Axion helioscopes as solar magnetometers

O’Hare, Ciaran A. J.; Caputo, Andrea; Millar, Alexander J.; Vitagliano, Edoardo

doi:10.1103/physrevd.102.043019

Cited by 44 publications

(74 citation statements)

References 115 publications

(177 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…where κ is the Z 2 -preserving coupling between two dark scalars and a Higgs, κ S 2 h, that can be computed in terms of the Lagrangian parameters in (89).…”

Section: A Minimal Dark Scalar Modelmentioning

confidence: 99%

See 1 more Smart Citation

Feebly-interacting particles: FIPs 2020 workshop report

et al. 2021

View full text Add to dashboard Cite

With the establishment and maturation of the experimental programs searching for new physics with sizeable couplings at the LHC, there is an increasing interest in the broader particle and astrophysics community for exploring the physics of light and feebly-interacting particles as a paradigm complementary to a New Physics sector at the TeV scale and beyond. FIPs 2020 has been the first workshop fully dedicated to the physics of feebly-interacting particles and was held virtually from 31 August to 4 September 2020. The workshop has gathered together experts from collider, beam dump, fixed target experiments, as well as from astrophysics, axions/ALPs searches, current/future neutrino experiments, and dark matter direct detection communities to discuss progress in experimental searches and underlying theory models for FIPs physics, and to enhance the cross-fertilisation across different fields. FIPs 2020 has been complemented by the topical workshop “Physics Beyond Colliders meets theory”, held at CERN from 7 June to 9 June 2020. This document presents the summary of the talks presented at the workshops and the outcome of the subsequent discussions held immediately after. It aims to provide a clear picture of this blooming field and proposes a few recommendations for the next round of experimental results.

show abstract

“…where κ is the Z 2 -preserving coupling between two dark scalars and a Higgs, κ S 2 h, that can be computed in terms of the Lagrangian parameters in (89).…”

Section: A Minimal Dark Scalar Modelmentioning

confidence: 99%

“…In some cases, this process may even dominate over the Primakoff rate, although there are some uncertainties on the exact structure of the magnetic field in the solar interior. See Refs [88][89][90][91]. for recent analyses.…”

mentioning

confidence: 99%

Feebly-interacting particles: FIPs 2020 workshop report

et al. 2021

View full text Add to dashboard Cite

show abstract

“…One way to search for axion dark matter is by observing its decay into two photons [13][14][15][16][17][18][19][20][21][22][23][24]. However, compact objects have long been known to offer a useful avenue in which to probe axions and ALPs in a variety of ways [25][26][27][28][29][30][31][32][33]. Neutron stars (NSs) in particular offer an exciting opportunity for increasing the possibility to detect axion dark matter by allowing axions to resonantly convert into radio photons in their magnetospheres.…”

Section: Jhep09(2021)105mentioning

confidence: 99%

Radio line properties of axion dark matter conversion in neutron stars

Battye

Garbrecht

McDonald

et al. 2021

J. High Energ. Phys.

View full text Add to dashboard Cite

Axions are well-motivated candidates for dark matter. Recently, much interest has focused on the detection of photons produced by the resonant conversion of axion dark matter in neutron star magnetospheres. Various groups have begun to obtain radio data to search for the signal, however, more work is needed to obtain a robust theory prediction for the corresponding radio lines. In this work we derive detailed properties for the signal, obtaining both the line shape and time-dependence. The principal physical effects are from refraction in the plasma as well as from gravitation which together lead to substantial lensing which varies over the pulse period. The time-dependence from the co-rotation of the plasma with the pulsar distorts the frequencies leading to a Doppler broadened signal whose width varies in time. For our predictions, we trace curvilinear rays to the line of sight using the full set of equations from Hamiltonian optics for a dispersive medium in curved spacetime. Thus, for the first time, we describe the detailed shape of the line signal as well as its time dependence, which is more pronounced compared to earlier results. Our prediction of the features of the signal will be essential for this kind of dark matter search.

show abstract

“…A more detailed study by Guarini et al [39] found that solar large-scale magnetic fields enhance the axion emissivity by the coherent conversion of thermal photons to axions. It was also reported that, in the Sun, the plasmon-axion conversion could compete with the Primakoff production of axions [58]. Equally, Caputo et al [21] found that, depending on the strength and nature of the solar magnetic field, the plasmon-axion conversion dominates over Primakoff production for energies lower than 200 eV .…”

Section: Introductionmentioning

confidence: 98%

Axion spectra and the associated x-ray spectra of low-mass stars

Lopes

2021

Preprint

View full text Add to dashboard Cite

Axion particles are among the best candidates to explain dark matter and resolve the strong CP problem in the Standard Model. If such a particle exists, the core of stars will produce them in large amounts. For the first time, we predict the axion spectra and their associated luminosities for several low-mass stars -one and two solar masses stars in the main sequence and post-main sequence stages of evolution. Equally, we also compute the x-ray excess emission resulting from the conversion of axions back to photons in the presence of a strong magnetic field in the envelope of these stars. Hence, a given star will have a unique axion spectrum and La axion luminosity. And if such star has a strong magnetic field in its stellar envelope, it will also show a characteristic x-ray spectrum and Laγ x-ray luminosity. Such radiation will add up to the x-ray electromagnetic spectrum and LX luminosity of the star. The present study focuses on axion models with an axion-photon coupling constant, 5 10 −11 GeV −1 , a value just below the most recent upper limit of 6.6 10 −11 GeV −1 found by CAST and IAXO helioscopes. The range of axion parameters discussed here spans many axion models' parameter space, including the DFSZ and KSVZ models. We found that axions with a mass in the range 10 −7 to 10 −5 eV and an axion-photon coupling constant of 5 10 −11 GeV −1 produce an axion emission spectra with an averaged axion energy that varies from 1 to 5 KeV, and an La ranging from 10 −6 to 7 10 −3 L⊙. We also predict that Laγ varies from 5 10 −8 to 10 −5 L⊙ for stars with an averaged magnetic field of 3 10 4 G in their atmospheres. Most of these Laγ predictions are larger than the LX observed in some stars. Therefore, such preliminary results show the potential of the next generation of stellar x-ray missions to constrain several classes of axion models.

show abstract

Axion helioscopes as solar magnetometers

Cited by 44 publications

References 115 publications

Feebly-interacting particles: FIPs 2020 workshop report

Feebly-interacting particles: FIPs 2020 workshop report

Radio line properties of axion dark matter conversion in neutron stars

Axion spectra and the associated x-ray spectra of low-mass stars

Contact Info

Product

Resources

About