ALMA high resolution observations of Betelgeuse: Persistent structure spanning the inner atmosphere
Abstract
The extended atmosphere of red supergiants (RSGs) forms an important link in the process of mass loss and the subsequent enrichment of the interstellar medium. Large-scale convection is thought to play a significant role, which is likely to result in irregularities in the surface. High resolution, high contrast sub-mm images of Betelgeuse - one of the closest RSGs - are used to probe the structure and temporal stability of the inner 1-2R⋆ of its atmosphere. Using ALMA in the longest baseline configuration, continuum emission and lines of SiO and CO and their isotopomers were observed at λ0.6-1.4mm, giving beamwidths down to 7mas at the shortest wavelengths. These were compared with a similar observation taken at 0.9mm approximately 7 years earlier. The observed continuum emission arises mostly from an optically-thick mm/sub-mm photosphere of radius 1.1-1.3R⋆ with a relatively constant temperature of ∼2300K, but with two hotter patches to the NE and SW. The brightest of these has a temperature enhancement of ∼800K, and its location and intensity appears relatively unchanged since the 2015 observation. The sub-mm photosphere shows deviations of up to ± 6% in radius, with weaker continuum extending out to ∼2.5R⋆ - similar to the extent of clumpy emission in SiO and CO. The hot regions of gas and deviations from radial symmetry are thought to be associated with active shocks driven by underlying convective cells, although their lifetimes appear longer than model predictions. They lie near the proposed poles of the star, which might suggest enhanced and relatively stable polar convection. The present data show no clear evidence for stellar rotation in the extended line emission or absorption against the photosphere, although the structure of the gas emission has changed significantly since 2015.
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BibTeX
@misc{dent2026alma,
title = {{ALMA high resolution observations of Betelgeuse: Persistent structure spanning the inner atmosphere}},
author = {W. R. F. Dent and A. M. S. Richards and G. M. Harper and L. D. Matthews and E. O'Gorman},
howpublished = {arXiv},
year = {2026},
month = aug,
doi = {10.48550/arxiv.2608.19339},
eprint = {2608.19339},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2608.19339},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - ALMA high resolution observations of Betelgeuse: Persistent structure spanning the inner atmosphere
AU - W. R. F. Dent
AU - A. M. S. Richards
AU - G. M. Harper
AU - L. D. Matthews
AU - E. O'Gorman
PY - 2026
DA - 2026/08/28
PB - arXiv
DO - 10.48550/arxiv.2608.19339
UR - https://arxiv.org/abs/2608.19339
AB - The extended atmosphere of red supergiants (RSGs) forms an important link in the process of mass loss and the subsequent enrichment of the interstellar medium. Large-scale convection is thought to play a significant role, which is likely to result in irregularities in the surface. High resolution, high contrast sub-mm images of Betelgeuse - one of the closest RSGs - are used to probe the structure and temporal stability of the inner 1-2R_⋆ of its atmosphere. Using ALMA in the longest baseline configuration, continuum emission and lines of SiO and CO and their isotopomers were observed at λ0.6-1.4mm, giving beamwidths down to 7mas at the shortest wavelengths. These were compared with a similar observation taken at 0.9mm approximately 7 years earlier. The observed continuum emission arises mostly from an optically-thick mm/sub-mm photosphere of radius 1.1-1.3R_⋆ with a relatively constant temperature of ∼2300K, but with two hotter patches to the NE and SW. The brightest of these has a temperature enhancement of ∼800K, and its location and intensity appears relatively unchanged since the 2015 observation. The sub-mm photosphere shows deviations of up to ± 6% in radius, with weaker continuum extending out to ∼2.5R_⋆ - similar to the extent of clumpy emission in SiO and CO. The hot regions of gas and deviations from radial symmetry are thought to be associated with active shocks driven by underlying convective cells, although their lifetimes appear longer than model predictions. They lie near the proposed poles of the star, which might suggest enhanced and relatively stable polar convection. The present data show no clear evidence for stellar rotation in the extended line emission or absorption against the photosphere, although the structure of the gas emission has changed significantly since 2015.
ER -