2016
DOI: 10.1103/physrevlett.116.161804
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Axion Dark Matter Coupling to Resonant Photons via Magnetic Field

Abstract: We show that the magnetic component of the photon field produced by dark matter axions via the two-photon coupling mechanism in a Sikivie Haloscope is an important parameter passed over in previous analysis and experiments. The interaction of the produced photons will be resonantly enhanced as long as they couple to the electric or magnetic mode structure of the Haloscope cavity. For typical Haloscope experiments the electric and magnetic coupling is the same and implicitly assumed in past sensitivity calculat… Show more

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Cited by 30 publications
(17 citation statements)
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“…Here B is the field strength of the external magnetic field, C is a mode dependent form factor of order 1 [29], which represents the degree of overlap between the cavity mode electromagnetic field and the electromagnetic field induced due to axion photon conversion (it is an integral of the dot product of these two fields), V is the volume of the detecting cavity, Q L is the loaded cavity quality factor (provided it is lower than the expected axion signal quality factor ∼ 10 6 ), and ρ a is the local axion dark matter density. The signal powers in axion haloscopes are extremely weak, even ADMX, which operates with a very large volume and high magnetic field system expects signal powers on the order of 10 −22 W. The challenges faced in the move to high frequency haloscopes are evident in equation 1.…”
Section: Haloscopesmentioning
confidence: 99%
“…Here B is the field strength of the external magnetic field, C is a mode dependent form factor of order 1 [29], which represents the degree of overlap between the cavity mode electromagnetic field and the electromagnetic field induced due to axion photon conversion (it is an integral of the dot product of these two fields), V is the volume of the detecting cavity, Q L is the loaded cavity quality factor (provided it is lower than the expected axion signal quality factor ∼ 10 6 ), and ρ a is the local axion dark matter density. The signal powers in axion haloscopes are extremely weak, even ADMX, which operates with a very large volume and high magnetic field system expects signal powers on the order of 10 −22 W. The challenges faced in the move to high frequency haloscopes are evident in equation 1.…”
Section: Haloscopesmentioning
confidence: 99%
“…However, because of the axion anomaly, this set of Maxwell's equations doesn't naturally satisfy certain boundary conditions. The general haloscope conditions that have been assumed in many previous approaches are [15,16] • zero current : J e = 0,…”
Section: Separation Of Maxwell's Equations For Haloscope Searchesmentioning
confidence: 99%
“…In Refs. [15,16], this problem was avoided by forcing the non-zero term in Eq.6 as a relationship of new fields E a and B a as…”
Section: Separation Of Maxwell's Equations For Haloscope Searchesmentioning
confidence: 99%
“…This anomalous current points along magnetic field in contrast with ordinary E&M , where the current is always orthogonal to B. Most of the recent proposals [14][15][16][17][18][19][20][21][22][23][24][25][26] to detect the dark matter axions are precisely based on this extra current (5).…”
Section: Axion θ Field and Variety Of Topological Phenomenamentioning
confidence: 93%
“…Still, it remains one of the most interesting resolutions of the strong CP problem to date, which has also led to numerous proposals for direct dark matter searches. Here we list but a fraction of the new (and old) ideas [14][15][16][17][18][19][20][21][22][23][24][25][26] On the other hand, one may also discuss a similar theta term in QED. It is normally assumed that a similar θ QED parameter in the abelian Maxwell Electrodynamics is unphysical (if magnetic monopoles are absent), and can be always removed from the system.…”
Section: Introductionmentioning
confidence: 99%