Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1559
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dc.contributor.authorBasu, S-
dc.date.accessioned2007-05-10T05:18:09Z-
dc.date.available2007-05-10T05:18:09Z-
dc.date.issued1993-
dc.identifier.citationBASI, Vol. 21, pp. 583-586en
dc.identifier.urihttp://hdl.handle.net/2248/1559-
dc.description.abstractThe Galactic disk is supposed to have been formed from gas condensing out from the halo. The rate at which this infall of gas occurs, the amount of infall, and the time scales over which gas falls on to the disc have important consequences for the chemical evolution of the Galaxy. However there are large uncertainties in the observed data about infall, and even basic questions like the actual origin of the gas, the amount of infall etc., have not been answered. In this work, we have used the observed metallicity distribution of low mass stars (the G-dwarf distribution) and the age-metallicity relation (AMR) to constrain the amount of infall and the infall time scale. Along with the infall time scales the history of star formation in the solar neighborhood can also be determineden
dc.format.extent307944 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.subjectChemical evolutionen
dc.subjectMilkly wave galaxyen
dc.titleThe infall time-scale in the solar neighborhooden
dc.typeArticleen
Appears in Collections:BASI Publications

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