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Magnetic massive stars from stellar mergers

Published online by Cambridge University Press:  29 August 2024

Fabian R. N. Schneider Open the ORCID record for Fabian R. N. Schneider [Opens in a new window] ,
Sebastian T. Ohlmann ,
Philipp Podsiadlowski ,
Friedrich K. Röpke ,
Steven A. Balbus ,
Rüdiger Pakmor  and
Volker Springel
Fabian R. N. Schneider*
Affiliation:
Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
Sebastian T. Ohlmann*
Affiliation:
Max Planck Computing and Data Facility, Gießenbachstr. 2, 85748 Garching, Germany
Philipp Podsiadlowski*
Affiliation:
University of Oxford, St Edmund Hall, Oxford, OX1 4AR, United Kingdom
Friedrich K. Röpke*
Affiliation:
Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Philosophenweg 12, 69120 Heidelberg, Germany
Steven A. Balbus*
Affiliation:
Department of Physics, University of Oxford, Keble Rd, Oxford OX1 3RH, United Kingdom
Rüdiger Pakmor*
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
Volker Springel*
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
*
email: [email protected]
email: [email protected]
email: [email protected]
email: [email protected]
email: [email protected]
email: [email protected], email: [email protected]
email: [email protected], email: [email protected]
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Abstract

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The first magnetic field in a star other than the Sun was detected in 1947 in the star 78 Vir. Today, we know that about 10% of these intermediate-mass and high-mass stars have strong, large-scale surface magnetic fields whose origin has remained a mystery till today. It has been suggested that merging of main-sequence and pre-main-sequence stars could produce such strong fields. The massive star τ Sco is a well-known member of the group of magnetic stars and is a blue straggler given its apparently young age compared to that of other members of the Upper Scorpius association. Here, we present 3D magnetohydrodynamic simulations of the coalescence of two massive main-sequence stars and 1D stellar evolution computations of the subsequent evolution of the merger product that can explain τ Sco’s magnetic field, apparent youth and other observed characteristics. We argue that field amplification in stellar mergers is a general mechanism to form strongly-magnetised massive stars. Such stars are promising progenitors of magnetars, which may give rise to some of the enigmatic fast radio bursts, and their supernova explosions may be affected by the strong magnetic fields.

Keywords

MHDbinaries: generalblue stragglersstars: evolutionstars: magnetic fields
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 212 - 217
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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