The past star-formation rate and the initial mass-function in the solar neighbourhood

1986 ◽  
Vol 128 (1) ◽  
pp. 253-264
Author(s):  
Helmut Meusinger
Keyword(s):  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Mass Function ◽  
Initial Mass Function ◽  
Solar Neighbourhood ◽  
Initial Mass ◽  
The Past

scholarly journals A New Theory of Star Formation: Analytical Mass Function and Star Formation Rate

1987 ◽  
Vol 115 ◽  
pp. 442-443
Author(s):  
A. Di Fazio
Keyword(s):  
Mass Spectrum ◽  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Mass Function ◽  
Initial Mass Function ◽  
Time Dependent ◽  
Initial Mass ◽  
Fragmentation Rate

An analytical, theoretical, time-dependent initial mass function is derived for the objects created in the fragmentation of a gravitationally unstable gas protocloud. The mass spectrum depends on the chemical-dynamical-radiative evolution of the protocloud and it peaks at a mass slightly greater than the minimum Jeans mass attained throughout the evolution. A fragmentation rate mass spectrum is also analytically derived.

Star Formation in Cooling Flows (Invited Paper)

1987 ◽  
Vol 7 (2) ◽  
pp. 132-135 ◽  
Author(s):  
P. E. J. Nulsen ◽  
R. M. Johnstone ◽  
A. C. Fabian
Keyword(s):  
Star Formation ◽  
Formation Rate ◽  
Line Emission ◽  
Mass Function ◽  
Initial Mass Function ◽  
Solar Neighbourhood ◽  
Initial Mass ◽  
Ambient Conditions ◽  
Cooling Flows ◽  
Cooling Flow

AbstractX-ray data show that substantial quantities of hot gas are cooling near the centres of many clusters and groups of galaxies. The existence of such cooling flows has been challenged because of the lack of evidence for star formation from the cooled gas. Spectra of cooling flow galaxies show filling in of the continuum shortward of the break at 4000 Å relative to normal elliptical galaxies. This is consistent with some continuing star formation. Extended regions of line emission are commonly associated with cooling flows. If the initial-mass-function of the newly formed stars which affect the 4000 Å break is like that which applies in the solar neighbourhood, then these stars can also power the line emission. The strength of the 4000 Å break is shown to correlate with the Hβ flux in the manner expected when this is the case. This allows us to esimate the star formation rate from the line luminosity.The rate of star formation required to account for the line emission still falls well short of the rate at which gas is inferred to be cooling. It is argued that, nevertheless, the cooling gas is probably forming into stars. The overall initial-mass-function must be different from that which applies in the solar neighbourhood, but this should not be surprising given the different ambient conditions in a cooling flow.

Sign in / Sign up

Export Citation Format

Share Document