Universal relations with fermionic dark matter
We have recently introduced a new model for the distribution of dark matter (DM) in galaxies, the Ruffini-Argüelles-Rueda (RAR) model, based on a self-gravitating system of massive fermions at finite temperatures. The RAR model, for fermion masses above keV, successfully describes the DM halos in ga...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
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EDP Sciences
2018-01-01
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| Series: | EPJ Web of Conferences |
| Online Access: | https://doi.org/10.1051/epjconf/201816804015 |
| _version_ | 1819299402261463040 |
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| author | Krut A. Argüelles C. R. Rueda J. A. Ruffini R. |
| author_facet | Krut A. Argüelles C. R. Rueda J. A. Ruffini R. |
| author_sort | Krut A. |
| collection | DOAJ |
| description | We have recently introduced a new model for the distribution of dark matter (DM) in galaxies, the Ruffini-Argüelles-Rueda (RAR) model, based on a self-gravitating system of massive fermions at finite temperatures. The RAR model, for fermion masses above keV, successfully describes the DM halos in galaxies, and predicts the existence of a denser quantum core towards the center of each configuration. We demonstrate here, for the first time, that the introduction of a cutoff in the fermion phase-space distribution, necessary to account for galaxies finite size and mass, defines a new solution with a compact quantum core which represents an alternative to the central black hole (BH) scenario for SgrA*. For a fermion mass in the range 48keV ≤ mc2 ≤ 345keV, the DM halo distribution fulfills the most recent data of the Milky Way rotation curves while harbors a dense quantum core of 4×106M⊙ within the S2 star pericenter. In particular, for a fermion mass of mc2 ∼ 50keV the model is able to explain the DM halos from typical dwarf spheroidal to normal elliptical galaxies, while harboring dark and massive compact objects from ∼ 103M⊙ tp to 108M⊙ at their respective centers. The model is shown to be in good agreement with different observationally inferred universal relations, such as the ones connecting DM halos with supermassive dark central objects. Finally, the model provides a natural mechanism for the formation of supermassive BHs as heavy as few ∼ 108M⊙. We argue that larger BH masses (few ∼ 109−10M⊙) may be achieved by assuming subsequent accretion processes onto the above heavy seeds, depending on accretion efficiency and environment. |
| first_indexed | 2024-12-24T05:45:13Z |
| format | Article |
| id | doaj.art-922909b35bd44f4c84af5a676379312c |
| institution | Directory Open Access Journal |
| issn | 2100-014X |
| language | English |
| last_indexed | 2024-12-24T05:45:13Z |
| publishDate | 2018-01-01 |
| publisher | EDP Sciences |
| record_format | Article |
| series | EPJ Web of Conferences |
| spelling | doaj.art-922909b35bd44f4c84af5a676379312c2022-12-21T17:12:36ZengEDP SciencesEPJ Web of Conferences2100-014X2018-01-011680401510.1051/epjconf/201816804015epjconf_icgaxiii-ik2018_04015Universal relations with fermionic dark matterKrut A.Argüelles C. R.Rueda J. A.Ruffini R.We have recently introduced a new model for the distribution of dark matter (DM) in galaxies, the Ruffini-Argüelles-Rueda (RAR) model, based on a self-gravitating system of massive fermions at finite temperatures. The RAR model, for fermion masses above keV, successfully describes the DM halos in galaxies, and predicts the existence of a denser quantum core towards the center of each configuration. We demonstrate here, for the first time, that the introduction of a cutoff in the fermion phase-space distribution, necessary to account for galaxies finite size and mass, defines a new solution with a compact quantum core which represents an alternative to the central black hole (BH) scenario for SgrA*. For a fermion mass in the range 48keV ≤ mc2 ≤ 345keV, the DM halo distribution fulfills the most recent data of the Milky Way rotation curves while harbors a dense quantum core of 4×106M⊙ within the S2 star pericenter. In particular, for a fermion mass of mc2 ∼ 50keV the model is able to explain the DM halos from typical dwarf spheroidal to normal elliptical galaxies, while harboring dark and massive compact objects from ∼ 103M⊙ tp to 108M⊙ at their respective centers. The model is shown to be in good agreement with different observationally inferred universal relations, such as the ones connecting DM halos with supermassive dark central objects. Finally, the model provides a natural mechanism for the formation of supermassive BHs as heavy as few ∼ 108M⊙. We argue that larger BH masses (few ∼ 109−10M⊙) may be achieved by assuming subsequent accretion processes onto the above heavy seeds, depending on accretion efficiency and environment.https://doi.org/10.1051/epjconf/201816804015 |
| spellingShingle | Krut A. Argüelles C. R. Rueda J. A. Ruffini R. Universal relations with fermionic dark matter EPJ Web of Conferences |
| title | Universal relations with fermionic dark matter |
| title_full | Universal relations with fermionic dark matter |
| title_fullStr | Universal relations with fermionic dark matter |
| title_full_unstemmed | Universal relations with fermionic dark matter |
| title_short | Universal relations with fermionic dark matter |
| title_sort | universal relations with fermionic dark matter |
| url | https://doi.org/10.1051/epjconf/201816804015 |
| work_keys_str_mv | AT kruta universalrelationswithfermionicdarkmatter AT arguellescr universalrelationswithfermionicdarkmatter AT ruedaja universalrelationswithfermionicdarkmatter AT ruffinir universalrelationswithfermionicdarkmatter |