At least one in a dozen stars show evidence of planetary ingestion according to a paper published in Nature today.
The international research team studied twin stars that should have identical composition. But, in about eight percent of cases, they differ, perplexing astronomers.
The team, led by ASTRO 3D researchers has found that the difference is due to one of the twins devouring planets or planetary material. The findings have been made possible thanks to a large dataset collected with the 6.5-metre Magellan Telescope and the European Southern Observatory’s Very Large Telescope, both in Chile, and the 10-meter Keck Telescope in Hawaii, United States.
“We looked at twin stars travelling together. They are born of the same molecular clouds and so should be identical,” says ASTRO 3D Researcher Dr Fan Liu, from Monash University, and lead author of the paper.
“Thanks to this very high precision analysis, we can see chemical differences between the twins. This provides very strong evidence that one of the stars has swallowed planets or planetary material and changed its composition.”
The phenomenon appeared in about eight per cent of the 91 pairs of twin stars that the team looked at. What makes this study compelling is that the stars were in their prime of life – so-called main sequence stars, rather than stars in their final phases such as red giants.
“This is different from previous studies where late-stage stars can engulf nearby planets when the star becomes a very giant ball,” Dr. Liu says.
There is some room for doubt as to whether the stars are swallowing planets whole or engulfing protoplanetary material but Dr. Liu suspects both are possible. “It’s complicated. The ingestion of the whole planet is our favoured scenario but of course we can also not rule out that these stars have ingested a lot of material from a protoplanetary disk,” he says.
The findings have wide-ranging implications for the study of the long-term evolution of planetary systems.
“Astronomers used to believe that these kinds of events were not possible. But from the observations in our study, we can see that, while the occurrence is not high, it is actually possible. This opens a new window for planet evolution theorists to study,” says Associate Professor Yuan-Sen Ting, a co-author and an ASTRO 3D researcher from the Australian National University (ANU).
The study forms part of a larger collaboration, the Complete Census of Co-moving Pairs of Objects (C3PO) initiative to spectroscopically observe a complete sample of all bright co-moving stars identified by the Gaia astrometric satellite, which is jointly led by Liu, Ting, and Associate Professor David Yong (also with ASTRO 3D at ANU).
“The findings presented here contribute to the big picture of a key ASTRO 3D research theme: the Chemical Evolution of the Universe. Specifically, they shed light on the distribution of chemical elements and their subsequent journey, which includes being consumed by stars,” said Professor Emma Ryan-Weber, Director of ASTRO 3D.
Scientists from Australia’s Swinburne University of Technology, University College Cork in Ireland, Carnegie Observatories, Ohio State University, Dartmouth College in United States, Konkoly Observatory in Hungry, and the Max Planck Institute for Astronomy took part in the research. Note: the researchers worked with twin stars known as co-natal – borne in the same molecular clouds and travelling together. They are not necessarily binary stars, though some of the pairs were.
ABOUT ASTRO 3D
The ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) is a $40m Research Centre of Excellence funded by the Australian Research Council (ARC) and nine collaborating Australian universities – The Australian National University, The University of Sydney, The University of Melbourne, Swinburne University of Technology, The University of Western Australia, Curtin University, Macquarie University, The University of New South Wales, and Monash University.
Contacts:
Niall Byrne (for ASTRO 3D)
+61 417-131-977, niall@scienceinpublic.com.au
Interviews
Fan Liu (ASTRO 3D, Monash University), +61 416 786 432, fan.liu@monash.edu
Yuan-Sen Ting (ASTRO 3D, ANU), +61 493 104 039, yuan-sen.ting@anu.edu.au
The paper is available at: https://doi.org/10.1038/s41586-024-07091-y
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Abstract and author list
At least one in a dozen stars shows evidence of planetary ingestion
Fan Liu1,2,3*, Yuan-Sen Ting3,4,5,6,7,8, David Yong3,4, Bertram Bitsch9,10, Amanda Karakas1,3, Michael T. Murphy2, Meridith Joyce11,12, Aaron Dotter13, Fei Dai14,15
Stellar chemical compositions can be altered by ingestion of planetary material [1, 2] and/or planet formation, which removes refractory material from the proto-stellar disc [3, 4]. These ‘planet signatures’ appear as correlations between elemental abundance differences and the dust condensation temperature [3, 5, 6].
Detecting these planet signatures, however, is challenging owing to unknown occurrence rates, small amplitudes, and heterogeneous star samples with large differences in stellar ages [7, 8]. Therefore, stars born together (that is, co-natal) with identical compositions can facilitate the detection of planet signatures.
Although previous spectroscopic studies have been limited to a small number of binary stars [9–13], the Gaia satellite [14] provides opportunities for detecting stellar chemical signatures of planets among co-moving pairs of stars confirmed to be co-natal [15, 16]. Here we report high-precision chemical abundances for a homogeneous sample of ninety-one co-natal pairs of stars with a well defined selection function and identify at least seven instances of planetary ingestion, corresponding to an occurrence rate of eight per cent. An independent Bayesian indicator is deployed, which can effectively disentangle the planet signatures from other factors, such as random abundance variation and atomic diffusion [17].
Our study provides evidence of planet signatures and facilitates a deeper understanding of the star-planet-chemistry connection by providing new observational constraints on the mechanisms of planet engulfment, formation and evolution.
1School of Physics and Astronomy, Monash University, Clayton, Victoria 3800, Australia.
2Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia.
3ARC Centre for All Sky Astrophysics in 3D (ASTRO-3D), Canberra, ACT, Australia.
4Research School of Astronomy and Astrophysics, Australian National University, Weston, ACT 2611, Australia. 5School of Computing, Australian National University, Acton, ACT 2601, Australia.
6Department of Astronomy, The Ohio State University, Columbus, OH 45701, USA.
7Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, OH 43210, USA. 8Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA.
9Max-Planck-Institut fu ̈r Astronomie, Knigstuhl 17, Heidelberg, 69117, Germany.
10Department of Physics, University College Cork, Cork, T12 R229, Ireland.
11HUN-REN Research Centre for Astronomy and Earth Sciences, Konkoly Observatory, Konkoly Thege Mikl ́os u ́t 15-17, Budapest, H-1121, Hungary.
12CSFK, MTA Centre of Excellence, Konkoly Thege Mikl ́os u ́t 15-17, Budapest, H-1121, Hungary.
13Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755, USA.
14Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E California Blvd, Pasadena, CA 91125, USA.
15Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA.