Magnetic Activity in Stellar Merger Products

Abstract

We study the expected X-ray luminosity of stellar merger products several years after merger. The X-ray emission is assumed to result from magnetic activity. The extended envelope of the merger product possesses a large convective region and it is expected to rotate fast. The rotation and convection might give rise to an efficient dynamo operation, therefore we expect strong magnetic activity. Using well known relations connecting magnetic activity and X-ray luminosity in other types of magnetically active stars, we estimate that the strong X-ray luminosity will start several years after merger, will reach a maximum of L_x~3x10^{30} erg/sec, and will slowly decline on a time scale of ~100 years. We predict that X-ray emission from V838 Mon which erupted in 2002 will be detected in 2008 with 20 hours of observation.

MNRAS, in press

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• Direct detection of a magnetic field in the photosphere of the single M giant EK Boo: How common is magnetic activity among M giants?
• Magnetically powered outbursts from white dwarf mergers
• An analysis of a spectrum of V838 Monocerotis in October 2005
• The continued optical to mid-IR evolution of V838 Monocerotis
• Dusty, Self-obscured Transients from Stellar Coalescence
• Lithium in coalesced non-compact stars
• Searching for the Next Galactic Luminous Red Nova
• XMM-Newton detection of a transient X-ray source in the vicinity of V838 Monocerotis
• V838 Monocerotis as seen by ALMA: a remnant of a binary merger in a triple system
• X-ray emission from candidate stellar merger remnant TYC 2597-735-1 and its Blue Ring Nebula