Kavli Affiliate: Erin Kara
| Summary:
The X-ray source in AGN is commonly referred to as the corona by analogy to stellar coronae. The similarities between the two suggest that the heating mechanism of AGN coronae is magnetic reconnection — as in cool stars — but this has not yet been directly observed. This work presents the first observational evidence for a magnetic reconnection flare in an AGN corona. We report on a flare in NGC 3783, which was observed with XRISM/Xtend and XMM-Newton/EPIC-PN exhibiting distinct temporal evolution in soft ($<2.0,$keV) and hard ($>2.0,$keV) X-rays. An Ultra-Fast Outflow (UFO) was detected during the event. The flare features the Neupert effect — a temporal signature widely observed in the Sun, which shows that the flare is powered by magnetic reconnection, with the UFO playing a role analogous to a solar Coronal Mass Ejection (CME). We derive an upper limit of $30 , R_g$ on the height of the magnetic loop from which the flare originates. Using the UFO’s measured properties to characterize the magnetic field, we obtain $B > 1.3 times 10^4,$G for the field annihilated during the flare from total energy considerations, and $B approx 500,$G for the momentary magnetic field during reconnection from a dynamical consideration.
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