X-ray-powered macronovae

Abstract

A macronova (or kilonova) was observed as an infrared excess several days after short gamma-ray burst, GRB 130603B. Although the $r$-process radioactivity is widely discussed as an energy source, it requires huge mass of ejecta from a neutron star (NS) binary merger. We propose a new model that the X-ray excess gives rise to the simultaneously observed infrared excess via thermal re-emission and explore what constraints this would place on the mass and velocity of the ejecta. This X-ray-powered model explains both the X-ray and infrared excesses with a single energy source by the central engine like a black hole, and allows for broader parameter region, in particular smaller ejecta mass $\sim 10^{-3}-10^{-2}{M}_{\odot }$ with iron mixed as suggested by general relativistic simulations for typical NS-NS mergers, than the previous models. We also discuss the other macronova candidates in GRB 060614 and GRB 080503, and implications for the search of electromagnetic counterparts to gravitational waves.

8 pages, 3 figures. Accepted for publication in Astrophysical Journal

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Cited by in corpus (37)

• The X-ray counterpart to the gravitational wave event GW 170817
• The Emergence of a Lanthanide-Rich Kilonova Following the Merger of Two Neutron Stars
• Swift and NuSTAR observations of GW170817: detection of a blue kilonova
• Kilonovae
• Kilonovae
• A Burst in a Wind Bubble and the Impact on Baryonic Ejecta: High-Energy Gamma-Ray Flashes and Afterglows from Fast Radio Bursts and Pulsar-Driven Supernova Remnants
• The Macronova in GRB 050709 and the GRB/macronova connection
• The electromagnetic counterparts of compact binary mergers
• First Multimessenger Observations of a Neutron Star Merger
• Long-lived Remnants from Binary Neutron Star Mergers
• Radioactive decay products in neutron star merger ejecta: heating efficiency and $\gamma$-ray emission
• Dynamics, nucleosynthesis, and kilonova signature of black hole - neutron star merger ejecta
• Gamma-ray burst progenitors
• Kilonova/Macronova Emission from Compact Binary Mergers
• Unveiling the Engines of Fast Radio Bursts, Super-Luminous Supernovae, and Gamma-Ray Bursts
• The Broad-band Counterpart of the Short GRB 200522A at $z=0.5536$: A Luminous Kilonova or a Collimated Outflow with a Reverse Shock?
• What Powered the Optical Transient AT2017gfo Associated with GW170817?
• Double Neutron Star Mergers and Short Gamma-Ray Bursts: Long-Lasting High-Energy Signatures and Remnant Dichotomy
• The lanthanide fraction distribution in metal-poor stars: a test of neutron star mergers as the dominant r-process site
• Bimodal Long-Lasting Components in Short Gamma-Ray Bursts: Promising Electromagnetic Counterparts to Neutron Star Binary Mergers
• Individual power density spectra of Swift gamma-ray bursts
• Are Ultra-Long Gamma-Ray Bursts Caused by Blue Supergiant Collapsars, Newborn Magnetars, or White Dwarf Tidal Disruption Events?
• Impact of Pulsar and Fallback Sources on Multifrequency Kilonova Models
• Is the macronova in GW170817 powered by the central engine?
• A Pulsar Wind Nebula Embedded in the Kilonova AT2017gfo Associated with GW 170817/GRB 170817A
• Subaru Hyper Suprime-Cam Survey for An Optical Counterpart of GW170817
• From Neutrino- to Photon-Cooled in Three Years: Can Fallback Accretion Explain the X-ray Excess in GW170817?
• Intermediate Luminosity Red Transients by Black Holes Born from Erupting Massive Stars
• Probing the Birth of Post-merger Millisecond Magnetars by X-ray and Gamma-ray Emission
• Linking extended and plateau emissions of short gamma-ray bursts
• Constraining the long-lived supramassive neutron stars by magnetar boosted kilonovae
• Fallback Accretion Model for the Years-to-Decades X-ray Counterpart to GW170817
• Correlation between peak energy and Fourier power density spectrum slope in gamma-ray bursts
• What if GW190425 did not produce a black hole promptly?
• Polarization of the first-hour macronovae
• Revealing physical activity of GRB central engine with macronova/kilonova data
• Features and prospects for kilonova remnant detection with current and future surveys