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X-Ray Searches for Axions from Super Star Clusters

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X-Ray Searches for Axions from Super Star Clusters PHYSICAL REVIEW LETTERS 125, 261102 (2020) X-Ray Searches for Axions from Super Star Clusters Christopher Dessert ,1,2,3 Joshua W. Foster,1,2,3 and Benjamin R. Safdi 1,2,3 1Leinweber Center for Theoretical Physics, Department of Physics, University of Michigan, Ann Arbor, Michigan 48109, USA 2Berkeley Center for Theoretical Physics, University of California, Berkeley, California 94720, USA 3Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA (Received 12 August 2020; revised 13 November 2020; accepted 23 November 2020; published 22 December 2020) Axions may be produced in abundance inside stellar cores and then convert into observable x rays in the Galactic magnetic fields. We focus on the Quintuplet and Westerlund 1 super star clusters, which host large numbers of hot, young stars including Wolf-Rayet stars; these stars produce axions efficiently through the axion-photon coupling. We use Galactic magnetic field models to calculate the expected x-ray flux locally from axions emitted from these clusters. We then combine the axion model predictions with archival Nuclear Spectroscopic Telescope Array (NuSTAR) data from 10–80 keV to search for evidence of axions. We find no significant evidence for axions and constrain the axion-photon coupling gaγγ ≲ 3.6 × −12 −1 −11 10 GeV for masses ma ≲ 5 × 10 eV at 95% confidence. DOI: 10.1103/PhysRevLett.125.261102 Ultralight axionlike particles that couple weakly to branch (HB) star lifetime, which would be modified in the ordinary matter are natural extensions to the standard presence of axion cooling [10]. model. For example, string compactifications often predict In this work, we produce some of the strongest −9 large numbers of such pseudoscalar particles that interact constraints to date on gaγγ for ma ≲ 10 eV through with the standard model predominantly through dimension- x-ray observations with the Nuclear Spectroscopic five operators [1,2]. If an axion couples to quantum Telescope Array (NuSTAR) telescope [11] of super star chromodynamics (QCD) then it may also solve the strong clusters (SSCs). The SSCs contain large numbers of CP problem [3–6]; in this work we refer to both the QCD hot, young, and massive stars, such as Wolf-Rayet (WR) axion and axionlike particles as axions. stars. We show that these stars, and as a result the SSCs, are Axions may interact electromagnetically through the highly efficient at producing axions with energies ˜ μν ∼10–100 operator L ¼ −gaγγaFμνF =4,wherea is the axion field, keV through the Primakoff process. These axions F is the electromagnetic field-strength tensor, with F˜ its may then convert into photons in the Galactic magnetic Hodge dual, and gaγγ is the dimensionful coupling constant fields, leading to signatures observable with space-based of axions to photons. This operator allows both the pro- x-ray telescopes such as NuSTAR. We analyze archival duction of axions in stellar plasmas through the Primakoff NuSTAR data from the Quintuplet SSC near the Galactic process [7,8] and the conversion of axions to photons in the Center (GC) along with the nearby Westerlund 1 (Wd1) −12 −1 presence of static external magnetic fields. Strong constraints cluster and constrain gaγγ ≲ 3.6 × 10 GeV at 95% ≲ 5 10−11 on gaγγ for low-mass axions come from the CERN Axion confidence for ma × eV. In Fig. 1 we show Solar Telescope (CAST) experiment [9], which searches for the locations of the stars within the Quintuplet cluster axions produced in the Solar plasma that free stream to Earth that are considered in this work on top of the background- and then convert to x rays in the magnetic field of the subtracted NuSTAR counts, from 10–80 keV, with the CAST detector. CAST has excluded axion couplings gaγγ ≳ point-spread function (PSF) of NuSTAR also indicated. In −11 −1 6.6 × 10 GeV for axion masses ma ≲ 0.02 eV at 95% the Supplemental Material [12] we show that observations confidence [9]. Primakoff axion production also opens a of the Arches SSC yield similar but slightly weaker limits. new pathway by which stars may cool, and strong Our work builds upon significant previous efforts to use −11 −1 imits (gaγγ ≲ 6.6 × 10 GeV at 95% confidence for stars as laboratories to search for axions. Some of the ma ≲ keV) are derived from observations of the horizontal strongest constraints on the axion-matter couplings, for example, come from examining how HB, white dwarf (WD), red giant, and neutron star (NS) cooling would be affected by an axion [10,20–28]. When the stars have large Published by the American Physical Society under the terms of magnetic fields, as is the case for WDs and NSs, the axions the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to