Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

D. Bollen; D. Kamath; O. De Marco; H. Van Winckel; M. Wardle

doi:10.1051/0004-6361/202038414

Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

D. Bollen^*, D. Kamath, O. De Marco, H. Van Winckel, M. Wardle

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

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Abstract

Aims. In this study we determine the morphology and mass-loss rate of jets emanating from the companion in post-Asymptotic giant branch (post-AGB) binary stars with a circumbinary disc. In doing so we also determine the mass-Accretion rates onto the companion, and investigate the source feeding the circum-companion accretion disc.

Methods. We perform a spatio-kinematic modelling of the jet of two well-sampled post-AGB binaries, BD+46°442 and IRAS 19135+3937, by fitting the orbital phased time series of Hα spectra. Once the jet geometry, velocity, and scaled density structure are computed, we carry out radiative transfer modelling of the jet for the first four Balmer lines to determine the jet densities, thus allowing us to compute the jet mass-loss rates and mass-Accretion rates. We distinguish the origin of the accretion by comparing the computed mass-Accretion rates with theoretically estimated mass-loss rates, both from the post-AGB star and from the circumbinary disc.

Results. The spatio-kinematic model of the jet reproduces the observed absorption feature in the Hα lines. The jets have an inner region with extremely low density in both objects. The jet model for BD+46°442 is tilted by 15° with respect to the orbital axis of the binary system. IRAS 19135+3937 has a smaller tilt of 6°. Using our radiative transfer model, we find the full 3D density structure of both jets. By combining these results, we can compute the mass-loss rates of the jets, which are of the order of 10^-7 - 10^-5 M_⊙ yr^-1. From this we estimate mass-Accretion rates onto the companion of 10^-6 - 10^-4 M_⊙ yr^-1.

Conclusions. Based on the mass-Accretion rates found for these two objects, we conclude that the circumbinary disc is most likely the source feeding the circum-companion accretion disc. This is in agreement with the observed depletion patterns in post-AGB binaries, which is caused by re-Accretion of gas from the circumbinary disc that is under-Abundant in refractory elements. The high accretion rates from the circumbinary disc imply that the lifetime of the disc will be short. Mass transfer from the post-AGB star cannot be excluded in these systems, but it is unlikely to provide a sufficient mass-Transfer rate to sustain the observed jet mass-loss rates.

Original language	English
Article number	A175
Pages (from-to)	1-16
Number of pages	16
Journal	Astronomy and Astrophysics
Volume	641
DOIs	https://doi.org/10.1051/0004-6361/202038414
Publication status	Published - 28 Sept 2020

Bibliographical note

Reproduced with permission from Astronomy & Astrophysics, Copyright ESO 2020. First published in Astronomy and Astrophysics, 641, A175, 2020, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/202038414. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

Keywords

accretion, accretion disks
binaries: spectroscopic
circumstellar matter
ISM: jets and outflows
stars: AGB and post-AGB
stars: mass-loss

Access to Document

10.1051/0004-6361/202038414

Publisher version (open access)Final published version, 7.51 MBLicence: Other

Cite this

@article{0297bc65487841d39667a68cb6ba4e49,

title = "Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems",

abstract = "Aims. In this study we determine the morphology and mass-loss rate of jets emanating from the companion in post-Asymptotic giant branch (post-AGB) binary stars with a circumbinary disc. In doing so we also determine the mass-Accretion rates onto the companion, and investigate the source feeding the circum-companion accretion disc.Methods. We perform a spatio-kinematic modelling of the jet of two well-sampled post-AGB binaries, BD+46°442 and IRAS 19135+3937, by fitting the orbital phased time series of Hα spectra. Once the jet geometry, velocity, and scaled density structure are computed, we carry out radiative transfer modelling of the jet for the first four Balmer lines to determine the jet densities, thus allowing us to compute the jet mass-loss rates and mass-Accretion rates. We distinguish the origin of the accretion by comparing the computed mass-Accretion rates with theoretically estimated mass-loss rates, both from the post-AGB star and from the circumbinary disc.Results. The spatio-kinematic model of the jet reproduces the observed absorption feature in the Hα lines. The jets have an inner region with extremely low density in both objects. The jet model for BD+46°442 is tilted by 15° with respect to the orbital axis of the binary system. IRAS 19135+3937 has a smaller tilt of 6°. Using our radiative transfer model, we find the full 3D density structure of both jets. By combining these results, we can compute the mass-loss rates of the jets, which are of the order of 10-7 - 10-5 M⊙ yr-1. From this we estimate mass-Accretion rates onto the companion of 10-6 - 10-4 M⊙ yr-1.Conclusions. Based on the mass-Accretion rates found for these two objects, we conclude that the circumbinary disc is most likely the source feeding the circum-companion accretion disc. This is in agreement with the observed depletion patterns in post-AGB binaries, which is caused by re-Accretion of gas from the circumbinary disc that is under-Abundant in refractory elements. The high accretion rates from the circumbinary disc imply that the lifetime of the disc will be short. Mass transfer from the post-AGB star cannot be excluded in these systems, but it is unlikely to provide a sufficient mass-Transfer rate to sustain the observed jet mass-loss rates. ",

keywords = "accretion, accretion disks, binaries: spectroscopic, circumstellar matter, ISM: jets and outflows, stars: AGB and post-AGB, stars: mass-loss",

author = "D. Bollen and D. Kamath and {De Marco}, O. and {Van Winckel}, H. and M. Wardle",

note = "Reproduced with permission from Astronomy & Astrophysics, Copyright ESO 2020. First published in Astronomy and Astrophysics, 641, A175, 2020, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/202038414. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.",

year = "2020",

month = sep,

day = "28",

doi = "10.1051/0004-6361/202038414",

language = "English",

volume = "641",

pages = "1--16",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

AU - Bollen, D.

