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Constraining planet formation around 6M⊙-8M⊙ stars
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Veras, Dimitri, Tremblay, Pier-Emmanuel, Hermes, J. J., McDonald, Catriona H., Kennedy, Grant M., Meru, Farzana and Gaensicke, Boris T. (2020) Constraining planet formation around 6M⊙-8M⊙ stars. Monthly Notices of the Royal Astronomical Society, 493 (1). pp. 765-775. doi:10.1093/mnras/staa241 ISSN 1745-3933.
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WRAP-constraining-planet-formation-around-6M⊙-8M⊙-stars-Veras-2020.pdf - Accepted Version - Requires a PDF viewer. Download (1237Kb) | Preview |
Official URL: http://dx.doi.org/10.1093/mnras/staa241
Abstract
Identifying planets around O-type and B-type stars is inherently difficult; the most massive known planet host has a mass of only about 3M⊙. However, planetary systems which survive the transformation of their host stars into white dwarfs can be detected via photospheric trace metals, circumstellar dusty and gaseous discs, and transits of planetary debris crossing our line-of-sight. These signatures offer the potential to explore the efficiency of planet formation for host stars with masses up to the core-collapse boundary at ≈8M⊙, a mass regime rarely investigated in planet formation theory. Here, we establish limits on where both major and minor planets must reside around ≈6M⊙ − 8M⊙ stars in order to survive into the white dwarf phase. For this mass range, we find that intact terrestrial or giant planets need to leave the main sequence beyond approximate minimum star-planet separations of respectively about 3 and 6 au. In these systems, rubble pile minor planets of radii 10, 1.0, and 0.1 km would have been shorn apart by giant branch radiative YORP spin-up if they formed and remained within, respectively, tens, hundreds and thousands of au. These boundary values would help distinguish the nature of the progenitor of metal-pollution in white dwarf atmospheres. We find that planet formation around the highest mass white dwarf progenitors may be feasible, and hence encourage both dedicated planet formation investigations for these systems and spectroscopic analyses of the highest mass white dwarfs.
| Item Type: | Journal Article | ||||||||||||||||||||||||
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| Subjects: | Q Science > QB Astronomy | ||||||||||||||||||||||||
| Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | ||||||||||||||||||||||||
| Library of Congress Subject Headings (LCSH): | Planetary systems, Satellites, Stars -- Orbits, Astrophysics, White dwarf stars -- Magnetic properties | ||||||||||||||||||||||||
| Journal or Publication Title: | Monthly Notices of the Royal Astronomical Society | ||||||||||||||||||||||||
| Publisher: | Oxford University Press | ||||||||||||||||||||||||
| ISSN: | 1745-3933 | ||||||||||||||||||||||||
| Official Date: | March 2020 | ||||||||||||||||||||||||
| Dates: |
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| Volume: | 493 | ||||||||||||||||||||||||
| Number: | 1 | ||||||||||||||||||||||||
| Page Range: | pp. 765-775 | ||||||||||||||||||||||||
| DOI: | 10.1093/mnras/staa241 | ||||||||||||||||||||||||
| Status: | Peer Reviewed | ||||||||||||||||||||||||
| Publication Status: | Published | ||||||||||||||||||||||||
| Reuse Statement (publisher, data, author rights): | This is a pre-copyedited, author-produced version of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Dimitri Veras, Pier-Emmanuel Tremblay, J J Hermes, Catriona H McDonald, Grant M Kennedy, Farzana Meru, Boris T Gänsicke, Constraining planet formation around 6M⊙-8M⊙ stars, Monthly Notices of the Royal Astronomical Society, , staa241, https://doi.org/10.1093/mnras/staa241 is available online at: https://doi.org/10.1093/mnras/staa241 | ||||||||||||||||||||||||
| Access rights to Published version: | Restricted or Subscription Access | ||||||||||||||||||||||||
| Date of first compliant deposit: | 11 February 2020 | ||||||||||||||||||||||||
| Date of first compliant Open Access: | 24 February 2020 | ||||||||||||||||||||||||
| RIOXX Funder/Project Grant: |
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