PROBING INTERMEDIATE-MASS BLACK HOLES WITH OPTICAL EMISSION LINES FROM TIDALLY DISRUPTED WHITE DWARFS
- Department of Astronomy and Astrophysics and Center for Gravitational Wave Physics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802 (United States)
We calculate the emission-line spectrum produced by the debris released when a white dwarf (WD) is tidally disrupted by an intermediate-mass black hole (IMBH; M {approx} 10{sup 2}-10{sup 5} M{sub sun}) and we explore the possibility of using the emission lines to identify such events and constrain the properties of the IMBH. To this end, we adopt and adapt the techniques developed by Strubbe and Quataert to study the optical emission lines produced when a main-sequence star is tidally disrupted by a supermassive black hole (BH). WDs are tidally disrupted outside of the event horizon of a <10{sup 5} M{sub sun} BH, which makes these tidal disruption events good signposts of IMBHs. We focus on the optical and UV emission lines produced when the accretion flare photoionizes the stream of debris that remains unbound during the disruption. We find that the spectrum is dominated by lines due to ions of C and O, the strongest of which are C IV {lambda}1549 at early times and [O III] {lambda}5007 at later times. Furthermore, we model the profile of the emission lines in the [O III] {lambda}{lambda}4959, 5007 doublet and find that it is highly asymmetric with velocity widths of up to {approx}2500 km s{sup -1}, depending on the properties of the WD-IMBH system and the orientation of the observer. Finally, we compare the models with observations of X-ray flares and optical emission lines in the cores of globular clusters and propose how future observations can test if these features are due to a WD that has been tidally disrupted by an IMBH.
- OSTI ID:
- 21567712
- Journal Information:
- Astrophysical Journal, Vol. 726, Issue 1; Other Information: DOI: 10.1088/0004-637X/726/1/34; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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