Simple analytic formula relating the mass and spin of accreting compact objects to their rapid X-ray variability
Following the previous research on epicyclic oscillations of accretion disks around black holes (BHs) and neutron stars (NSs), a new model of high-frequency quasi-periodic oscillations (QPOs) has been proposed (CT model), which deals with oscillations of fluid in marginally overflowing accretion tor...
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description | Following the previous research on epicyclic oscillations of accretion disks around black holes (BHs) and neutron stars (NSs), a new model of high-frequency quasi-periodic oscillations (QPOs) has been proposed (CT model), which deals with oscillations of fluid in marginally overflowing accretion tori (i.e., tori terminated by cusps). According to preliminary investigations, the model provides better fits of the NS QPO data compared to the relativistic precession (RP) model. It also implies a significantly higher upper limit on the Galactic microquasars BH spin. A short analytic formula has been noticed to well reproduce the model's predictions on the QPO frequencies in Schwarzschild spacetimes. Here we derive an extended version of this formula that applies to rotating compact objects. We start with the consideration of Kerr spacetimes and derive a formula that is not restricted to a particular specific angular momentum distribution of the inner accretion flow, such as Keplerian or constant. Finally, we consider Hartle-Thorne spacetimes and include corrections implied by the NS oblateness. For a particular choice of a single parameter, our relation provides frequencies predicted by the CT model. For another value, it provides frequencies predicted by the RP model. We conclude that the formula is well applicable for rotating oblateness NSs and both models. We briefly illustrate application of our simple formula on several NS sources and confirm the expectation that the CT model is compatible with realistic values of the NS mass and provides better fits of data than the RP model. |
doi_str_mv | 10.48550/arxiv.2203.04787 |
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According to preliminary investigations, the model provides better fits of the NS QPO data compared to the relativistic precession (RP) model. It also implies a significantly higher upper limit on the Galactic microquasars BH spin. A short analytic formula has been noticed to well reproduce the model's predictions on the QPO frequencies in Schwarzschild spacetimes. Here we derive an extended version of this formula that applies to rotating compact objects. We start with the consideration of Kerr spacetimes and derive a formula that is not restricted to a particular specific angular momentum distribution of the inner accretion flow, such as Keplerian or constant. Finally, we consider Hartle-Thorne spacetimes and include corrections implied by the NS oblateness. For a particular choice of a single parameter, our relation provides frequencies predicted by the CT model. For another value, it provides frequencies predicted by the RP model. We conclude that the formula is well applicable for rotating oblateness NSs and both models. We briefly illustrate application of our simple formula on several NS sources and confirm the expectation that the CT model is compatible with realistic values of the NS mass and provides better fits of data than the RP model.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2203.04787</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Accretion disks ; Angular momentum ; Black holes ; Neutron stars ; Physics - High Energy Astrophysical Phenomena ; Quasi-Periodic Oscillations ; Rotation ; Spacetime ; Toruses</subject><ispartof>arXiv.org, 2022-03</ispartof><rights>2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2203.04787$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.3847/1538-4357/ac5ab6$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Török, Gabriel</creatorcontrib><creatorcontrib>Kotrlová, Andrea</creatorcontrib><creatorcontrib>Matuszková, Monika</creatorcontrib><creatorcontrib>Klimovičová, Kateřina</creatorcontrib><creatorcontrib>Lančová, Debora</creatorcontrib><creatorcontrib>Urbancová, Gabriela</creatorcontrib><creatorcontrib>Šrámková, Eva</creatorcontrib><title>Simple analytic formula relating the mass and spin of accreting compact objects to their rapid X-ray variability</title><title>arXiv.org</title><description>Following the previous research on epicyclic oscillations of accretion disks around black holes (BHs) and