Alma’s view of the IRAS-07299 star-forming region and the massive binary system at its center.
While it is known that most massive stars possess orbiting stellar companions it has been unclear how this comes about. Are the stars born together from a common, spiralling gas disk at the center of a collapsing cloud, or do they pair up later by chance encounters in a crowded star cluster?
Understanding the dynamics of forming binaries has been difficult because the protostars in these systems are still enveloped in a thick cloud of gas and dust that prevents most light from escaping. Fortunately, it is possible to see them using radio waves, as long as they can be imaged with sufficiently high spatial resolution.
In the current research, published in Nature Astronomy, the researchers led by Yichen Zhang (RIKEN Cluster for Pioneering Research
, Japan) and Jonathan Tan (Chalmers and University of Virginia), used the Atacama Large Millimeter/Submillimeter Array (Alma) telescope array in northern Chile to observe, at high spatial resolution, a star-forming region known as IRAS07299-1651, which is located about 5,500 light years (1.68 kiloparsecs) away in the constellation Puppis.
The observations showed that already at this early stage, the cloud contains two objects, a massive “primary” central star and another “secondary” forming star, also of high mass. For the first time, the research team were able to use these observations to deduce the dynamics of the system. The observations showed that the two forming stars are quite far apart, separated by a distance of about 180 astronomical units (180 times the distance from the Earth to the Sun). They are currently orbiting each other with a period of at most 600 years, and have a total mass at least 18 times that of our Sun.
“This is an exciting finding because we have long been perplexed by the question of whether stars form into binaries during the initial collapse of the star-forming cloud or whether they are created during later stages. Our observations clearly show that the division into binary stars takes place early on, while they are still in their infancy,” says Yichen Zhang.
Another finding of the study was that the binary stars are being nurtured from a common disk fed by the collapsing cloud and favoring a scenario in which the secondary star of the binary formed as a result of fragmentation of the disk originally around the primary. This allows the initially smaller secondary protostar to “steal” infalling matter from its sibling. Eventually they should emerge as quite similar "twins”.
“This is an important result for understanding the birth of massive stars. Such stars are important throughout the universe, not least for producing, at the ends of their lives, the heavy elements that make up our Earth and are in our bodies”, says Jonathan Tan.
“What is important now is to look at other examples to see whether this is a unique situation or something that is common for the birth of all massive stars”, concludes Yichen Zhang.
Robert Cumming, communicator, Onsala Space Observatory, Chalmers University of Technology, +46 31-772 5500, +46 70-493 31 14, email@example.com
Jonathan Tan, professor of astrophysics, Chalmers University of Technology, +46 31 772 6516, firstname.lastname@example.org
Image and film clip
Image A (top and above right): Alma’s view of the IRAS-07299 star-forming region and the massive binary system at its center.
The background image shows dense, dusty streams of gas (shown in green) that appear to be flowing toward the center of the system. Gas that is moving toward us -- as traced by the methanol molecule -- is shown in blue; motions away from us in red. The inset image shows a zoom-in view of the massive forming binary, with the brighter, primary protostar moving toward us shown in blue and the fainter, secondary protostar moving away from us shown in red. The blue and red dotted lines show an example of orbits of the primary and secondary spiraling around their center of mass (marked by the cross). Link to full-resolution image
Image credit: ALMA (ESO/NAOJ/NRAO)/Y. Zhang et al
A movie composed of images taken by Alma showing the gas streams, as traced by the methanol molecule, with different line-of-sight color-coded velocities, around the massive binary protostar system. The grey background image shows the overall distribution, from all velocities, of dust emission from the dense gas streams.
More about the research and about Alma
The research findings are reported in Nature Astronomy in the article Dynamics of a massive binary at birth by Yichen Zhang, Jonathan C. Tan, Kei E. I. Tanaka, James M. De Buizer, Mengyao Liu, Maria T. Beltrán, Kaitlin Kratter, Diego Mardones and Guido Garay, doi: 10.1038/s41550-019-0718-y
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.