{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1871428068073229184.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1007/978-94-011-4780-4_24"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.astro-ph/9810052"}}],"dc:title":[{"@value":"The Effect of Self-Gravity of Gas on Gas Fuelling in the Barred Galaxy with a Supermassive Black Hole"}],"description":[{"notation":[{"@value":"In our previous paper, we have shown that a gas disk in the nuclear region of a barred galaxy which contains a central supermassive black hole (SMBH) rapidly evolves into a nuclear gas ring by the effect of an additional inner Lindblad resonance caused by the SMBH. In this paper, we investigate the fate of the gas ring, involving self-gravity of gas, using two-dimensional hydrodynamical simulations. We find that the gas ring becomes gravitationally unstable for a gas surface density of gas above a critical value, and fragments into several gas clumps. Some denser clumps increase their mass via the accretion of the surrounding gas and collisions with other clumps, and finally a very massive gas clump (10^7 M_sun) is formed. Due to the torque from the most massive clump, a part of the gas in the ring loses its angular momentum and falls into the galactic center. As a result, a nuclear gas disk (50 pc) is formed around the SMBH. The accretion rate for $R<50$ pc attains about 1 M_sun/yr for 3.5*10^7 yr. At the final phase of the bar-driven fueling, self-gravity is crucial for the angular momentum transfer of the gas. This is a new mechanism for gas fueling to the vicinity of the SMBH."}]},{"notation":[{"@value":"14 pages, 7 figures, AASTeX, submitted to ApJ"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1891428068073229185","@type":"Researcher","foaf:name":[{"@value":"Asao Habe"}]},{"@id":"https://cir.nii.ac.jp/crid/1891428068073229186","@type":"Researcher","foaf:name":[{"@value":"Keiichi Wada"}]},{"@id":"https://cir.nii.ac.jp/crid/1891428068073229184","@type":"Researcher","foaf:name":[{"@value":"Hiroyuki Fukuda"}]}],"publication":{"dc:publisher":[{"@value":"Springer Netherlands"}],"prism:publicationDate":"1999-01-01"},"dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20(astro-ph)","dc:title":"Astrophysics (astro-ph)"},{"@id":"https://cir.nii.ac.jp/all?q=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics","dc:title":"Astrophysics"}],"dataSourceIdentifier":[{"@type":"OPENAIRE","@value":"doi_dedup___::d1a1dc248f380387175d751f1762a54f"}]}