NS-WD Accretion

From FRB Theory Wiki
Revision as of 08:56, 26 September 2018 by Emma Platts (talk | contribs) (Created page with " <!-- Brings in the summary table --> <!-- This is an example. Change the right hand side of all these assignments --> {{FRBTableTemplate |Category = Accretion...")
(diff) ← Older revision | Latest revision (diff) | Newer revision → (diff)
Jump to: navigation, search

Summary Table
Category Progenitor Type Energy Mechanism Emission Mechanism Counterparts References Brief Comments
LF Radio HF Radio Microwave Terahertz Optical/IR X-rays Gamma-rays Gravitational Waves Neutrinos
Accretion NS-WD Repeating Mag. reconnection Curv. Yes Yes -- -- -- -- -- -- -- http://adsabs.harvard.edu/abs/2016ApJ...823L..28G

Definitions: LF Radio (3 MHz to 3 GHz); HF Radio (3 GHz to 30 GHz); Microwave (30 to 300 GHz)

Model Description

This model considers the interaction between the bipolar magnetic �fields of a NS and a magnetic white dwarf (WD) as a possible origin of repeating FRBs. As the WD exceeds its Roche lobe, the NS accretes the infalling matter. Upon their approach, the magnetized materials may trigger magnetic reconnection and emit curvature radiation. In a rapidly rotating neutron star, the angular momentum added by accretion is lost to gravitational radiation, but the mass transfer may be violent enough for the angular momentum of the WD to dominate over the gravitational radiation. In this case, the WD is kicked away from the NS, and the process of accretion, and thus magnetic reconnection, may repeat. The timescale of emission is assumed to be the same as that of magnetic reconnection, and the time interval between adjacent bursts is derived from its relationship to the mass transferred by the �rst burst. There are multiple parameter sets that can describe a repeating FRB, an example of which produces timescales roughly consistent with FRB 121102. Counterparts to this model are not speci�ed, other than to say that possible gamma-ray emission from synchrotron radiation is unlikely detectable.

Observational Constraints