An international team of astronomers used ALMA to capture high-resolution images of eight protoplanetary disks in the Sigma Orionis cluster, which is irradiated by intense ultraviolet light from a massive nearby star. To their surprise, they found evidence of gaps and rings in most of the disks—structures commonly associated with the formation of giant planets, like Jupiter.
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Rings of dust surrounding HL Tauri, with line patterns showing the orientation of polarized light. A new paper published by Stephens, et al., using ALMA, provides the deepest dust polarization image of any protoplanetary disk captured thus far, revealing details about the dust grains in the disk. Credit: NSF/AUI/NRAO/B. Saxton/Stephens et al.
Highest Resolution Dust Polarization Image Ever Taken Toward a Protoplanetary Disk
One of the primary goals of the Atacama Large Millimeter/submillimeter Array (ALMA) is to study the formation and evolution of planetary systems. Young stars are often surrounded by a disk of gas and dust, out of which planets can form. One of the first high resolution images that ALMA captured was of HL Tauri, a young star just 480 light-years away surrounded by a protoplanetary disk. The disk has visible gaps which could be where young protoplanets are forming. Planetary formation is a complex process that we still don’t fully understand. During this process, dust grains in the disk are growing in size as they collide and stick to each other, causing them to slowly grow to potentially become objects similar to those within our solar system.
One of the ways to study dust grains in these complex structures is to look at the orientation of the light waves they emit, which is known as polarization. Earlier studies of HL Tauri have mapped this polarization, but a new study from Stephens, et al. has captured a polarization image of HL Tauri in unprecedented detail. The resulting image is based on 10x more polarization measurements than of any other disk, and 100x more measurements than most disks. It is by far the deepest polarization image of any disk captured thus far, according to research published today in Nature.
The image was captured at a resolution of 5 AU, which is about the distance from the Sun to Jupiter. Previous polarization observations were at a much lower resolution and didn’t reveal the subtle patterns of polarization within the disk. For example, the team found the amount of polarized light to be greater on one side of the disk than the other, which is likely due to asymmetries in the distribution in the dust grains or their properties across the disk. Dust grains aren’t often spherical. They can be oblate like a thick pancake, or prolate like a grain of rice. When light is emitted by or scatters off these dust grains, it can become polarized, meaning that the waves of light are oriented in a particular direction rather than just randomly. These new results suggest that grains behave more like prolate grains, and they put strong constraints on the shape and size of dust grains within the disk.
A surprising result of the study is that there is more polarization within the gaps of the disk than the rings, even though there is more dust in the rings. The polarization within the gaps is more azimuthal, which suggests the polarization comes from aligned dust grains within the gaps. The polarization of the rings is more uniform, suggesting the polarization largely comes from scattering. In general, the polarization comes from a mix of scattering and dust alignment. Based on the data, it is unclear what is causing the dust grains to align, but they are likely not aligned along the magnetic field of the disk, which is the case for most dust outside of protoplanetary disks. Currently, it is thought that the grains are aligned mechanically, perhaps by their own aerodynamics, as they revolve around the central young star.
What will studies of HL Tau reveal next? This new publication makes clear that high resolution is needed for polarization observations to learn the details about the dust grains. As the world’s most powerful millimeter/ submillimeter telescope, ALMA will be a fundamental instrument for continuing this research.
About ALMA & NRAO
The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of the European Organisation for Astronomical Research in the Southern Hemisphere (ESO), the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile. ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada (NRC) and the Ministry of Science and Technology (MOST) and by NINS in cooperation with the Academia Sinica (AS) in Taiwan and the Korea Astronomy and Space Science Institute (KASI).
ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory (NRAO), managed by Associated Universities, Inc. (AUI), on behalf of North America; and by the National Astronomical Observatory of Japan (NAOJ) on behalf of East Asia. The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.
NRAO is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.
Media Contact
Jill Malusky, NRAO & GBO News & Public Information Manager
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This news article was originally published on the NRAO website on November 15, 2023.
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