dc.contributor.author | Rueda, JA | |
dc.contributor.author | Rufini, R | |
dc.contributor.author | Wang, Y | |
dc.contributor.author | Bianco, CL | |
dc.contributor.author | Blanco-Iglesias, JM | |
dc.contributor.author | Karlica, M | |
dc.contributor.author | Loren-Aguilar, P | |
dc.contributor.author | Moradi, R | |
dc.contributor.author | Sahakyan, N | |
dc.date.accessioned | 2019-03-27T13:12:01Z | |
dc.date.issued | 2019-03-29 | |
dc.description.abstract | It has been recently proposed that the ejected matter from white dwarf (WD) binary mergers can produce transient, optical and infrared emission similar to the “kilonovae”
of neutron star (NS) binary mergers. To confirm this we calculate the electromagnetic emission from WD-WD mergers and compare with kilonova observations. We simulate WD-WD
mergers leading to a massive, fast rotating, highly magnetized WD with an adapted version of the smoothed-particle-hydrodynamics (SPH) code Phantom. We thus obtain initial
conditions for the ejecta such as escape velocity, mass and initial position and distribution.
The subsequent thermal and dynamical evolution of the ejecta is obtained by integrating the
energy-conservation equation accounting for expansion cooling and a heating source given
by the fallback accretion onto the newly-formed WD and its magneto-dipole radiation. We
show that magnetospheric processes in the merger can lead to a prompt, short gamma-ray
emission of up to ≈ 1046 erg in a timescale of 0.1–1 s. The bulk of the ejecta initially expands
non-relativistically with velocity 0.01 c and then it accelerates to 0.1 c due to the injection
of fallback accretion energy. The ejecta become transparent at optical wavelengths around
∼ 7 days post-merger with a luminosity 1041–1042 erg s−1
. The X-ray emission from the
fallback accretion becomes visible around ∼ 150–200 day post-merger with a luminosity of
1039 erg s−1
. We also predict the post-merger time at which the central WD should appear
as a pulsar depending on the value of the magnetic field and rotation period. | en_GB |
dc.description.sponsorship | Ministerio de Educación Cultura y Deporte | en_GB |
dc.identifier.citation | Published online 29 March 2019 | en_GB |
dc.identifier.doi | 10.1088/1475-7516/2019/03/044 | |
dc.identifier.uri | http://hdl.handle.net/10871/36651 | |
dc.language.iso | en | en_GB |
dc.publisher | IOP Publishing | en_GB |
dc.rights.embargoreason | Under embargo until 29 March 2020 in compliance with publisher policy | |
dc.title | Electromagnetic emission of white dwarf binary mergers | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2019-03-27T13:12:01Z | |
dc.identifier.issn | 1475-7516 | |
dc.description | This is the author accepted manuscript. The final version is available from IOP Publishing via the DOI in this record | en_GB |
dc.identifier.journal | Journal of Cosmology and Astroparticle Physics | en_GB |
dc.rights.uri | http://www.rioxx.net/licenses/all-rights-reserved | en_GB |
dcterms.dateAccepted | 2019-03-19 | |
rioxxterms.version | AM | en_GB |
rioxxterms.licenseref.startdate | 2019-03-19 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2019-03-27T10:36:45Z | |
refterms.versionFCD | AM | |
refterms.panel | B | en_GB |