JWST’s Insights Into Protoplanetary Disks

Hydrocarbon Molecules Protoplanetary Disk Around a Very Low-Mass Star

Artist’s impression of a protoplanetary disk around a very low-mass star. It depicts a selection of hydrocarbon molecules (Methane, CH4; Ethane, C2H6; Ethylene, C2H2; Diacetylene, C4H2; Propyne, C3H4; Benzene, C6H6) detected in the disk around ISO-ChaI 147. Credit: ALMA (ESO/NAOJ/NRAO) / MPIA

Observations from the James Webb Space Telescope have revealed a high concentration of hydrocarbons in the protoplanetary disk of a young star with very low mass.

James Webb Space Telescope (JWST) observations have revealed abundant hydrocarbons in the protoplanetary disk surrounding a young, very-low-mass star – findings that provide novel insights into the chemical environment from which many terrestrial planets, in particular, are born.

Efficiency of Planet Formation Around VLMSs

Planets form in disks of gas and dust that orbit young stars. Observations show that terrestrial planets form more efficiently than gas giant planets around very-low-mass stars (VLMSs) – those with less than 0.3 solar masses. Although the chemical compositions of the inner disk regions around higher mass stars have been previously studied, very few inner disk regions around VLMSs have been investigated.

Protoplanetary Disc of SO-ChaI 147 (Webb MIRI Emission Spectrum)

The spectrum revealed by Webb’s Mid-InfraRed Instrument (MIRI) shows the richest hydrocarbon chemistry seen to date in a protoplanetary disc, consisting of 13 carbon-bearing molecules up to benzene. This includes the first extrasolar detection of ethane (C2H6), the largest fully-saturated hydrocarbon detected outside our Solar System. Since fully-saturated hydrocarbons are expected to form from more basic molecules, detecting them here gives researchers clues about the chemical environment. The team also successfully detected ethylene (C2H4), propyne (C3H4), and the methyl radical CH3, for the first time in a protoplanetary disc. This graphic highlights the detections of ethane (C2H6), methane (CH4), propyne (C3H4), cyanoacetylene (HC3N), and the methyl radical CH3. Credit: NASA, ESA, CSA, R. Crawford (STScI)

Mid-Infrared Spectroscopy Reveals Disk Chemistry

Using the JWST’s mid-infrared spectroscopy instrument, Aditya Arabhavi and colleagues investigated the chemical composition of the planet-forming disk around ISO-ChaI 147, a young 0.11-solar-mass star in the Chameleon I star-forming region.

Implications of a High Carbon/Oxygen Ratio

The researchers found that the inner disk region surrounding this star has a carbon-rich chemistry featuring 13 carbon-bearing molecules, including ethane and benzine. This abundance in hydrocarbon molecules starkly contrasts the lack of observed oxygen-bearing molecules, suggesting that the region has a carbon to oxygen radio of >1.

According to the research team, this high carbon/oxygen ratio indicates radial transport of material within the disk, likely affecting the bulk composition of any planets forming within the disk.

For more on this discovery:

Reference: “Abundant hydrocarbons in the disk around a very-low-mass star” by A. M. Arabhavi, I. Kamp, Th. Henning, E. F. van Dishoeck, V. Christiaens, D. Gasman, A. Perrin, M. Güdel, B. Tabone, J. Kanwar, L. B. F. M. Waters, I. Pascucci, M. Samland, G. Perotti, G. Bettoni, S. L. Grant, P. O. Lagage, T. P. Ray, B. Vandenbussche, O. Absil, I. Argyriou, D. Barrado, A. Boccaletti, J. Bouwman, A. Caratti o Garatti, A. M. Glauser, F. Lahuis, M. Mueller, G. Olofsson, E. Pantin, S. Scheithauer, M. Morales-Calderón, R. Franceschi, H. Jang, N. Pawellek, D. Rodgers-Lee, J. Schreiber, K. Schwarz, M. Temmink, M. Vlasblom, G. Wright, L. Colina and G. Östlin, 6 June 2024, Science.
DOI: 10.1126/science.adi8147

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