Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...290....7b&link_type=abstract
Astronomy and Astrophysics 290, 7-18 (1994)
Astronomy and Astrophysics
Astrophysics
26
Galaxies: Interactions, Kinematics, And Dynamics, Active, Nuclei, Ism
Scientific paper
Merging galaxies sometimes show quasar-like activity, which suggests that the interstellar gas is efficiently transferred to the vicinity of their nucleus (where a massive black hole is considered to exist.). In order to elucidate gas fueling mechanism in galaxy mergers, we have numerically investigated the dynamical evolution of gas in the late phase of mergers. It is found that in some cases (e.g., a retrograde merger involving two compact galaxy cores), the dynamical heating by two sinking cores and subsequent dissipative cloud-cloud collisions drive a large fraction of disk gas (~10^8^Msun_) into the central 10pc. It is also found that most of models have shown a qualitatively similar behavior that gas infall to the central 10pc becomes prominent only after the coalescence of two cores. This tendency of nuclear activity remains unchanged even if we include gas consumption by star formation in our models. Our numerical study predicts that the radiation emitted from the nuclear region of completed mergers showing a single nucleus originates from accretion power induced activity around a massive black hole whereas star formation is prime energy source of the radiation from less advanced mergers showing two distinct nuclei.
Bekki Kenji
Noguchi Masayuki
No associations
LandOfFree
Gas fueling to the central 10pc in merging galaxies. does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Gas fueling to the central 10pc in merging galaxies., we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Gas fueling to the central 10pc in merging galaxies. will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1067295