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2011ApJ...726...27P -
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Astrophys. J., 726, 27 (2011/January-1)
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An initial mass function for individual stars in galactic disks. I. Constraining the shape of the initial mass function.
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PARRAVANO A., McKEE C.F. and HOLLENBACH D.J.
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Abstract (from CDS):
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We derive a semi-empirical galactic initial mass function (IMF) from observational constraints. We assume that the IMF, ψ(m), is a smooth function of the stellar mass m. The mass dependence of the proposed IMF is determined by five parameters: the low-mass slope γ, the high-mass slope -Γ (taken to be -1.35), the characteristic mass m_{ch}(∼ the peak mass of the IMF), and the lower and upper limits on the mass, m_{ℓ} and m_{u}(taken to be 0.004 and 120 M_{☉}, respectively): ψ(m)dln m ∝ m ^{–Γ}{1 - exp [ - (m/m_{ch})^{γ+Γ}]}dln m. The values of γ and m_{ch} are derived from two integral constraints: (1) the ratio of the number density of stars in the range m = 0.1-0.6 M_{☉} to that in the range m = 0.6-0.8 M_{☉} as inferred from the mass distribution of field stars in the local neighborhood and (2) the ratio of the number of stars in the range m = 0.08-1 M_{☉} to the number of brown dwarfs in the range m = 0.03-0.08 M_{☉} in young clusters. The IMF satisfying the above constraints is characterized by the parameters γ = 0.51 and m_{ch}= 0.35 M_{☉}(which corresponds to a peak mass of 0.27 M_{☉} ). This IMF agrees quite well with the Chabrier IMF for the entire mass range over which we have compared with data, but predicts significantly more stars with masses <0.03 M_{☉}; we also compare with other IMFs in current use and give a number of important parameters implied by the IMFs.

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Abstract Copyright:
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Journal keyword(s):
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evolution - stars: formation - stars: luminosity function, mass function
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Simbad objects:
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18

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2019.12.08-20:15:59

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