Stars form in interstellar clouds of molecular gas and dust. Previous studies of star formation primarily focused on formation of single stars like the Sun, and a standard picture of single star formation has been established. According to the standard picture, a dense gas condensation in an interstellar cloud first collapses gravitationally and forms a single protostar at the center. In fact, previous observations have found such collapsing gas motions to feed materials toward the central protostars.
Compared to single star formation, our understanding of binary star formation has been limited. However, more than half of stars with a mass similar to that of the Sun are known to be binaries, and it is thus crucial to unveil the physical mechanism of binary formation observationally to obtain more comprehensive understanding of star formation. Theoretically, a disk surrounding the “baby twin” stars is considered to feed materials to the central baby twin stars and grow them. While recent observations have found such disks surrounding the baby twin stars, named “circumbinary disks,” those observations could not image the structures and gas motions of the disks to feed materials to the binary because of the insufficient imaging resolution and sensitivity.
The research team used ALMA to observe the baby twin star L1551 NE located in the constellation Taurus the Bull at a distance of 460 light-years, with a 1.6 times better imaging resolution and a six times better sensitivity than those of their previous observations with the SubMillimeter Array (SMA). They observed L1551 NE in the emission from dust at a 0.9-millimeter wavelength, a tracer of distribution of interstellar materials, and carbon monoxide molecular emission, which can be used to study gas motion with the Doppler effect. They found a gas component associated with each binary star and a disk surrounding both stars, a circumbinary disk, with a radius of 300 astronomical units (1 AU is the Earth-Sun distance). The radius corresponds to 10 times the orbital radius of Neptune in our solar system. For the first time, they succeeded in imaging the detailed structures of the circumbinary disk and found that the circumbinary disk consists of a southern U-shaped feature and northern emission protrusions pointing to the northwest and the northeast.
To understand these newly identified features, the research team constructed a theoretical model of binary formation in L1551 NE using the supercomputer ATERUI at the National Astronomical Observatory of Japan (NAOJ). The southern U-shaped feature and northern emission protrusions observed with ALMA can be reproduced with a pair of spiral arms stemming from each baby twin. The research team also investigated the observed gas motion as seen in the carbon monoxide molecular emission and identified faster rotating motions in the spiral arms and slower rotating motions in the inter-arm regions. The inter-arm regions also exhibit a falling gas motion toward the central baby twin stars — namely, the ongoing feeding process of the materials to the baby twin stars. These results show that the baby twin stars “shake” the surrounding circumbinary disk and induce the falling gas motion to feed the materials to the baby twin. “Our high-resolution ALMA observation has unveiled live images of the growth of the baby twins for the first time,” said Takakuwa.
“Our ALMA observation has revealed gas feeding to the baby twin stars from the surrounding disk,” said Tomoaki Matsumoto from Hosei University, who constructed the theoretical model with the supercomputer. “Our ALMA results match with our theoretical prediction remarkably accurately.”
“We succeeded in unveiling structures and motions in the circumbinary disk with such a high accuracy because of the high imaging resolution and sensitivity of ALMA,” said Kazuya Saigo and Takakuwa. “In this ALMA era, high-resolution ALMA observations coupled with thorough numerical simulations will be more and more important. Our research on L1551 NE using ALMA and theoretical modeling using a supercomputer can be regarded as an upcoming research trend.”
Credit: T. Matsumoto (Hosei University)
