On Disk Formation around Isolated Black Holes via Stream Accretion
We investigate accretion onto an isolated black hole from uniform winds. If the winds are directed toward the black hole, then the accretion process can be well described by the classical Bondi–Hoyle–Lyttleton or BHL accretion. If the wind is not directed toward the black hole and flows past it, the...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad9b96 |
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| author | Priyesh Kumar Tripathi Indranil Chattopadhyay Raj Kishor Joshi |
| author_facet | Priyesh Kumar Tripathi Indranil Chattopadhyay Raj Kishor Joshi |
| author_sort | Priyesh Kumar Tripathi |
| collection | DOAJ |
| description | We investigate accretion onto an isolated black hole from uniform winds. If the winds are directed toward the black hole, then the accretion process can be well described by the classical Bondi–Hoyle–Lyttleton or BHL accretion. If the wind is not directed toward the black hole and flows past it, then a smaller fraction of the flow can be attracted by the black hole, and this type of accretion cannot be described by the classical BHL, and we coin the second kind as the lateral BHL. We show that the classical BHL cannot form an accretion disk, while lateral BHL can form transient accretion disks. To describe the thermodynamics of the flow, we have used a variable adiabatic index equation of state which depends on the temperature of the flow as well as the composition of the gas. We show that the electron-proton gas forms an accretion disk, which disappears and forms a shock cone, only to form the disk again at a later time, while for flows with fewer protons, the accretion disk, once lost, does not reappear again. Only when the flow is pair-dominated does it form a persistent accretion disk. We also show that a shock cone is less luminous than the accretion disk. |
| format | Article |
| id | doaj-art-16a07a90d7b94c9280d96f1b122d413b |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-16a07a90d7b94c9280d96f1b122d413b2025-01-20T14:59:35ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197916110.3847/1538-4357/ad9b96On Disk Formation around Isolated Black Holes via Stream AccretionPriyesh Kumar Tripathi0https://orcid.org/0009-0002-7498-6899Indranil Chattopadhyay1https://orcid.org/0000-0002-2133-9324Raj Kishor Joshi2https://orcid.org/0000-0002-9036-681XAryabhatta Research Institute of Observational Sciences (ARIES) , Manora Peak, Nainital 263001, India; Department of Applied Physics, Mahatma Jyotiba Phule Rohilkhand University , Bareilly 243006, IndiaAryabhatta Research Institute of Observational Sciences (ARIES) , Manora Peak, Nainital 263001, IndiaAryabhatta Research Institute of Observational Sciences (ARIES) , Manora Peak, Nainital 263001, IndiaWe investigate accretion onto an isolated black hole from uniform winds. If the winds are directed toward the black hole, then the accretion process can be well described by the classical Bondi–Hoyle–Lyttleton or BHL accretion. If the wind is not directed toward the black hole and flows past it, then a smaller fraction of the flow can be attracted by the black hole, and this type of accretion cannot be described by the classical BHL, and we coin the second kind as the lateral BHL. We show that the classical BHL cannot form an accretion disk, while lateral BHL can form transient accretion disks. To describe the thermodynamics of the flow, we have used a variable adiabatic index equation of state which depends on the temperature of the flow as well as the composition of the gas. We show that the electron-proton gas forms an accretion disk, which disappears and forms a shock cone, only to form the disk again at a later time, while for flows with fewer protons, the accretion disk, once lost, does not reappear again. Only when the flow is pair-dominated does it form a persistent accretion disk. We also show that a shock cone is less luminous than the accretion disk.https://doi.org/10.3847/1538-4357/ad9b96AccretionAstrophysical black holesHydrodynamical simulationsShocks |
| spellingShingle | Priyesh Kumar Tripathi Indranil Chattopadhyay Raj Kishor Joshi On Disk Formation around Isolated Black Holes via Stream Accretion The Astrophysical Journal Accretion Astrophysical black holes Hydrodynamical simulations Shocks |
| title | On Disk Formation around Isolated Black Holes via Stream Accretion |
| title_full | On Disk Formation around Isolated Black Holes via Stream Accretion |
| title_fullStr | On Disk Formation around Isolated Black Holes via Stream Accretion |
| title_full_unstemmed | On Disk Formation around Isolated Black Holes via Stream Accretion |
| title_short | On Disk Formation around Isolated Black Holes via Stream Accretion |
| title_sort | on disk formation around isolated black holes via stream accretion |
| topic | Accretion Astrophysical black holes Hydrodynamical simulations Shocks |
| url | https://doi.org/10.3847/1538-4357/ad9b96 |
| work_keys_str_mv | AT priyeshkumartripathi ondiskformationaroundisolatedblackholesviastreamaccretion AT indranilchattopadhyay ondiskformationaroundisolatedblackholesviastreamaccretion AT rajkishorjoshi ondiskformationaroundisolatedblackholesviastreamaccretion |