The salty emission of the intermediate-mass AGB star OH 30.1 -0.7

Fuente: arXiv

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Bibliographic Details
Main Authors:	Danilovich, T., Richards, A. M. S., Van de Sande, M., Gottlieb, C. A., Millar, T. J., Karakas, A. I., Müller, H. S. P., Justtanont, K., Plane, J. M. C., Etoka, S., Wallström, S. H. J., Decin, L., Engels, D., Groenewegen, M. A. T., Kerschbaum, F., Khouri, T., de Koter, A., Olofsson, H., Paladini, C., Stancliffe, R. J.
Format:	Preprint
Published:	2024
Subjects:	Solar and Stellar Astrophysics
Online Access:	Acceder al recurso
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_version_	1866915083224875008
author	Danilovich, T. Richards, A. M. S. Van de Sande, M. Gottlieb, C. A. Millar, T. J. Karakas, A. I. Müller, H. S. P. Justtanont, K. Plane, J. M. C. Etoka, S. Wallström, S. H. J. Decin, L. Engels, D. Groenewegen, M. A. T. Kerschbaum, F. Khouri, T. de Koter, A. Olofsson, H. Paladini, C. Stancliffe, R. J.
author_facet	Danilovich, T. Richards, A. M. S. Van de Sande, M. Gottlieb, C. A. Millar, T. J. Karakas, A. I. Müller, H. S. P. Justtanont, K. Plane, J. M. C. Etoka, S. Wallström, S. H. J. Decin, L. Engels, D. Groenewegen, M. A. T. Kerschbaum, F. Khouri, T. de Koter, A. Olofsson, H. Paladini, C. Stancliffe, R. J.
contents	We analyse continuum and molecular emission, observed with ALMA, from the dust-enshrouded intermediate-mass AGB star OH 30.1 -0.7. We find a secondary peak in the continuum maps, "feature B", separated by 4.6" from the AGB star, which corresponds to a projected separation of $1.8 \times 10^4$ au, placing a lower limit on the physical separation. This feature is most likely composed of cold dust and is likely to be ejecta associated with the AGB star, though we cannot rule out that it is a background object. The molecular emission we detect includes lines of CO, SiS, CS, SO$_2$, NS, NaCl, and KCl. We find that the NS emission is off centre and arranged along an axis perpendicular to the direction of feature B, indicative of a UV-emitting binary companion (e.g. a G-type main sequence star or hotter), perhaps on an eccentric orbit, contributing to its formation. However, the NaCl and KCl emission constrain the nature of that companion to not be hotter than a late B-type main sequence star. We find relatively warm emission arising from the inner wind and detect several vibrationally excited lines of SiS (3 = 1), NaCl (up to 3 = 4) and KCl (up to 3 = 2), and emission from low energy levels in the mid to outer envelope, as traced by SO$_2$. The CO emission is abruptly truncated around 3.5" or 14,000 au from the continuum peak, suggesting that mass loss at a high rate may have commenced as little as 2800 years ago.
format	Preprint
id	arxiv_https___arxiv_org_abs_2411_08235
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	The salty emission of the intermediate-mass AGB star OH 30.1 -0.7 Danilovich, T. Richards, A. M. S. Van de Sande, M. Gottlieb, C. A. Millar, T. J. Karakas, A. I. Müller, H. S. P. Justtanont, K. Plane, J. M. C. Etoka, S. Wallström, S. H. J. Decin, L. Engels, D. Groenewegen, M. A. T. Kerschbaum, F. Khouri, T. de Koter, A. Olofsson, H. Paladini, C. Stancliffe, R. J. Solar and Stellar Astrophysics We analyse continuum and molecular emission, observed with ALMA, from the dust-enshrouded intermediate-mass AGB star OH 30.1 -0.7. We find a secondary peak in the continuum maps, "feature B", separated by 4.6" from the AGB star, which corresponds to a projected separation of $1.8 \times 10^4$ au, placing a lower limit on the physical separation. This feature is most likely composed of cold dust and is likely to be ejecta associated with the AGB star, though we cannot rule out that it is a background object. The molecular emission we detect includes lines of CO, SiS, CS, SO$_2$, NS, NaCl, and KCl. We find that the NS emission is off centre and arranged along an axis perpendicular to the direction of feature B, indicative of a UV-emitting binary companion (e.g. a G-type main sequence star or hotter), perhaps on an eccentric orbit, contributing to its formation. However, the NaCl and KCl emission constrain the nature of that companion to not be hotter than a late B-type main sequence star. We find relatively warm emission arising from the inner wind and detect several vibrationally excited lines of SiS (3 = 1), NaCl (up to 3 = 4) and KCl (up to 3 = 2), and emission from low energy levels in the mid to outer envelope, as traced by SO$_2$. The CO emission is abruptly truncated around 3.5" or 14,000 au from the continuum peak, suggesting that mass loss at a high rate may have commenced as little as 2800 years ago.
title	The salty emission of the intermediate-mass AGB star OH 30.1 -0.7
topic	Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2411.08235