 2025 Read the published version in Nature Astronomy → Version 1 posted You are reading this latest preprint version Abstract In protoplanetary disks around young stars, magnetic fields play an important role for disk evolution and planet formation [1-3]. Polarized thermal emission from magnetically aligned grains is one of the reliable methods to trace magnetic fields [4,5]. However, it has been difficult to observe magnetic field by dust polarization in protoplanetary disks because other polarization mechanisms involving grown dust grains become efficient [6,7,8]. Here, we report muti-wavelengths (0.87 mm, 1.3 mm, 2.1 mm, and 2.7 mm) observations of polarized thermal emission in the protoplanetary disk around HD 142527 that shows the lopsided dust distribution [9,10,11,12]. We revealed that the smaller dust still exhibits magnetic alignment in the southern part of the disk. Furthermore, angular offsets between the observed magnetic field and the disk azimuthal direction were discovered, which can be used for a novel approach to measure the relative strengths of each component (radial (B r ), azimuthal (B ∅ ), and vertical (B z )) of 3D magnetic field. Applying this method, we, for the first time, derived the magnetic field around a 200-au radius from the protostar as |B r |:|B ∅ |:|B z | ~ 0.26±0.01:1:0.23±0.03 and a strength of ~ 0.3 milli Gauss. Our observations provide some key parameters of magnetic activities including the plasma beta, which have been only assumed in theoretical studies. In addition, the radial and vertical angular momentum transfer show comparable, which poses a challenge to theoretical studies of protoplanetary disks. Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Astrophysical magnetic fields Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Astrophysical disks Physical sciences/Astronomy and planetary science/Astronomy and astrophysics/Astrophysical dust Full Text Additional Declarations There is NO Competing Interest. Cite Share Download PDF Status: Published Journal Publication published 05 Feb, 2025 Read the published version in Nature Astronomy → Version 1 posted You are reading this latest preprint version Research Square lets you share your work early, gain feedback from the community, and start making changes to your manuscript prior to peer review in a journal. As a division of Research Square Company, we’re committed to making research communication faster, fairer, and more useful. We do this by developing innovative software and high quality services for the global research community. Our growing team is made up of researchers and industry professionals working together to solve the most critical problems facing scientific publishing. Also discoverable on Platform About Our Team In Review Editorial Policies Advisory Board Help Center Resources Author Services Accessibility API Access RSS feed Manage Cookie Preferences © Research Square 2026 | ISSN 2693-5015 (online) Privacy Policy Terms of Service Do Not Sell My Personal Information {"props":{"pageProps":{"initialData":{"identity":"rs-4303060","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Article","associatedPublications":[],"authors":[{"id":310550362,"identity":"1da2c1eb-aa4c-4506-bf91-ecd94503506f","order_by":0,"name":"Satoshi 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Polarized thermal emission from magnetically aligned grains is one of the reliable methods to trace magnetic fields [4,5]. However, it has been difficult to observe magnetic field by dust polarization in protoplanetary disks because other polarization mechanisms involving grown dust grains become efficient [6,7,8]. Here, we report muti-wavelengths (0.87 mm, 1.3 mm, 2.1 mm, and 2.7 mm) observations of polarized thermal emission in the protoplanetary disk around HD 142527 that shows the lopsided dust distribution [9,10,11,12]. We revealed that the smaller dust still exhibits magnetic alignment in the southern part of the disk. 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