scholarly journals Mass Distribution of elementary fermions

2021 ◽  
Author(s):  
Li-Gong Mishulan
Keyword(s):  
Observational Data ◽  
Mass Distribution ◽  
Neutrino Oscillations ◽  
Careful Analysis ◽  
Geometric Progression ◽  
The Masses

Abstract Through careful analysis of the observational data on the mass of elementary fermions, we determine that an intrinsic pattern does exist. A geometric progression is proposed to describe the mass distribution of elementary fermions, and using the observational data of neutrino oscillations, we estimate the masses of neutrino.

scholarly journals A geometric progression on the mass of elementary fermions

2021 ◽  
Author(s):  
Li-Gong Mishulan
Keyword(s):  
Standard Model ◽  
Observational Data ◽  
Mass Distribution ◽  
Particle Physics ◽  
Physical Mechanism ◽  
Careful Analysis ◽  
Geometric Progression ◽  
Neutrino Masses ◽  
Three Generations ◽  
The Standard Model

Abstract The Standard Model of particle physics contains three generations of elementary fermions, which have prominent mass hierarchies. Through careful analysis of the observational data on the mass of elementary fermions, we determine that an intrinsic pattern does exist. A geometric progression is proposed to describe the mass distribution of elementary fermions, and using the observational data of neutrino oscillations, we can estimate the neutrino masses for all three generations. At the same time, we propose a hypothesis about the mass distribution of elementary fermions and explore the quantum physical mechanism of the origin of the elementary fermions masses hierarchies.

scholarly journals Neutron star masses

2012 ◽  
Vol 8 (S291) ◽  
pp. 146-146
Author(s):  
David Nice
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Observational Data ◽  
Mass Distribution ◽  
Binary Star ◽  
Star Mass ◽  
Star Evolution ◽  
Neutron Star Mass ◽  
Present Understanding

AbstractNeutron star masses can be inferred from observations of binary pulsar systems, particularly by the measurement of relativistic phenomena within these orbits. The observed distribution of masses can be used to infer or constrain the equation of state for nuclear matter and to study astrophysical processes such as supernovae and binary star evolution. In this talk, I will review our present understanding of the neutron star mass distribution with an emphasis on the observational data.

On approach to determine the internal potential and gravitational energy of ellipsoid

2021 ◽  
Vol 8 (3) ◽  
pp. 359-367
Author(s):  
М. M. Fys ◽  
◽  
А. M. Brydun ◽  
М. I. Yurkiv ◽  
◽  
...  
Keyword(s):  
Distribution Function ◽  
Mass Distribution ◽  
Special Form ◽  
Iterative Process ◽  
Three Dimensional ◽  
Gravitational Energy ◽  
One Dimensional ◽  
Piecewise Continuous ◽  
The Masses ◽  
Internal Potential

Formulas are derived for the calculation of the potential of bodies, which surface is a sphere or an ellipsoid, and the distribution function has a special form: a piecewise continuous one-dimensional function and a three-dimensional mass distribution. For each of these cases, formulas to calculate both external and internal potentials are derived. With their help, further the expressions are given for calculation of the potential (gravitational) energy of the masses of such bodies and their corresponding distributions. For spherical bodies, the exact and approximate relations for determining the energy are provided, which makes it possible to compare the iterative process and the possibility of its application to an ellipsoid. The described technique has been tested by a specific numerical example.

scholarly journals Weak lensing constraints on the dark matter haloes of early type galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 71-73
Author(s):  
Priyamvada Natarajan
Keyword(s):  
Dark Matter ◽  
Mass Distribution ◽  
Current Work ◽  
Weak Lensing ◽  
Early Type ◽  
Host Galaxies ◽  
The Masses

AbstractConstraints on the masses of dark matter haloes associated with galaxies in the field and in clusters have been successfully obtained used galaxy-galaxy lensing techniques. Weak lensing thus provides important information on the mass distribution in galaxies at large radii in a statistical fashion. Current work suggests that all galaxies possess extended dark matter haloes, however those that host galaxies in clusters are less extended and less massive.

scholarly journals Do Nuclear Star Clusters and Supermassive Black Holes Follow the Same Host-Galaxy Correlations?

