scholarly journals Improved treatment of dark matter capture in neutron stars III: nucleon and exotic targets

2021 ◽  
Vol 2021 (11) ◽  
pp. 056
Author(s):  
Filippo Anzuini ◽  
Nicole F. Bell ◽  
Giorgio Busoni ◽  
Theo F. Motta ◽  
Sandra Robles ◽  
...  
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Neutron Stars ◽  
Capture Rate ◽  
Form Factors ◽  
Mass Range ◽  
Strong Interactions ◽  
Dependent Form ◽  
Free Fermi ◽  
Total Capture

Abstract We consider the capture of dark matter (DM) in neutron stars via scattering on hadronic targets, including neutrons, protons and hyperons. We extend previous analyses by including momentum dependent form factors, which account for hadronic structure, and incorporating the effect of baryon strong interactions in the dense neutron star interior, rather than modelling the baryons as a free Fermi gas. The combination of these effects suppresses the DM capture rate over a wide mass range, thus increasing the cross section for which the capture rate saturates the geometric limit. In addition, variation in the capture rate associated with the choice of neutron star equation of state is reduced. For proton targets, the use of the interacting baryon approach to obtain the correct Fermi energy is essential for an accurate evaluation of the capture rate in the Pauli-blocked regime. For heavy neutron stars, which are expected to contain exotic matter, we identify cases where DM scattering on hyperons contributes significantly to the total capture rate. Despite smaller neutron star capture rates, compared to existing analyses, we find that the projected DM-nucleon scattering sensitivity greatly exceeds that of nuclear recoil experiments for a wide DM mass range.

ACCRETION OF DARK MATTER IN NEUTRON STARS

2011 ◽  
Vol 20 (supp02) ◽  
pp. 109-116
Author(s):  
MOISÉS RAZEIRA ◽  
ALEXANDRE MESQUITA ◽  
CÉSAR A. Z. VASCONCELLOS ◽  
ROSANA O. GOMES
Keyword(s):  
Dark Matter ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Capture Rate ◽  
Stellar Objects ◽  
Effective Models

In this work we study the effect of the accretion of dark matter into neutron stars. We have considered two relativistic nuclear effective models for the structure of neutron stars (ZM and Boguta-Bodmer) and three profiles for dark matter (Navarro-Frenk-White, Einasto, and Burkert). We have analyzed the effects of these effective models and profiles in the equation of state of nuclear matter and in the capture rate of dark matter by neutron stars. Our results confirm that the capture rate of dark matter by neutron stars is strongly model dependent. This leads to more questions than answers due to the uncertainties in the significance of the results, requiring therefore for its elucidation new signatures of capture of dark matter by these stellar objects.

scholarly journals Nucleon Structure and Strong Interactions in Dark Matter Capture in Neutron Stars

2021 ◽  
Vol 127 (11) ◽  
Author(s):  
Nicole F. Bell ◽  
Giorgio Busoni ◽  
Theo F. Motta ◽  
Sandra Robles ◽  
Anthony W. Thomas ◽  
...  
Keyword(s):  
Dark Matter ◽  
Neutron Stars ◽  
Strong Interactions ◽  
Nucleon Structure

scholarly journals Neutron to dark matter decay in neutron stars

2018 ◽  
Vol 33 (31) ◽  
pp. 1844020 ◽  
Author(s):  
T. F. Motta ◽  
P. A. M. Guichon ◽  
A. W. Thomas
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Neutron Stars ◽  
Decay Width ◽  
Decay Mode ◽  
Measurement Problem ◽  
Dark Matter Particle ◽  
Neutron Decay ◽  
Astrophysical Data ◽  
The Universe

Recent proposals have suggested that a previously unknown decay mode of the neutron into a dark matter particle could solve the long lasting measurement problem of the neutron decay width. We show that, if the dark particle in neutron decay is the major component of the dark matter in the universe, this proposal is in disagreement with modern astrophysical data concerning neutron star masses.

scholarly journals Double dark matter admixed neutron star

2018 ◽  
Vol 27 (16) ◽  
pp. 1950002 ◽  
Author(s):  
Zeinab Rezaei
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Equations Of State ◽  
Compact Object ◽  
Gravitational Redshift ◽  
Two Fluid

The dark matter (DM) in neutron stars can exist from the lifetime of the progenitor or when captured by this compact object. The properties of DM that enter the neutron stars through each step could be different from each other. Here, we investigate the structure of neutron stars which are influenced by the DM in two processes. Applying a generalization of two-fluid formalism to three-fluid one and the equation-of-state from the rotational curves of galaxies, we explore the structure of double DM admixed neutron stars. The behavior of the neutron and DM portions for these stars is considered. In addition, the influence of the DM equations of state on the stars with different contributions of visible and DM are studied. The gravitational redshift of these stars in different cases of DM equations of state is investigated.

scholarly journals Future directions in the microwave cavity search for dark matter axions

2014 ◽  
Vol 29 (19) ◽  
pp. 1443004 ◽  
Author(s):  
T. M. Shokair ◽  
J. Root ◽  
K. A. Van Bibber ◽  
B. Brubaker ◽  
Y. V. Gurevich ◽  
...  
Keyword(s):  
Dark Matter ◽  
Mass Range ◽  
Dark Matter Halo ◽  
Microwave Cavity ◽  
Strong Interactions ◽  
Dark Matter Candidate ◽  
Test Bed ◽  
Technological Advances ◽  
Pseudoscalar Particle ◽  
Low Mass