AU - Kamath, D.

AU - De Marco, O.

AU - Van Winckel, H.

AU - Wardle, M.

N1 - Reproduced with permission from Astronomy & Astrophysics, Copyright ESO 2020. First published in Astronomy and Astrophysics, 641, A175, 2020, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/202038414. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

PY - 2020/9/28

Y1 - 2020/9/28

N2 - Aims. In this study we determine the morphology and mass-loss rate of jets emanating from the companion in post-Asymptotic giant branch (post-AGB) binary stars with a circumbinary disc. In doing so we also determine the mass-Accretion rates onto the companion, and investigate the source feeding the circum-companion accretion disc.Methods. We perform a spatio-kinematic modelling of the jet of two well-sampled post-AGB binaries, BD+46°442 and IRAS 19135+3937, by fitting the orbital phased time series of Hα spectra. Once the jet geometry, velocity, and scaled density structure are computed, we carry out radiative transfer modelling of the jet for the first four Balmer lines to determine the jet densities, thus allowing us to compute the jet mass-loss rates and mass-Accretion rates. We distinguish the origin of the accretion by comparing the computed mass-Accretion rates with theoretically estimated mass-loss rates, both from the post-AGB star and from the circumbinary disc.Results. The spatio-kinematic model of the jet reproduces the observed absorption feature in the Hα lines. The jets have an inner region with extremely low density in both objects. The jet model for BD+46°442 is tilted by 15° with respect to the orbital axis of the binary system. IRAS 19135+3937 has a smaller tilt of 6°. Using our radiative transfer model, we find the full 3D density structure of both jets. By combining these results, we can compute the mass-loss rates of the jets, which are of the order of 10-7 - 10-5 M⊙ yr-1. From this we estimate mass-Accretion rates onto the companion of 10-6 - 10-4 M⊙ yr-1.Conclusions. Based on the mass-Accretion rates found for these two objects, we conclude that the circumbinary disc is most likely the source feeding the circum-companion accretion disc. This is in agreement with the observed depletion patterns in post-AGB binaries, which is caused by re-Accretion of gas from the circumbinary disc that is under-Abundant in refractory elements. The high accretion rates from the circumbinary disc imply that the lifetime of the disc will be short. Mass transfer from the post-AGB star cannot be excluded in these systems, but it is unlikely to provide a sufficient mass-Transfer rate to sustain the observed jet mass-loss rates.

AB - Aims. In this study we determine the morphology and mass-loss rate of jets emanating from the companion in post-Asymptotic giant branch (post-AGB) binary stars with a circumbinary disc. In doing so we also determine the mass-Accretion rates onto the companion, and investigate the source feeding the circum-companion accretion disc.Methods. We perform a spatio-kinematic modelling of the jet of two well-sampled post-AGB binaries, BD+46°442 and IRAS 19135+3937, by fitting the orbital phased time series of Hα spectra. Once the jet geometry, velocity, and scaled density structure are computed, we carry out radiative transfer modelling of the jet for the first four Balmer lines to determine the jet densities, thus allowing us to compute the jet mass-loss rates and mass-Accretion rates. We distinguish the origin of the accretion by comparing the computed mass-Accretion rates with theoretically estimated mass-loss rates, both from the post-AGB star and from the circumbinary disc.Results. The spatio-kinematic model of the jet reproduces the observed absorption feature in the Hα lines. The jets have an inner region with extremely low density in both objects. The jet model for BD+46°442 is tilted by 15° with respect to the orbital axis of the binary system. IRAS 19135+3937 has a smaller tilt of 6°. Using our radiative transfer model, we find the full 3D density structure of both jets. By combining these results, we can compute the mass-loss rates of the jets, which are of the order of 10-7 - 10-5 M⊙ yr-1. From this we estimate mass-Accretion rates onto the companion of 10-6 - 10-4 M⊙ yr-1.Conclusions. Based on the mass-Accretion rates found for these two objects, we conclude that the circumbinary disc is most likely the source feeding the circum-companion accretion disc. This is in agreement with the observed depletion patterns in post-AGB binaries, which is caused by re-Accretion of gas from the circumbinary disc that is under-Abundant in refractory elements. The high accretion rates from the circumbinary disc imply that the lifetime of the disc will be short. Mass transfer from the post-AGB star cannot be excluded in these systems, but it is unlikely to provide a sufficient mass-Transfer rate to sustain the observed jet mass-loss rates.

KW - accretion, accretion disks

KW - binaries: spectroscopic

KW - circumstellar matter

KW - ISM: jets and outflows

KW - stars: AGB and post-AGB

KW - stars: mass-loss

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JO - Astronomy and Astrophysics

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M1 - A175

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Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

Abstract

Bibliographical note

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ARC - DECRA: Cosmic Alchemy: Revealing the Origin of Elements in the Universe

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Determining mass-accretion and jet mass-loss rates in post-asymptotic giant branch binary systems

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

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ARC - DECRA: Cosmic Alchemy: Revealing the Origin of Elements in the Universe

Cite this