Abstract
The fundamental premises concerning the existence of a universal basic distribution describing the initial mass functions (IMFs) of various astronomical objects on scales from brown dwarfs to clusters of galaxies are considered. This distribution has the form dN ∝ M−2dM, where M is the mass of an object and N the number of objects with a given mass. It is shown that, at least for objects forming as a result of fragmentation (e.g., stars, star clusters), the basis of this distribution may correspond to a white-noise model. The classical problem of the formation of the IMF for stars is discussed in this context, incuding the relationship between the mass function of protostellar clouds and the stellar IMF. The main factors determining the mass functions of galaxies and galaxy clusters are also considered.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
