scholarly journals Statistical evaporation of rotating clusters. II. Angular momentum distribution

2003 ◽  
Vol 119 (18) ◽  
pp. 9469-9475 ◽  
Author(s):  
P. Parneix ◽  
F. Calvo
Keyword(s):  
Angular Momentum ◽  
Momentum Distribution

A model for calculating the angular momentum distribution of fission fragments

1969 ◽  
Vol 136 (2) ◽  
pp. 465-480 ◽  
Author(s):  
J.O. Rasmussen ◽  
W. Nörenberg ◽  
H.J. Mang
Keyword(s):  
Angular Momentum ◽  
Momentum Distribution ◽  
Fission Fragments

scholarly journals Planetary populations according to the orbital angular momentum

2009 ◽  
Vol 5 (S265) ◽  
pp. 420-421
Author(s):  
João A. S. Amarante ◽  
Helio J. Rocha-Pinto
Keyword(s):  
Angular Momentum ◽  
Solar System ◽  
Orbital Angular Momentum ◽  
Momentum Distribution ◽  
Semimajor Axis ◽  
Terrestrial Planets ◽  
Planetary Mass ◽  
Exoplanetary Systems ◽  
Planetary Migration ◽  
Two Populations

AbstractWe investigate the angular momentum distribution of known exoplanetary systems, as a function of the planetary mass, orbital semimajor axis and metallicity of the host star. We find exoplanets seems to be classified according to at least two ‘populations’, with respect to their angular momentum properties. This classification is independent on the composition of the planet and seems to be valid for both jovian and neptunian planets, and probably can be extrapolated to the terrestrial planets of the Solar System. We analyse these ‘populations’ considering the phenomenon of planetary migration.

Angular momentum distribution in strong-field frustrated tunneling ionization

2018 ◽  
Vol 16 (4) ◽  
pp. 040202 ◽  
Author(s):  
Jintai Liang Jintai Liang ◽  
Ruozhou Zhang Ruozhou Zhang ◽  
Xiaomeng Ma Xiaomeng Ma ◽  
Yueming Zhou Yueming Zhou ◽  
Peixiang Lu Peixiang Lu
Keyword(s):  
Angular Momentum ◽  
Momentum Distribution ◽  
Strong Field ◽  
Tunneling Ionization

scholarly journals Properties of Dark Matter Halos in Disk Galaxies

2004 ◽  
Vol 220 ◽  
pp. 281-286 ◽  
Author(s):  
Roelof S. de Jong ◽  
Susan Kassin ◽  
Eric F. Bell ◽  
Stéphane Courteau
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Momentum Distribution ◽  
Surface Brightness ◽  
High Surface ◽  
Large Set ◽  
Dark Matter Halos ◽  
Rotation Curves ◽  
Galaxy Assembly ◽  
Adiabatic Contraction

We present a simple technique to estimate mass-to-light (M/L) ratios of stellar populations based on two broadband photometry measurements, i.e. a colour-M/L relation. We apply the colour-M/L relation to galaxy rotation curves, using a large set of galaxies that span a great range in Hubble type, luminosity and scale size and that have accurately measured HI and/or Hα rotation curves. Using the colour-M/L relation, we construct stellar mass models of the galaxies and derive the dark matter contribution to the rotation curves.We compare our dark matter rotation curves with adiabatically contracted Navarro, Frenk, & White (1997, NFW hereafter) dark matter halos. We find that before adiabatic contraction most high surface brightness galaxies and some low surface brightness galaxies are well fit by a NFW dark matter profile. However, after adiabatic contraction, most galaxies are poorly fit in the central few kpc. the observed angular momentum distribution in the baryonic component is poorly matched by ACDM model predictions, indicating that the angular momentum distribution is not conserved during the galaxy assembly process. We find that in most galaxies the dark matter distribution can be derived by scaling up the HI gas contribution. However, we find no consistent value for the scaling factor among all the galaxies.

scholarly journals Lithium Abundances in Solar-Type Stars

2000 ◽  
Vol 198 ◽  
pp. 495-497 ◽  
Author(s):  
L. da Silva ◽  
G. F. Porto de Mello
Keyword(s):  
Angular Momentum ◽  
Momentum Distribution ◽  
The Sun ◽  
Atmospheric Parameters ◽  
Solar Type ◽  
Subgiant Stars ◽  
High Degree ◽  
Li Content

We report Li abundances from the λ6707 line for 19 nearby dwarf and subgiant solar-type stars. The unevolved stars in this sample present high (> 2.00) Li abundances. We found a few cases of subgiant stars which present high Li content. The Sun seems to be part of a population of nearly unevolved stars which have depleted their Li to a high degree: all other metal-normal, near ZAMS stars in our sample show higher than solar Li content. There seems to be no correlation of the degree of Li depletion with mass, atmospheric parameters or state of evolution: as an example we found a star (HR1532) almost identical to the Sun in its state of evolution and atmospheric parameters, but with over ten times the solar Li abundance. We propose that different histories of angular momentum distribution at star birth, and/or post-birth angular momentum evolution, may account for these differences.

scholarly journals Angular Momentum Accretion onto Disc Galaxies

2018 ◽  
Vol 14 (A30) ◽  
pp. 228-232
Author(s):  
Filippo Fraternali ◽  
Gabriele Pezzulli
Keyword(s):  
Angular Momentum ◽  
Star Formation ◽  
Momentum Distribution ◽  
Intergalactic Medium ◽  
Star Forming ◽  
Gas Accretion ◽  
Hot Corona ◽  
Inside Out ◽  
Disc Galaxies ◽  
Hubble Time

AbstractThroughout the Hubble time, gas makes its way from the intergalactic medium into galaxies fuelling their star formation and promoting their growth. One of the key properties of the accreting gas is its angular momentum, which has profound implications for the evolution of, in particular, disc galaxies. Here, we discuss how to infer the angular momentum of the accreting gas using observations of present-day galaxy discs. We first summarize evidence for ongoing inside-out growth of star forming discs. We then focus on the chemistry of the discs and show how the observed metallicity gradients can be explained if gas accretes onto a disc rotating with a velocity 20 – 30% lower than the local circular speed. We also show that these gradients are incompatible with accretion occurring at the edge of the discs and flowing radially inward. Finally, we investigate gas accretion from a hot corona with a cosmological angular momentum distribution and describe how simple models of rotating coronae guarantee the inside-out growth of disc galaxies.

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