Magnetic Field Amplification During the Common Envelope Phase

Abstract

During the common envelope (CE) phase, a giant star in a binary system overflows its Roche lobe and unstable mass transfer leads to a spiral-in of the companion, resulting in a close binary system or in a merger of the stellar cores. Dynamo processes during the CE phase have been proposed as a mechanism to generate magnetic fields that are important for forming magnetic white dwarfs (MWDs) and for shaping planetary nebulae. Here, we present the first magnetohydrodynamics simulations of the dynamical spiral-in during a CE phase. We find that magnetic fields are strongly amplified in the accretion stream around the $1M_{\odot }$ companion as it spirals into the envelope of a $2M_{\odot }$ RG. This leads to field strengths of 10 to 100 kG throughout the envelope after 120 d. The magnetic field amplification is consistent with being driven by the magnetorotational instability. The field strengths reached in our simulation make the magnetic field interesting for diagnostic purposes, but they are dynamically irrelevant. They are also too small to explain the formation of the highest fields found in MWDs, but may be relevant for luminous red novae, and detecting magnetic fields in these events would support the scenario as proposed here.

5 pages, 2 figures, 1 table. Accepted for publication in MNRAS Letters

References in corpus (9)

• Magnetic White Dwarfs
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Cited by in corpus (6)

• The impact of companions on stellar evolution
• Constructing stable 3D hydrodynamical models of giant stars
• Energy transport by convection in the common envelope evolution
• Energizing the last phase of common envelope removal
• Formation Scenario of the Progenitor of iPTF13bvn Revisited
• Common envelope: progress and transients