X-Ray Signatures of Axion Conversion in Magnetic White Dwarf Stars

Dessert, Christopher; Long, Andrew J.

doi:10.1103/physrevlett.123.061104

Cited by 58 publications

(57 citation statements)

References 90 publications

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“…from astrophysical observables including WDLF [68], the tip of RGB [69] and the R parameter (with two models) [64], as well as the constraints from the global fit of the solar data [70], LUX [73], and PandaX [74], with arrows denoting excluded regions. We do not show constraints from CAST [75] and magnetic WDs [71] by assuming the axion mass ≳1 eV. The shaded green region contains 1σ to 4σ contours favored by the anomalous stellar cooling [25,72].…”

Section: Fig 3 He 2d Axion Couplings Parameter Fit For the Xenon1tmentioning

confidence: 94%

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Reexamining the Solar Axion Explanation for the XENON1T Excess

et al. 2020

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The XENON1T collaboration has observed an excess in electronic recoil events below 5 keV over the known background, which could originate from beyond-the-standard-model physics. The solar axion is a well-motivated model that has been proposed to explain the excess, though it has tension with astrophysical observations. The axions traveling from the Sun can be absorbed by the electrons in the xenon atoms via the axion-electron coupling. Meanwhile, they can also scatter with the atoms through the inverse Primakoff process via the axion-photon coupling, which emits a photon and mimics the electronic recoil signals. We found that the latter process cannot be neglected. After including the keV photon produced via the inverse Primakoff process in the detection, the tension with the astrophysical constraints can be significantly reduced. We also explore scenarios involving additional new physics to further alleviate the tension with the astrophysical bounds.

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Section: Fig 3 He 2d Axion Couplings Parameter Fit For the Xenon1tmentioning

confidence: 94%

“…The global fit of the solar data constrains g aγ < 4.1 × 10 −10 GeV −1 [70]. Other constraints such as x-ray observations on magnetic WDs [71] get significantly weakened for axion mass ≳1 meV. In Fig.…”

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confidence: 90%

Reexamining the Solar Axion Explanation for the XENON1T Excess

et al. 2020

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“…In this manner, we use c aγγ = 1 and show the current limit from CAST [66] in blue shading and the future prospect of BabyIAXO and IAXO [48] by red dot-dashed curves. Similarly, a potential reach in g aee is shown for c aγγ = 1 by the magenta dot-dashed curve obtained from a future sensitivity on g aee × g aγγ using dedicated X-ray observations of the white dwarfs (WDs) [67] with XMM-Newton [68].…”

Section: Electronsmentioning

confidence: 99%

Predictions for axion couplings from ALP cogenesis

Hall

Harigaya

2021

J. High Energ. Phys.

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Adding an axion-like particle (ALP) to the Standard Model, with a field velocity in the early universe, simultaneously explains the observed baryon and dark matter densities. This requires one or more couplings between the ALP and photons, nucleons, and/or electrons that are predicted as functions of the ALP mass. These predictions arise because the ratio of dark matter to baryon densities is independent of the ALP field velocity, allowing a correlation between the ALP mass, ma, and decay constant, fa. The predicted couplings are orders of magnitude larger than those for the QCD axion and for dark matter from the conventional ALP misalignment mechanism. As a result, this scheme, ALP cogenesis, is within reach of future experimental ALP searches from the lab and stellar objects, and for dark matter.

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“…At higher photon mixings 10 −10 , Mirror Stars might look superficially like White Dwarfs, though detailed spectral analysis is still likely to uncover inconsistencies. In this case, the X-ray signal would still provide conclusive evidence of the Mirror Star's nature, providing additional motivation to study white dwarfs with X-ray observations, see also [117]. Kinetic mixing values in this range could also be constrained by mirror capture in the Sun, depending on the density of the "mirror interstellar medium".…”

Section: Discussionmentioning

confidence: 95%

Signatures of mirror stars

Curtin

Setford

2020

J. High Energ. Phys.

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Motivated by theories of Neutral Naturalness, we argue that Mirror Stars are a generic possibility in any hidden sector with analogues of Standard Model (SM) electromagnetism and nuclear physics. We show that if there exists a tiny kinetic mixing between the dark photon and the SM photon, Mirror Stars capture SM matter from the interstellar medium, which accumulates in the core of the Mirror Star and radiates in the visible spectrum. This signature is similar to, but in most cases much fainter than, ordinary white dwarfs. We also show for the first time that in the presence of captured SM matter, a fraction of dark photons from the core of the Mirror Star convert directly to SM photons, which leads to an X-ray signal that represents a direct probe of the properties of the Mirror Star core. These two signatures together are a highly distinctive, smoking gun signature of Mirror Stars. We show that Mirror Stars could be discovered in both optical and X-ray searches up to approximately 100-1000 light years away, for a range of well-motivated values of the kinetic mixing parameter.

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X-Ray Signatures of Axion Conversion in Magnetic White Dwarf Stars

Cited by 58 publications

References 90 publications

Reexamining the Solar Axion Explanation for the XENON1T Excess

Reexamining the Solar Axion Explanation for the XENON1T Excess

Predictions for axion couplings from ALP cogenesis

Signatures of mirror stars

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