2012 ◽  
Vol 2012 ◽  
pp. 1-11 ◽  
Author(s):  
Peter Erwin ◽  
Dimitri Alexei Gadotti
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Careful Analysis ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Host Galaxy ◽  
Mass Ratio ◽  
Host Galaxies ◽  
Order Of Magnitude ◽  
The Masses

Studies have suggested that there is a strong correlation between the masses of nuclear star clusters (NSCs) and their host galaxies, a correlation which is said to be an extension of the well-known correlations between supermassive black holes (SMBHs) and their host galaxies. But careful analysis of disk galaxies—including 2D bulge/disk/bar decompositions—shows that while SMBHs correlate with the stellar mass of thebulgecomponent of galaxies, the masses of NSCs correlate much better with thetotalgalaxy stellar mass. In addition, the mass ratioMNSC/M⋆, totfor NSCs in spirals (at least those with Hubble types Sc and later) is typically an order of magnitude smaller than the mass ratioMBH/M⋆, bulof SMBHs. The absence of a universal “central massive object” correlation argues against common formation and growth mechanisms for both SMBHs and NSCs. We also discuss evidence for a break in the NSC-host galaxy correlation, galaxies with Hubble types earlier than Sbc appear to host systematically more massive NSCs than do types Sc and later.

scholarly journals Dynamical Reference Frame — Current Relevance and Future Prospects

2000 ◽  
Vol 180 ◽  
pp. 120-126 ◽  
Author(s):  
E.M. Standish
Keyword(s):  
Observational Data ◽  
Reference Frame ◽  
Future Prospects ◽  
Data Types ◽  
Inertial Space ◽  
Lunar Laser ◽  
The Masses ◽  
Fundamental Reference

AbstractPlanetary and lunar ephemerides are no longer used for the determination of inertial space. Instead, the new fundamental reference frame, the ICRF, is inherently less susceptible to extraneous, non-inertial rotations than would be a dynamical reference frame determined by the ephemerides. Consequently, the ephemerides are now adjusted onto the ICRF, and they are fit to two modern, accurate observational data types: ranging (radar, lunar laser, spacecraft) and VLBI (of spacecraft near planets).The uncertainties remaining in the inner planet ephemerides are on the order of 1 kilometer, both in relative positions between the bodies and in the orientation of the inner system as a whole. The predictive capabilities of the inner planet ephemerides are limited by the uncertainties in the masses of many asteroids. For this reason, future improvements to the ephemerides must await determinations of many asteroid masses. Until then, it will be necessary to constantly update the ephemerides with a continuous supply of observational data.

The masses of 18 pairs of double neutron stars and implications for their origin

2018 ◽  
Vol 14 (S346) ◽  
pp. 474-477
Author(s):  
ChengMin Zhang ◽  
YiYan Yang
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Mass Distribution ◽  
Binary Stars ◽  
Formation Process ◽  
Initial Conditions ◽  
Mean Value ◽  
Solar Mass ◽  
The Mean ◽  
The Masses

AbstractFor the observed 18 pairs of double neutron star (DNS) systems, we find that DNS mass distribution is very narrow and its mean value (about 1.34 solar mass) is less than the mean of all measured pulsars of about 1.4 solar mass. To interpret the special DNS mass characteristics, we analyze the DNS formation process, via the phases of HMXBs, by investigating the evolution of massive binary stars. Moreover, in DNSs, two classes of NSs are taken into account, formed by supernova (SN) and electron capture (EC), respectively, and generally the NS mass by SN is bigger than that by EC. Quantitatively, with various initial conditions of binary stars, the observed special DNS distribution can be satisfactorily explained.

