Astronomers used the Subaru Telescope to observe a disk around the young star RY Tau, finding that a “fluffy” layer above the disk appears to be a remnant of material from an earlier phase of stellar and disk development.
An international team of astronomers that are members of the Strategic Exploration of Exoplanets and Disks with Subaru Telescope (SEEDS) Project has used Subaru Telescope’s High Contrast Instrument for the Subaru Next Generation Adaptive Optics (HiCIAO) to observe a disk around the young star RY Tau (Tauri). The team’s analysis of the disk shows that a “fluffy” layer above it is responsible for the scattered light observed in the infrared image. Detailed comparisons with computer simulations of scattered light from the disk reveal that this layer appears to be a remnant of material from an earlier phase of stellar and disk development, when dust and gas were falling onto the disk.
Since 2009, the five-year SEEDS Project (Note) has focused on direct imaging of exoplanets, i.e., planets orbiting stars outside of our Solar System, and disks around a targeted total of 500 stars. Planet formation, an exciting and active area for astronomical research, has long fascinated many scientists. Disks of dust and gas that rotate around young stars are of particular interest, because astronomers think that these are the sites where planets form— in these so-called “protoplanetary disks.” Since young stars and disks are born in molecular clouds, giant clouds of dust and gas, the role of dust becomes an important feature of understanding planet formation; it relates not only to the formation of rocky, Earth-like planets and the cores of giant Jupiter-like planets but also to that of moons, planetary rings, comets, and asteroids.
As a part of the SEEDS Project, the current team of researchers used HiCIAO mounted on the Subaru Telescope to observe a possible planet-forming disk around the young star RY Tau. This star is about 460 light years away from Earth in the constellation Taurus and is around half a million years old. The disk has a radius of about 70 AU (10 billion kilometers), which is a few times larger than the orbit of Neptune in our own Solar System.
Astronomers have developed powerful instruments to obtain images of protoplanetary disks, and Subaru Telescope’s HiCIAO is one of them. HiCIAO uses a mask to block out the light of the central star, which may be a million times brighter than its disk. They can then observe light from the star that has been reflected from the surface of the disk. The scattered light will reveal the structure of the surface of the disk, which is very small in scale and difficult to observe, even with large telescopes. Observers use HiCIAO with a 188 element adaptive optics system to reduce the blurring effects of the Earthʼs atmosphere, making the images significantly sharper.
This team succeeded in capturing a near-infrared image (1.65 μm) associated with the RY Tau disk. Unlike many other protoplanetary disks, the disk emission is offset from the center of the star (Figure 2, left). In contrast to longer wavelength observations, which are associated with the midplane of the disk, near-infrared, scattered light coming from the surface of the disk produced this offset (Figure 2, right), which provides information about the vertical structure of the disk.
Changes in structure perpendicular to the surface of a disk are much harder to investigate because there are few good examples to study. Therefore, the information about vertical structure that this image provides is a contribution to understanding the formation of planets, which depends strongly on the structure of the disk, including structures such as spirals and rings, as well as height.
The team performed extensive computer simulations of the scattered light, for disks with different masses, shapes, and types of dust (Figure 3). They found that the scattered light is probably not associated with the main surface of the disk, which is the usual explanation for the scattered light image (Figure 4a). Instead, the observed infrared emission can be explained if the emission is associated with a fluffy upper layer, which is almost transparent and not completely transparent (Figure 4b). The team estimated the dust mass in this layer to be about half the mass of Earthʼs Moon.
Why is this fluffy layer observed in this disk, but not in many other possible planet-forming disks? The team suspects that this layer is a remnant of the dust that fell onto the star and the disk during earlier stages of formation. In most stars, unlike RY Tau, this layer dissipates by this stage in the formation of the star, but RY Tau may still have it because of its youth. It may act as a special comforter to warm the inside of the disk for baby planets being born there. This may affect the number, size, and composition of the planets being born in this system.
The Atacama Large Millimeter/Submillimeter Array (ALMA), a superb international millimeter/submillimeter telescope, will soon be making extensive observations of protoplanetary disks, which will allow scientists to directly observe ongoing planet formation in the midplane of a disk. By comparing SEEDS and ALMA observations scientists may be able to understand the details of how planets form, something that has raised fascinating questions for centuries.
The SEEDS Project began in 2009 for a five-year period, using 120 observing nights at Subaru Telescope, located at the summit of Mauna Kea on the island of Hawaii. The goal of the project is to explore hundreds of nearby stars in an effort to directly image extrasolar planets and protoplanetary/debris disks that surround less massive stars like the Sun. Principal investigator Motohide Tamura (University of Tokyo and NAOJ) leads the project.
Reference: “High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk around RY Tau” by Michihiro Takami, Jennifer L. Karr, Jun Hashimoto, Hyosun Kim, John Wisniewski, Thomas Henning, Carol A. Grady, Ryo Kandori, Klaus W. Hodapp, Tomoyuki Kudo, Nobuhiko Kusakabe, Mei-Yin Chou, Yoichi Itoh, Munetake Momose, Satoshi Mayama, Thayne Currie, Katherine B. Follette, Jungmi Kwon, Lyu Abe, Wolfgang Brandner, Timothy D. Brandt, Joseph Carson, Sebastian E. Egner, Markus Feldt, Olivier Guyon, Yutaka Hayano, Masahiko Hayashi, Saeko Hayashi, Miki Ishii, Masanori Iye, Markus Janson, Gillian R. Knapp, Masayuki Kuzuhara, Michael W. McElwain, Taro Matsuo, Shoken Miyama, Jun-Ichi Morino, Amaya Moro-Martin, Tetsuo Nishimura, Tae-Soo Pyo, Eugene Serabyn, Hiroshi Suto, Ryuji Suzuki, Naruhisa Takato, Hiroshi Terada, Christian Thalmann, Daigo Tomono, Edwin L. Turner, Makoto Watanabe, Toru Yamada, Hideki Takami, Tomonori Usuda and Motohide Tamura, 17 July 2013, The Astrophysical Journal.
This research was supported in part by the following:
- National Science Council grant 100-2112-M-001-007-MY3
- National Science Foundation (U.S.A.) grants 1008440 1009203 and 1009314
- Ministry of Education, Culture, Sports, Science and Technology (MEXT, Japan) Grants-in-Aid for Scientific Research in a Priority Area 2200000, 23103004.
- The Center for the Promotion of Integrated Sciences (CPISS) of The Graduate University for Advanced Studies (SOKENDAI, Japan)