The formation of discs in the interior of AGB stars from the tidal disruption of planets and brown dwarfs
Abstract
ABSTRACT A significant fraction of isolated white dwarfs host magnetic fields in excess of a MegaGauss. Observations suggest that these fields originate in interacting binary systems where the companion is destroyed thus leaving a singular, highly magnetized white dwarf. In post-main-sequence evolution, radial expansion of the parent star may cause orbiting companions to become engulfed. During the common envelope phase, as the orbital separation rapidly decreases, low-mass companions will tidally disrupt as they approach the giant’s core. We hydrodynamically simulate the tidal disruption of planets and brown dwarfs, and the subsequent accretion disc formation, in the interior of an asymptotic giant branch star. Compared to previous steady-state simulations, the resultant discs form with approximately the same mass fraction as estimated but have not yet reached steady state and are morphologically more extended in height and radius. The long-term evolution of the disc and the magnetic fields generated therein require future study.
- Publication Date:
- Research Org.:
- Univ. of Rochester, NY (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC); National Science Foundation (NSF); National Aeronautics and Space Administration (NASA); National Technical Institute for the Deaf (NTID)
- OSTI Identifier:
- 1854264
- Alternate Identifier(s):
- OSTI ID: 1979562
- Grant/Contract Number:
- SC0001063; SC0020432; SC0020434; AST-2009713; HST-AR-15044; SPDI-15992; ACI-1548562; AST-1813298; HST-AR-12832.01-A
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 511 Journal Issue: 4; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; accretion; accretion discs; stars; AGB and post-AGB; binaries; close; white dwarfs
Citation Formats
Guidarelli, G., Nordhaus, J., Carroll-Nellenback, J., Chamanady, L., Frank, A., and Blackman, E. G. The formation of discs in the interior of AGB stars from the tidal disruption of planets and brown dwarfs. United Kingdom: N. p., 2022.
Web. doi:10.1093/mnras/stac463.
Guidarelli, G., Nordhaus, J., Carroll-Nellenback, J., Chamanady, L., Frank, A., & Blackman, E. G. The formation of discs in the interior of AGB stars from the tidal disruption of planets and brown dwarfs. United Kingdom. https://doi.org/10.1093/mnras/stac463
Guidarelli, G., Nordhaus, J., Carroll-Nellenback, J., Chamanady, L., Frank, A., and Blackman, E. G. Tue .
"The formation of discs in the interior of AGB stars from the tidal disruption of planets and brown dwarfs". United Kingdom. https://doi.org/10.1093/mnras/stac463.
@article{osti_1854264,
title = {The formation of discs in the interior of AGB stars from the tidal disruption of planets and brown dwarfs},
author = {Guidarelli, G. and Nordhaus, J. and Carroll-Nellenback, J. and Chamanady, L. and Frank, A. and Blackman, E. G.},
abstractNote = {ABSTRACT A significant fraction of isolated white dwarfs host magnetic fields in excess of a MegaGauss. Observations suggest that these fields originate in interacting binary systems where the companion is destroyed thus leaving a singular, highly magnetized white dwarf. In post-main-sequence evolution, radial expansion of the parent star may cause orbiting companions to become engulfed. During the common envelope phase, as the orbital separation rapidly decreases, low-mass companions will tidally disrupt as they approach the giant’s core. We hydrodynamically simulate the tidal disruption of planets and brown dwarfs, and the subsequent accretion disc formation, in the interior of an asymptotic giant branch star. Compared to previous steady-state simulations, the resultant discs form with approximately the same mass fraction as estimated but have not yet reached steady state and are morphologically more extended in height and radius. The long-term evolution of the disc and the magnetic fields generated therein require future study.},
doi = {10.1093/mnras/stac463},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 4,
volume = 511,
place = {United Kingdom},
year = {Tue Mar 08 00:00:00 EST 2022},
month = {Tue Mar 08 00:00:00 EST 2022}
}
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