Ram-pressure stripping of a kicked Hill sphere: Prompt electromagnetic emission from the merger of stellar mass black holes in an AGN accretion disk

B. McKernan; K. E. S. Ford; I. Bartos; M. J. Graham; W. Lyra; S. Marka; Z. Marka; N. P. Ross; D. Stern; Y. Yang

doi:10.3847/2041-8213/ab4886

paper

Ram-pressure stripping of a kicked Hill sphere: Prompt electromagnetic emission from the merger of stellar mass black holes in an AGN accretion disk

arXiv:1907.03746 · doi:10.3847/2041-8213/ab4886

Abstract

Accretion disks around supermassive black holes (SMBH) are promising sites for stellar mass black hole (BH) mergers due to mass segregation and merger acceleration by disk gas torques. Here we show that a GW-kick at BH merger causes ram-pressure stripping of gas within the BH Hill sphere. If $R_{H} \geq H$ , the disk height, an off-center UV flare at $a_{BH} \sim 1 0^{3} r_{g}$ emerges within $t_{UV} \sim O (2 days) (a_{BH} /1 0^{3} r_{g}) (M_{SMBH} /1 0^{8} M_{⊙}) (v_{kick} /1 0^{2} km/s)$ post-merger and lasts O $(R_{H} / v_{kick}) \sim O (5 t_{UV}$ ). The flare emerges with luminosity O( $1 0^{42} erg/s) (t_{UV} /2 days)^{- 1} (M_{Hill} /1 M_{⊙}) (v_{kick} /1 0^{2} km/s)^{2}$ . AGN optical/UV photometry alters and asymmetric broad emission line profiles can develop after weeks. If $R_{H} < H$ , detectability depends on disk optical depth. Follow-up by large optical sky surveys is optimized for small GW error volumes and for LIGO/Virgo triggers $> 50 M_{⊙}$ .

arXiv comment5pages, 2 figures, ApJL (accepted)

Ram-pressure stripping of a kicked Hill sphere: Prompt electromagnetic emission from the merger of stellar mass black holes in an AGN accretion disk

Abstract

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