neutron stars (NSs), a new model of high-frequency quasi-periodic oscillations (QPOs) has been proposed (CT model), which deals with oscillations of fluid in marginally overflowing accretion tori (i.e., tori terminated by cusps). According to preliminary investigations, the model provides better fits of the NS QPO data compared to the relativistic precession (RP) model. It also implies a significantly higher upper limit on the Galactic microquasars BH spin. A short analytic formula has been noticed to well reproduce the model's predictions on the QPO frequencies in Schwarzschild spacetimes. Here we derive an extended version of this formula that applies to rotating compact objects. We start with the consideration of Kerr spacetimes and derive a formula that is not restricted to a particular specific angular momentum distribution of the inner accretion flow, such as Keplerian or constant. Finally, we consider Hartle-Thorne spacetimes and include corrections implied by the NS oblateness. For a particular choice of a single parameter, our relation provides frequencies predicted by the CT model. For another value, it provides frequencies predicted by the RP model. We conclude that the formula is well applicable for rotating oblateness NSs and both models. We briefly illustrate application of our simple formula on several NS sources and confirm the expectation that the CT model is compatible with realistic values of the NS mass and provides better fits of data than the RP model.</description><subject>Accretion disks</subject><subject>Angular momentum</subject><subject>Black holes</subject><subject>Neutron stars</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Quasi-Periodic Oscillations</subject><subject>Rotation</subject><subject>Spacetime</subject><subject>Toruses</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkD1PwzAURS0kJKrSH8CEJeYU5zl2nBFVfFSqxEAHtujFccBVUhvbrci_J22ZnnTfuXc4hNzlbFkoIdgjhl97XAIwvmRFqcorMgPO80wVADdkEeOOMQayBCH4jPgPO_jeUNxjPyaraefCcOiRBtNjsvsvmr4NHTDGCWlp9HZPXUdR62DOb-0GjzpR1-yMTpEmd2rYQAN629LPLOBIjxgsNra3abwl1x320Sz-75xsX563q7ds8_66Xj1tMhTAM5BFrvIiF5VpmQSlVakLJSVMqa44L6sWWmhy2UltjJKsaISqpGpF00hoGZ-T-8vsWUftgx0wjPVJS33WMhEPF8IH93MwMdU7dwiThliD5KUCNrH8Dw9wZVs</recordid><startdate>20220309</startdate><enddate>20220309</enddate><creator>Török, Gabriel</creator><creator>Kotrlová, Andrea</creator><creator>Matuszková, Monika</creator><creator>Klimovičová, Kateřina</creator><creator>Lančová, Debora</creator><creator>Urbancová, Gabriela</creator><creator>Šrámková, Eva</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20220309</creationdate><title>Simple analytic formula relating the mass and spin of accreting compact objects to their rapid X-ray variability</title><author>Török, Gabriel ; 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According to preliminary investigations, the model provides better fits of the NS QPO data compared to the relativistic precession (RP) model. It also implies a significantly higher upper limit on the Galactic microquasars BH spin. A short analytic formula has been noticed to well reproduce the model's predictions on the QPO frequencies in Schwarzschild spacetimes. Here we derive an extended version of this formula that applies to rotating compact objects. We start with the consideration of Kerr spacetimes and derive a formula that is not restricted to a particular specific angular momentum distribution of the inner accretion flow, such as Keplerian or constant. Finally, we consider Hartle-Thorne spacetimes and include corrections implied by the NS oblateness. For a particular choice of a single parameter, our relation provides frequencies predicted by the CT model. For another value, it provides frequencies predicted by the RP model. We conclude that the formula is well applicable for rotating oblateness NSs and both models. We briefly illustrate application of our simple formula on several NS sources and confirm the expectation that the CT model is compatible with realistic values of the NS mass and provides better fits of data than the RP model.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2203.04787</doi><oa>free_for_read</oa></addata></record> |
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subjects | Accretion disks Angular momentum Black holes Neutron stars Physics - High Energy Astrophysical Phenomena Quasi-Periodic Oscillations Rotation Spacetime Toruses |
title | Simple analytic formula relating the mass and spin of accreting compact objects to their rapid X-ray variability |
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