The axion is a light pseudoscalar particle which suppresses CP-violating effects in strong interactions and also happens to be an excellent dark matter candidate. Axions constituting the dark matter halo of our galaxy may be detected by their resonant conversion to photons in a microwave cavity permeated by a magnetic field. The current generation of the microwave cavity experiment has demonstrated sensitivity to plausible axion models, and upgrades in progress should achieve the sensitivity required for a definitive search, at least for low mass axions. However, a comprehensive strategy for scanning the entire mass range, from 1–1000 μeV, will require significant technological advances to maintain the needed sensitivity at higher frequencies. Such advances could include sub-quantum-limited amplifiers based on squeezed vacuum states, bolometers, and/or superconducting microwave cavities. The Axion Dark Matter eXperiment at High Frequencies (ADMX-HF) represents both a pathfinder for first data in the 20–100 μeV range (~5–25 GHz), and an innovation test-bed for these concepts.

scholarly journals Neutron decay, dark matter and neutron stars

2019 ◽  
Vol 219 ◽  
pp. 05006
Author(s):  
D.H. Beck
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Neutron Stars ◽  
Nucleon Nucleon ◽  
Neutron Decay ◽  
Neutron Lifetime ◽  
Nucleon Interaction ◽  
Star Mass ◽  
Neutron Star Mass ◽  
Nucleon Nucleon Interaction

Following up on a suggestion that decay to a dark matter fermion might explain the 4σ discrepancy in the neutron lifetime, we consider the implications of such a fermion on neutron star structure. We find that including it reduces the maximum neutron star mass to well below the observed masses. In order to recover stars with the observed masses, the (repulsive) self-interactions of the dark fermion would have to be stronger than those of the nucleon-nucleon interaction.

scholarly journals Neutron Stars and Dark Matter

Universe ◽  
2020 ◽  
Vol 6 (12) ◽  
pp. 222
Author(s):  
Antonino Del Popolo ◽  
Morgan Le Delliou ◽  
Maksym Deliyergiyev
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Neutron Stars ◽  
Cross Section ◽  
Galactic Center ◽  
Interaction Strength ◽  
Dark Matter Particle ◽  
Galactic Centre ◽  
Interaction Cross Section ◽  
Neutron Star Mass

Neutron stars change their structure with accumulation of dark matter. We study how their mass is influenced from the environment. Close to the sun, the dark matter accretion from the neutron star does not have any effect on it. Moving towards the galactic center, the density increase in dark matter results in increased accretion. At distances of some fraction of a parsec, the neutron star acquire enough dark matter to have its structure changed. We show that the neutron star mass decreases going towards the galactic centre, and that dark matter accumulation beyond a critical value collapses the neutron star into a black hole. Calculations cover cases varying the dark matter particle mass, self-interaction strength, and ratio between the pressure of dark matter and ordinary matter. This allow us to constrain the interaction cross section, σdm, between nucleons and dark matter particles, as well as the dark matter self-interaction cross section.

scholarly journals Review of low energy nuclear astrophysics

2021 ◽  
Vol 36 (22) ◽  
pp. 2130019
Author(s):  
Leonard S. Kisslinger ◽  
Debasish Das
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Star Formation ◽  
Neutron Star ◽  
Neutron Stars ◽  
Nuclear Energy ◽  
Massive Stars ◽  
Nuclear Astrophysics ◽  
Low Energy ◽  
The Sun

In this review of Low Energy Nuclear Astrophysics, we review the nuclear energy and evolution of the sun. Then we review the estimate of dark matter from galaxy rotation. Next, we discuss neutron star formation from the gravitational collapse of massive stars which produces neutron stars and their velocity. Then the origin of supernovae, the estimate of dark energy from supernovae acceleration, and experiments related to low energy nuclear astrophysics are reviewed.

scholarly journals The Large Range of Dark Matter content in Dwarf Galaxies and its Implications

1996 ◽  
Vol 171 ◽  
pp. 435-435
Author(s):  
S.A. Pustilnik ◽  
V.A. Lipovetsky ◽  
J.-M. Martin ◽  
T.X. Thuan
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Large Range ◽  
Dwarf Galaxy ◽  
Rotational Velocity ◽  
Matter Content ◽  
Optical Observations ◽  
Strong Interactions ◽  
Formation Mechanisms ◽  
Mass Ratio

We present the analysis of a new set of radio and optical observations of a large sample of Byurakan Blue Compact Galaxies. HI spectra were obtained with the Nançay 300-m and Green Bank 43-m radio telescopes. CCD-images were taken with the KPNO 0.9-m and Whipple Observatory 1.2-m telescopes. Dark Matter (DM) to luminous mass ratios in these BCGs were found to vary from about less than 0.5 up to 14. Recent data taken from the literature indicate this same range. This result has important consequences on models of dwarf galaxy formation, indicating possibly different formation mechanisms. The standard CDM model of dwarfs formation requires large DM halos. However the formation of dwarfs as tidal debris resulting from strong interactions of massive spirals leads naturally to dwarfs with low content of DM. On Fig.1 we show DM to luminous mass ratio versus rotational velocity for our BCGs and some other galaxies.

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