Fragmentation and Distribution of Asteroids

1971 ◽  
Vol 12 ◽  
pp. 263-295 ◽  
Author(s):  
Julius S. Dohnanyi
Keyword(s):  
Mass Distribution ◽  
Initial Distribution ◽  
Target Object ◽  
Inelastic Collisions ◽  
Steady State Distribution ◽  
State Distribution ◽  
Geologic Time ◽  
Constant Change ◽  
Geologic Time Scale ◽  
The Masses

As a result of mutual inelastic collisions, frequent on a geologic time scale, the mass distribution of asteroids undergoes constant change. Using a simplified velocity distribution for asteroids, the redistribution of their masses caused by collisions can be mathematically modeled as a stochastic process and the distribution of asteroidal masses can then be obtained as the solution. This paper is a review of recent progress on this problem.The most detailed discussion of this problem considers the influence of the following collisional processes on the asteroidal mass distribution: (1) loss of asteroids by catastrophic breakup, (2) creation of new objects from the fragments of a catastrophically disrupted one, (3) erosive reduction in the masses of individual asteroids, and (4) erosive creation of new objects (i.e., production of secondary ejecta during erosive cratering by projectiles not large enough to catastrophically disrupt the target object). The main result is that after a sufficiently long period of time the population of asteroids may reach a quasi-steady-state distribution, regardless of the initial distribution. This final distribution is a product of a slowly decreasing function of time by a power law of index 11/6 for masses smaller than the largest asteroids. For the largest asteroids, an additional factor is included that expresses the influence on the distribution of the absence of masses larger than those observed. The observed distribution of bright asteroids from the McDonald asteroidal survey and that of faint ones from the Palomar-Leiden asteroidal survey are each individually consistent with the theoretical distribution, although they differ from each other by a numerical factor.

scholarly journals SUPPRESSION OF 0ν2β DECAY FROM CP VIOLATION

2007 ◽  
Vol 16 (02) ◽  
pp. 561-565
Author(s):  
MAREK GÓŹDŹ ◽  
WIESŁAW A. KAMIŃSKI
Keyword(s):  
Cp Violation ◽  
Beta Decay ◽  
Half Life ◽  
Neutrino Oscillations ◽  
Mass Matrix ◽  
Neutrinoless Double Beta Decay ◽  
Double Beta Decay ◽  
Weak Basis ◽  
The Masses ◽  
Mass Basis

The observed phenomenon of neutrino oscillations is interpreted as the proof that neutrinos must have mass. As this is true for the neutrinos in the mass basis, the mass matrix in the flavor (weak) basis may still contain zeros. This can happen if the CP violating phases, usually neglected, come into play and result in suppression of processes which half-life depends on the masses of νe, νμ, or ντ. In the present paper we investigate the possibility of such suppression of the neutrinoless double beta decay (0ν2β).

scholarly journals Mass distributions of meteorites

2020 ◽  
Vol 493 (3) ◽  
pp. 4058-4064
Author(s):  
Alberto S Betzler ◽  
Ernesto P Borges
Keyword(s):  
Statistical Mechanics ◽  
Observational Data ◽  
Mass Distribution ◽  
Exponential Function ◽  
Fragmentation Process ◽  
Statistical Distributions ◽  
Mass Distributions ◽  
Gibbs Entropy ◽  
Collection Sites

ABSTRACT For at least five decades, the study of the mass distribution of meteorites has been carried out. This study aims to obtain the flux of material that comes to the Earth’s surface. For this, the observational data were modelled statistical distributions of the most varied types, derived from Gibbs entropy. However, it appears that the fragmentation process is probably complex in nature. Given this particularity, we model the mass distribution of meteorites using the q-exponential function, derived from Tsallis non-extensive statistical mechanics. This distribution is capable of modelling the entire observed spectrum of meteorite mass regardless of whether the specimens originate from the fragmentation of a single meteorite, belong to the same mineralogical group or type, or when are separated by collection sites on the Earth’s surface. We suggest that most meteorite samples are incomplete in certain mass ranges due to the action of the so-called gathering bias.

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