can be converted to x rays in the stellar magnetospheres the author(s) and the published article’s title, journal citation, [29–32]. Intriguingly, in Refs. [31,32] observations of the and DOI. Funded by SCOAP3. Magnificent Seven nearby isolated NSs found evidence for 0031-9007=20=125(26)=261102(7) 261102-1 Published by the American Physical Society PHYSICAL REVIEW LETTERS 125, 261102 (2020) To compute the axion luminosity in a given star, we use the stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA) [37,38] to find, at any particular time in the stellar evolution, radial profiles of temperature, density, and composition. The simulation states are specified by an initial metallicity Z, an initial stellar mass, an initial rotation velocity, and an age. The initial metallicity is taken to be constant for all stars. In the Supplemental Material [12] we show that the Quintuplet and Arches clusters, which are both near the GC, are likely to have initial metallicities in the range Z ∈ ð0.018; 0.035Þ, consistent with the conclusions of previous works which place the initial metallicities of these clusters near solar (solar metallicity is Z ≈ 0.02) [39,40]. Note that higher metallicities generally lead to the stars entering the WR classifications sooner, when their cores are cooler. Rotation may also cause certain massive stars to be classified as WR FIG. 1. The stacked and pixelated background-subtracted count stars at younger ages. We model the initial rotation – μ data (10 80 keV) from the NuSTAR observations of the distribution as a Gaussian distribution with mean rot Quintuplet SSC. The locations of the stars are indicated in black, σ and standard deviation rot for non-negative rotation while the 90% energy containment region for emission associated μ ≈ 100 speeds [41,42]. References [41,42] found rot and with the SSC is indicated by the black circle, accounting for the σ ≈ 140 rot km=s, but to assess systematic uncertainties we NuSTAR point spread function (PSF). RA0 and DEC0 denote the vary μ between 50 and 150 km=s [41]. locations of the cluster center. We find no evidence for axion- rot induced emission from this SSC, which would follow the spatial We draw initial stellar velocities from the velocity counts template illustrated in the inset panel. distribution described above (from 0 to 500 km=s) and initial stellar masses from the Kroupa initial mass function [43] (from 15 to 200 M⊙). We use MESA to evolve the stars a hard x-ray excess consistent with the expected axion from pre-main sequence (pre-MS)—before core hydrogen spectrum from nucleon bremsstrahlung. This work extends ignition—to near supernova. At each time step we assign these efforts by allowing the axions to convert to x rays not each stellar model a spectroscopic classification using the just in the stellar magnetic fields but also in the Galactic definitions in Refs. [44,45]. We then construct an ensemble magnetic fields [33–35]. of models for each spectroscopic classification by joining Axion production in SSCs.—During helium burning, together the results of the different simulations that result particularly massive stars may undergo considerable mass in the same classification for stellar ages within the age loss, especially through either rotation or binary interaction, range for star formation in the cluster; for Quintuplet, this which can begin to peel away the hydrogen envelope, age range is between 3.0 and 3.6 Myr [46]. Note that each revealing the hot layers underneath and reversing the simulation generally provides multiple representative cooling trend. Stars undergoing this process are known models, taken at different time steps. In total we compute as WR stars, and these stars are the most important in our 105 models per stellar classification. analyses. If the star has a small (< 40% abundance) Quintuplet hosts 71 stars of masses ≳50 M⊙, with a remaining hydrogen envelope, it is classified as a WNh substantial WR cohort [46]. In particular it has 14 star; at < 5% hydrogen abundance it is classified as a WN WC þ WN stars, and we find that these stars dominate star; otherwise, it is classified as WC or WO, which the predicted axion flux. For example, at gaγγ ¼ indicates the presence of >2% carbon, and oxygen, 10−12 GeV−1 we compute that the total axion luminosity 0 035 μ 150 respectively, in the atmosphere. from the SSC (with Z ¼ . and rot ¼ km=s) is 2 1þ0.7 1035 Axions are produced through the photon coupling gaγγ in . −0.4 × erg=s, with WC þ WN stars contributing the high-mass stars in SSCs through the Primakoff process ∼70% of that flux. Note that the uncertainties arise from γ þðe−;ZÞ → a þðe−;ZÞ. This process converts a stellar performing multiple (500) draws of the stars from our photon to an axion in the screened electromagnetic field of ensembles of representative models.
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