Please note that eDoc will be permanently shut down in the first quarter of 2021!      Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astrophysik     Collection: High Energy Astrophysics at MPA     Display Documents



  history
ID: 10373.0, MPI für Astrophysik / High Energy Astrophysics at MPA
Accretion onto the supermassive black hole in M87
Authors:Di Matteo, T.; Allen, S. W.; Fabian, A. C.; Wilson, A. S.; Young, A. J.
Language:English
Date of Publication (YYYY-MM-DD):2003-01-01
Title of Journal:The Astrophysical Journal
Journal Abbrev.:Astrophys. J.
Volume:582
Issue / Number:1
Start Page:133
End Page:140
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:Chandra X-ray observations of the giant elliptical galaxy M87 resolve the thermal state of the hot interstellar medium into the accretion (Bondi) radius of its central 3 x 10(9) M-circle dot black hole. We measure the X-ray gas temperature and density profiles and calculate the Bondi accretion rate, (M)over dot(Bondi) similar to 0.1 M-circle dot yr(-1). The X- ray luminosity of the active nucleus of M87 observed with Chandra is L-X,L-0.5-7 keV similar to 7 x 10(40) ergs s(-1). This value is much less than the predicted nuclear luminosity, L-Bondi similar to5 x 10(44) ergs s(-1), for accretion at the Bondi rate with a canonical accretion radiative efficiency of 10%. If the black hole in M87 accretes at this rate it must do so at a much lower radiative efficiency than the canonical value. The multiwavelength spectrum of the nucleus is consistent with that predicted by an advection-dominated flow. However, as is likely, the X-ray nucleus is dominated by jet emission then the properties of flow must be modified, possibly by out flows. We show that the overall energetics of the system are just consistent with the predicted Bondi nuclear power. This suggests that either most of the accretion energy is released in the relativistic jet or the central engine of M87 undergoes on-off activity cycles. We show that, at present, the energy dumped into the ISM by the jet may reduce the accretion rate onto the black hole by a factor proportional to (v(j)/c(s))(-2), where v(j) is the jet velocity and c(s) the ISM sound speed, and that this is sufficient to account for the low nuclear luminosity.
Free Keywords:accretion; accretion disks; black hole physics; galaxies : active; galaxies : individual (M87); galaxies : jets; X-rays : galaxies
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astrophysik
External Affiliations:Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA; 02138 USA; Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA; Max Planck Inst Astrophys, D-85740 Garching, Germany; Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15231 USA; Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England; Univ Maryland, Dept Astron, College Pk, MD 20742 USA
Identifiers:ISI:000180000600014
ISSN:0004-637X
URL:http://www.journals.uchicago.edu/ApJ/journal/issue...
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.