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Article: Thin accretion disk signatures of slowly rotating black holes in Horava gravity

TitleThin accretion disk signatures of slowly rotating black holes in Horava gravity
Authors
KeywordsGravitation and cosmology
Astrophysics and astroparticles
Issue Date2011
PublisherInstitute of Physics Publishing. The Journal's web site is located at http://www.iop.org/EJ/cqg
Citation
Classical and Quantum Gravity, 2011, v. 28 n. 16, article no. 165001 How to Cite?
AbstractIn this work, we consider the possibility of observationally testing Hořava gravity by using the accretion disk properties around slowly rotating black holes of the Kehagias–Sfetsos (KS) solution in asymptotically flat spacetimes. The energy flux, temperature distribution, the emission spectrum as well as the energy conversion efficiency are obtained, and compared to the standard slowly rotating general relativistic Kerr solution. Comparing the mass accretion in a slowly rotating KS geometry in Hořava gravity with the one of a slowly rotating Kerr black hole, we verify that the intensity of the flux emerging from the disk surface is greater for the slowly rotating Kehagias–Sfetsos solution than for rotating black holes with the same geometrical mass and accretion rate. We also present the conversion efficiency of the accreting mass into radiation, and show that the rotating KS solution provides a much more efficient engine for the transformation of the accreting mass into radiation than the Kerr black holes. Thus, distinct signatures appear in the electromagnetic spectrum, leading to the possibility of directly testing Hořava gravity models by using astrophysical observations of the emission spectra from accretion disks.
Persistent Identifierhttp://hdl.handle.net/10722/145572
ISSN
2015 Impact Factor: 2.837
2015 SCImago Journal Rankings: 1.633
ISI Accession Number ID
Funding AgencyGrant Number
government of the Hong Kong SAR
Fundacao para a Ciencia e TecnologiaPTDC/FIS/102742/2008
CERN/FP/109381/2009
Funding Information:

The work of TH is supported by an RGC grant of the government of the Hong Kong SAR. FSNL acknowledges financial support of the Fundacao para a Ciencia e Tecnologia through the grants PTDC/FIS/102742/2008 and CERN/FP/109381/2009.

 

DC FieldValueLanguage
dc.contributor.authorHarko, TCen_US
dc.contributor.authorKovacs, Zen_US
dc.contributor.authorLobo, SSN-
dc.date.accessioned2012-02-28T01:55:38Z-
dc.date.available2012-02-28T01:55:38Z-
dc.date.issued2011en_US
dc.identifier.citationClassical and Quantum Gravity, 2011, v. 28 n. 16, article no. 165001en_US
dc.identifier.issn0264-9381-
dc.identifier.urihttp://hdl.handle.net/10722/145572-
dc.description.abstractIn this work, we consider the possibility of observationally testing Hořava gravity by using the accretion disk properties around slowly rotating black holes of the Kehagias–Sfetsos (KS) solution in asymptotically flat spacetimes. The energy flux, temperature distribution, the emission spectrum as well as the energy conversion efficiency are obtained, and compared to the standard slowly rotating general relativistic Kerr solution. Comparing the mass accretion in a slowly rotating KS geometry in Hořava gravity with the one of a slowly rotating Kerr black hole, we verify that the intensity of the flux emerging from the disk surface is greater for the slowly rotating Kehagias–Sfetsos solution than for rotating black holes with the same geometrical mass and accretion rate. We also present the conversion efficiency of the accreting mass into radiation, and show that the rotating KS solution provides a much more efficient engine for the transformation of the accreting mass into radiation than the Kerr black holes. Thus, distinct signatures appear in the electromagnetic spectrum, leading to the possibility of directly testing Hořava gravity models by using astrophysical observations of the emission spectra from accretion disks.-
dc.languageengen_US
dc.publisherInstitute of Physics Publishing. The Journal's web site is located at http://www.iop.org/EJ/cqgen_US
dc.relation.ispartofClassical and Quantum Gravityen_US
dc.rightsClassical and Quantum Gravity. Copyright © Institute of Physics Publishing.-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectGravitation and cosmology-
dc.subjectAstrophysics and astroparticles-
dc.titleThin accretion disk signatures of slowly rotating black holes in Horava gravityen_US
dc.typeArticleen_US
dc.identifier.emailHarko, TC: harko@hkucc.hku.hken_US
dc.identifier.emailKovacs, Z: zkovacs@hku.hken_US
dc.identifier.emailLobo, SSN: flobo@cii.fc.ul.pt-
dc.identifier.authorityHarko, TC=rp01333en_US
dc.description.naturepostprint-
dc.identifier.doi10.1088/0264-9381/28/16/165001-
dc.identifier.scopuseid_2-s2.0-80051779477-
dc.identifier.hkuros198639en_US
dc.identifier.volume28en_US
dc.identifier.issue16, article no. 165001-
dc.identifier.isiWOS:000294010300016-
dc.publisher.placeUnited Kingdom-
dc.identifier.citeulike9599228-

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