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Author Xiao, Di ♦ Dai, Zi-Gao
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ COMPARATIVE EVALUATIONS ♦ COSMIC X-RAY SOURCES ♦ DETECTION ♦ EFFICIENCY ♦ EMISSION ♦ GALAXIES ♦ LUMINOSITY ♦ MAGNETIC FIELDS ♦ NEUTRON STARS ♦ PULSARS ♦ RED SHIFT ♦ SOLAR RADIO BURSTS ♦ SPIN ♦ STELLAR WINDS
Abstract Recently, a precise (sub-arcsecond) localization of the repeating fast radio burst (FRB) 121102 led to the discovery of persistent radio and optical counterparts, the identification of a host dwarf galaxy at a redshift of z = 0.193, and several campaigns of searches for higher-frequency counterparts, which gave only upper limits on the emission flux. Although the origin of FRBs remains unknown, most of the existing theoretical models are associated with pulsars, or more specifically, magnetars. In this paper, we explore persistent high-energy emission from a rapidly rotating highly magnetized pulsar associated with FRB 121102 if internal gradual magnetic dissipation occurs in the pulsar wind. We find that the efficiency of converting the spin-down luminosity to the high-energy (e.g., X-ray) luminosity is generally much smaller than unity, even for a millisecond magnetar. This provides an explanation for the non-detection of high-energy counterparts to FRB 121102. We further constrain the spin period and surface magnetic field strength of the pulsar with the current high-energy observations. In addition, we compare our results with the constraints given by the other methods in previous works and expect to apply our new method to some other open issues in the future.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2017-09-10
Publisher Place United States
Journal Astrophysical Journal
Volume Number 846
Issue Number 2


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