| Issue |
A&A
Volume 648, April 2021
|
|
|---|---|---|
| Article Number | C3 | |
| Number of page(s) | 1 | |
| Section | Astrophysical processes | |
| DOI | https://doi.org/10.1051/0004-6361/201935917e | |
| Published online | 27 April 2021 | |
Bondi accretion for adiabatic flows onto a massive black hole with an accretion disc
The one dimensional problem (Corrigendum)
1
Environmental Physics Laboratory (EPHYSLAB), Facultad de Ciencias, Campus de Ourense, Universidad de Vigo, Ourense 32004, Spain
e-mail: josem.ramirez@gmail.com
2
School of Physical Sciences and Nanotechnology, Yachay Tech University, 100119 Urcuqui, Ecuador
3
Área de Física de Procesos Irreversibles, Departamento de Ciencias Básicas, Universidad Autónoma Metropolitana-Azcapotzalco (UAM-A), Av. San Pablo 180, 02200 Ciudad de México, Mexico
4
Instituto de Ciencias Básicas e Ingenierías, Universidad Autónoma del Estado de Hidalgo (UAEH), Ciudad Universitaria, Carretera Pachuca-Tulancingo km. 4.5 s/n, Colonia Carboneras, Mineral de la Reforma, 42184 Hidalgo, Mexico
5
Departamento de Física, Instituto Nacional de Investigaciones Nucleares (ININ), Carretera México-Toluca km. 36.5, La Marquesa, 52750 Ocoyoacac, Estado de México, Mexico
Key words: accretion, accretion disks / black hole physics / gravitation / hydrodynamics / line: formation / errata, addenda
A more appropriate observational reference for footnote 2 (page 4) of the article is:
For warm absorbers in AGNs, L ∼ 1043−46, nH ∼ 10(7−9), ξ ∼ (1−10), and r ∼ (1−10) pc (Ramírez et al. 2008). Physically, this distance seems to be a plausible location for warm absorber outflows to take place given the timescale variability of the central source and the ionization parameter, as well as the role that radiation pressure might be playing in these objects. We might adapt our calculations to other extragalactic sources, e.g. ultra-luminous sources (ULXs; Pinto et al. 2019) in the near future.
The second change is the value of μ in the footnote 5 (page 6). The correct value is μ = 0.7:
With T = 107 K, γ = 1.1, and μ = 0.7.
References
- Ramírez, J. M., Komossa, S., Burwitz, V., & Mathur, S. 2008, ApJ, 681, 965 [NASA ADS] [CrossRef] [Google Scholar]
© ESO 2021
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