mass function

mass function

1. The only information that can be determined about the masses m 1 and m 2 of the two components of a spectroscopic binary when the spectral lines of only one component (of mass m 1) can be observed. It is equal to
(m 2 3 sin3 i )/(m 1 + m 2 )2
where m 1 and m 2 are measured in solar masses and i is the inclination of the orbit.
2. (Salpeter mass function) See stellar mass.
References in periodicals archive ?
The team used detailed analyses of about 250 stars with masses between 15 and 200 times the mass of our Sun to determine the distribution of massive stars born in 30 Doradus -- the so-called initial mass function (IMF).
The shape of the mass function is shown as the red dash line in Figure (5).
By further developing my cosmological chemical-evolution models, and exploiting the huge, unique, and already available data-sets for ancient Local group stars, I will simultaneously study the chemical evolution of the Milky Way and its dwarf satellites to: 1) define the host environment (halo regions, dwarf galaxies) and properties (chemistry, kinematics) of second-generation stars; 2) select candidates for high-resolution spectroscopic follow-up; 3) constrain strongly the primordial initial mass function.
Keeping the math at an algebra level, this handbook explains the probability mass function and distributional parameters for discrete uniform, binomial, multinomial, hypergeometric, geometric, negative binomial, and Poisson distributions.
Furthermore, it is also possible to trace the mass function of SMBHs (including non-active SMBHs) from the AGN luminosity function by neglecting merging of SMBHs.
As foundation of evidence combination and key content of D-S theory, mass function represents supporting degree of events happening.
where H(Y | Z) is estimated from the probability mass function of Y and Z, and is compared with a threshold to decide the current knowledge of the PU.
He said that if this result is confirmed by future studies it would mean that the initial mass function is not dependent on how the stars form but on the availability of material nearby the embryonic stars from which they accrete their mass.
Initial results suggest that the level of substructure observed in dark matter haloes is higher, with a flatter mass function, than to what is expected from simulations of galaxy formation.