Effects of axions on Population III stars

Choplin, Arthur; Coc, A.; Meynet, Georges; Olive, Keith A.; Uzan, Jean‐Philippe; Vangioni, Elisabeth

doi:10.1051/0004-6361/201731040

Cited by 14 publications

(9 citation statements)

References 54 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…An interesting question is what impacts they might have on small-scale structures, such as stars and supernovae. DM admixed in star provide extra gravity to alter the stellar structure (Brito et al 2015) and additional heating/cooling to alter its surface luminosity and lifespan (Bramante 2015;Choplin et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Accretion-induced Collapse of Dark Matter Admixed White Dwarfs. II. Rotation and Gravitational-wave Signals

Zha¹,

Chu²,

Leung

et al. 2019

ApJ

View full text Add to dashboard Cite

We present axisymmetric hydrodynamical simulations of accretion-induced collapse (AIC) of dark matter (DM) admixed rotating white dwarfs (WD) and their burst gravitational-wave (GW) signals. For initial WD models with the same central baryon density, the admixed DM is found to delay the plunge and bounce phases of AIC, and decrease the central density and mass of the proto-neutron star (PNS) produced. The bounce time, central density and PNS mass generally depend on two parameters, the admixed DM mass M DM and the ratio between the rotational kinetic and gravitational energies of the inner core at bounce β ic,b . The emitted GWs have generic waveform shapes and the variation of their amplitudes h + show a degeneracy on β ic,b and M DM . We found that the ratios between the GW amplitude peaks around bounce allow breaking the degeneracy and extraction of both β ic,b and M DM . Even within the uncertainties of nuclear matter equation of state, a DM core can be inferred if its mass is greater than 0.03 M ⊙ . We also discuss possible DM effects on the GW signals emitted by PNS g-mode oscillations. GW may boost the possibility for the detection of AIC, as well as open a new window in the indirect detection of DM.

show abstract

Section: Introductionmentioning

confidence: 99%

Accretion-induced Collapse of Dark Matter Admixed White Dwarfs. II. Rotation and Gravitational-wave Signals

Zha¹,

Chu²,

Leung

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…Despite the relatively compressed range of values of g 10 that we simulate, we do find that a photophilic axion with a coupling g 10 = 5, in modest tension with solar data [40], will change the BHMG at a level exceeding the known uncertainties and scatter. We also take this opportunity to remark that the effects of photophilic axions on population-III stars have been studied by [23] (without the inclusion of pul-sations) using the Geneva code [43]. Interestingly, [23] find a novel feature for g 10 ≥ 1, where trajectories in the T c -ρ c plane curve to higher densities at fixed T c , indicating increased core contraction.…”

Section: Fig 2 Topmentioning

confidence: 99%

“…We also take this opportunity to remark that the effects of photophilic axions on population-III stars have been studied by [23] (without the inclusion of pul-sations) using the Geneva code [43]. Interestingly, [23] find a novel feature for g 10 ≥ 1, where trajectories in the T c -ρ c plane curve to higher densities at fixed T c , indicating increased core contraction. This raises the possibility that photophilic axions may cause some stars to avoid the instability region completely, which would in its most spectacular manifestation lead to the absence of a mass gap.…”

Section: Fig 2 Topmentioning

confidence: 99%

Missing in Action: New Physics and the Black Hole Mass Gap

Croon,

McDermott,

Sakstein

2020

Preprint

View full text Add to dashboard Cite

We demonstrate the power of the black hole mass gap as a novel probe of fundamental physics. New light particles that couple to the Standard Model can act as an additional source of energy loss in the cores of population-III stars, dramatically altering their evolution. We investigate the effects of two paradigmatic weakly coupled, low-mass particles, axions and hidden photons, and find that the pulsational pair instability, which causes a substantial amount of mass loss, is suppressed. As a result, it is possible to form black holes of 72M or heavier, deep inside the black hole mass gap predicted by the Standard Model. The upper edge of the mass gap is raised to > 130M , implying that heavier black holes, anticipated to be observed after LIGO's sensitivity is upgraded, would also be impacted. In contrast, thermally produced heavy particles would remain in the core, leading to the tantalizing possibility that they drive a new instability akin to the electron-positron pair instability. We investigate this effect analytically and find that stars that avoid the electronpositron pair instability could experience this new instability. We discuss our results in light of current and upcoming gravitational wave interferometer detections of binary black hole mergers.

show abstract

“…One possible mechanism is the so-called mirror reflection principle. When a star leaves the red giant branch to the blue loop, nuclear burning energy is used to expand the core (Choplin et al 2017). Because of the mirror reflection principle, the expansion of the core leads to the contraction of the envelope and thus higher effective temperature.…”

Section: Evolution Of the Corementioning

confidence: 99%

Elimination of the Blue Loops in the Evolution of Intermediate-mass Stars by the Neutrino Magnetic Moment and Large Extra Dimensions

Mori,

Balantekin,

Kajino

et al. 2020

Preprint

View full text Add to dashboard Cite

For searching beyond Standard Model physics, stars are laboratories which complement terrestrial experiments. Massless neutrinos in the Standard Model of particle physics cannot have a magnetic moment, but massive neutrinos have a finite magnetic moment in the minimal extension of the Standard Model. Large extra dimensions are a possible solution of the hierarchy problem. Both of these provide additional energy loss channels in stellar interiors via the electromagnetic interaction and radiation into extra dimensions, respectively, and thus affect stellar evolution. We perform simulations of stellar evolution with such additional energy losses and find that they eliminate the blue loops in the evolution of intermediate-mass stars. The existence of Cepheid stars can be used to constrain the neutrino magnetic moment and large extra dimensions. In order for Cepheids to exist, the neutrino magnetic moment should be smaller than the range ∼ 2×10 −10 to 4×10 −11 µ B , where µ B is the Bohr magneton, and the fundamental scale in the (4+2)-spacetime should be larger than ∼ 2 to 5 TeV, depending on the rate of the 12 C(α, γ) 16 O reaction. The fundamental scale also has strong dependence on the metallicity. This value of the magnetic moment is in the range explored in the reactor experiments, but higher than the limit inferred from globular clusters. Similarly the fundamental scale value we constrain corresponds to a size of the compactified dimensions comparable to those explored in the torsion balance experiments, but is smaller than the limits inferred from collider experiments and low-mass stars.

show abstract

Effects of axions on Population III stars

Cited by 14 publications

References 54 publications

Accretion-induced Collapse of Dark Matter Admixed White Dwarfs. II. Rotation and Gravitational-wave Signals

Accretion-induced Collapse of Dark Matter Admixed White Dwarfs. II. Rotation and Gravitational-wave Signals

Missing in Action: New Physics and the Black Hole Mass Gap

Elimination of the Blue Loops in the Evolution of Intermediate-mass Stars by the Neutrino Magnetic Moment and Large Extra Dimensions

Contact Info

Product

Resources

About