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• W2006337514 endingPage "31" @default.
• W2006337514 startingPage "31" @default.
• W2006337514 abstract "Recent observations suggest that in black hole X-ray binaries jet/outflow formation is related to the hot plasma in the vicinity of the black hole, either in the form of an advection-dominated accretion flow at low accretion rates or in a disk corona at high accretion rates. We test the viability of this scenario for supermassive black holes using two samples of active galactic nuclei distinguished by the presence (radio-strong) and absence (radio-weak) of well-collimated, relativistic jets. Each is centered on a narrow range of black hole mass but spans a very broad range of Eddington ratios, effectively simulating, in a statistical manner, the behavior of a single black hole evolving across a wide spread in accretion states. Unlike the relationship between the radio and optical luminosity, which shows an abruptly break between high- and low-luminosity sources at an Eddington ratio of ~1, the radio emission-a measure of the jet power-varies continuously with the hard X-ray (2-10 keV) luminosity, roughly as L_R propto L_X^(0.6-0.75). This relation, which holds for both radio-weak and radio-strong active galaxies, is similar to the one seen in X-ray binaries. Jet/outflow formation appears to be closely linked to the conditions that give rise to the hot, optically thin coronal emission associated with accretion flows, both in the regime of low and high accretion rates." @default.
• W2006337514 created "2016-06-24" @default.
• W2006337514 creator A5010175299 @default.
• W2006337514 creator A5019522737 @default.
• W2006337514 creator A5052257716 @default.
• W2006337514 creator A5054184482 @default.
• W2006337514 date "2013-05-21" @default.
• W2006337514 modified "2023-10-03" @default.
• W2006337514 title "A PHYSICAL LINK BETWEEN JET FORMATION AND HOT PLASMA IN ACTIVE GALACTIC NUCLEI" @default.
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• W2006337514 doi "https://doi.org/10.1088/0004-637x/770/1/31" @default.
• W2006337514 hasPublicationYear "2013" @default.

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