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Large granulation cells on the surface of the giant star π1 Gruis



Convection plays a major part in many astrophysical processes, including energy transport, pulsation, dynamos and winds on evolved stars, in dust clouds and on brown dwarfs1,2. Most of our knowledge about stellar convection has come from studying the Sun: about two million convective cells with typical sizes of around 2,000 kilometres across are present on the surface of the Sun3—a phenomenon known as granulation. But on the surfaces of giant and supergiant stars there should be only a few large (several tens of thousands of times larger than those on the Sun) convective cells3, owing to low surface gravity. Deriving the characteristic properties of convection (such as granule size and contrast) for the most evolved giant and supergiant stars is challenging because their photospheres are obscured by dust, which partially masks the convective patterns4. These properties can be inferred from geometric model fitting5,6,7, but this indirect method does not provide information about the physical origin of the convective cells5,6,7. Here we report interferometric images of the surface of the evolved giant star π1 Gruis, of spectral type8,9 S5,7. Our images show a nearly circular, dust-free atmosphere, which is very compact and only weakly affected by molecular opacity. We find that the stellar surface has a complex convective pattern with an average intensity contrast of 12 per cent, which increases towards shorter wavelengths. We derive a characteristic horizontal granule size of about 1.2 × 1011 metres, which corresponds to 27 per cent of the diameter of the star. Our measurements fall along the scaling relations between granule size, effective temperature and surface gravity that are predicted by simulations of stellar surface convection10,11,12.

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Figure 1: The stellar surface of π1 Gruis.
Figure 2: Power spectral density.
Figure 3: The characteristic horizontal scale of granulation of π1 Gruis versus theoretical predictions.

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C.P. acknowledges the support of the Fonds National de la Recherche Scientifique (F.R.S.-FNRS), Belgium. C.S., G.S. are supported by the PRODEX office, Belgium. This research has been funded by the Belgian Science Policy Office under contract BR/143/A2/STARLAB (S.S., A.J., S.V.E.). K.K. is supported by a FRIA grant (Belgium). F.B. acknowledges funding by the National Science Foundation, NSF-AST numbers 1445935 and 1616483. J.K. acknowledges the Philip Leverhulme Prize (PLP-2013-110). S.V.E. thanks the Fondation ULB for its support. The research leading to these results has received funding from the European Union’s Horizon 2020 research and innovation programme under Grant Agreement 730890 (OPTICON) and from the Austrian Science Fund (FWF) under project AP23006-N16. We thank all the ESO/VLTI staff for supporting our observations.

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Authors and Affiliations



This project was initiated by C.P. A.M. carried out the observations. J.B.L.B. performed the data reduction, F.B. and J.B.L.B. performed the image reconstruction. The contrast and the PSD analysis was carried on by C.P., B.F. and F.B. The stellar parameter determination was made by C.P., S.V.E., S.S., and K.K. A.J. gave crucial help through all the scientific analysis. The text was written by C.P., F.B. and A.J., and edited by the other authors that contributed to the scientific discussion.

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Correspondence to C. Paladini.

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The authors declare no competing financial interests.

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Reviewer Information Nature thanks P. Kervella, J. Young and the other anonymous reviewer(s) for their contribution to the peer review of this work.

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Extended data figures and tables

Extended Data Figure 1 The PIONIER data.

The upper left panel shows in black the PIONIER squared visibilities V and in blue the Fourier transform of the SQUEEZE image (first spectral channel) on a linear (main panel) and semi-logarithmic (inset) scale. The upper right panel is the same, but for the closure phase. The lower left panel shows the uv coverage of the data. The blue data correspond to observations acquired with the short VLTI array configuration (called ‘A1-B2-C1-D0’). The red data correspond to observations acquired with the intermediate array configuration (‘D0-G1-H0-I1’).

Extended Data Figure 2 SQUEEZE images and error images.

ac, The first row of images corresponds to the adopted SQUEEZE images; the second row, labelled ‘+STD DEV’, corresponds to images one standard deviation above the average image; and the third row of images, labelled ‘-STD DEV’ shows images one standard deviation below the average image.

Extended Data Figure 3 Spectral energy distribution.

Comparison between the spectral energy distribution (yellow stars) and the best-fitting MARCS synthetic spectrum (black line). Note the presence of a moderate infrared excess longwards of 10 μm (105 Å) attributable to circumstellar dust.

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Paladini, C., Baron, F., Jorissen, A. et al. Large granulation cells on the surface of the giant star π1 Gruis. Nature 553, 310–312 (2018).

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