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Impulsive radio events in quiet solar corona and axion quark nugget dark matter

Shuailiang Ge, Md Shahriar Rahim Siddiqui, Ludovic Van Waerbeke, and Ariel Zhitnitsky
Phys. Rev. D 102, 123021 – Published 21 December 2020
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  • INTRODUCTION
  • THE AQN MODEL: THE BASICS
  • THE AQN MODEL: APPLICATION TO THE SOLAR…
  • THE AQN MODEL CONFRONTS THE RADIO…
  • THE AQN MODEL: WAIT TIME DISTRIBUTION
  • CONCLUSION AND FUTURE DEVELOPMENT
  • ACKNOWLEDGMENTS
  • APPENDICES
    • References

    Abstract

    The Murchison Widefield Array (MWA) recorded impulsive radio events in the quiet solar corona at frequencies 98, 120, 132, and 160 MHz [S. Mondal, D. Oberoi, and A. Mohan, Astrophys. J. 895, L39 (2020)]. We propose that these radio events are the direct manifestation of dark matter annihilation events within the axion quark nugget (AQN) framework. It has been argued [A. Zhitnitsky, J. Cosmol. Astropart. Phys. 10 (2017) 050; N. Raza, L. vanWaerbeke, and A. Zhitnitsky, Phys. Rev. D 98, 103527 (2018)] that the AQN-annihilation events in the quiet solar corona can be identified with the nanoflares conjectured by Parker [Astrophys. J. 264, 642 (1983)]. We further support this claim by demonstrating that observed impulsive radio events [S. Mondal, D. Oberoi, and A. Mohan, Astrophys. J. 895, L39 (2020)], including their rate of appearance, their temporal and spatial distributions, and their energetics, are matching the generic consequences of AQN annihilations in the quiet corona. We propose to test this idea by analyzing the correlated clustering of impulsive radio events in different frequency bands. These correlations are expressed in terms of the time delays between radio events in different frequency bands measured in seconds. We also make generic predictions for low (80 and 89 MHz) and high (179, 196, 217, and 240 MHz) frequency bands, that have been recorded, but not published, by Mondal et al. [Astrophys. J. 895, L392020]. We finally suggest to test our proposal by studying possible cross-correlation between MWA radio signals and Solar Orbiter recording of extreme UV photons (aka “campfires”).

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    • Received 13 September 2020
    • Accepted 27 November 2020

    DOI:https://doi.org/10.1103/PhysRevD.102.123021

    © 2020 American Physical Society

    Physics Subject Headings (PhySH)

    1. Research Areas
    AxionsDark matter
    Gravitation, Cosmology & AstrophysicsParticles & Fields

    Authors & Affiliations

    Shuailiang Ge*, Md Shahriar Rahim Siddiqui†, Ludovic Van Waerbeke‡, and Ariel Zhitnitsky§

    • Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada

    • *slge@phas.ubc.ca
    • †shahriar.naf07@gmail.com
    • ‡waerbeke@phas.ubc.ca
    • §arz@phas.ubc.ca

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    Vol. 102, Iss. 12 — 15 December 2020

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    Images

    • Figure 1
      Figure 1

      Left: the impact rate of AQNs with the size above B¯ where B¯ varies from Bmin to Bmax for different groups of AQNs. The horizontal black dashed line is the observed rate of radio events (11). Right: the result from the second-round simulation where we focus on large AQNs only. Again, the horizontal black dashed line is (11). The vertical dashed lines are the corresponding B¯ for different groups. More details about the numerical simulations that lead to these two subfigures can be found in the Appendix.

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    • Figure 2
      Figure 2

      Left: the luminosity generated by the annihilation of AQNs with the size above B¯ where B¯ varies from Bmin to Bmax for different groups of AQNs. Right: the result from the second-round simulation where we focus on large AQNs only. The vertical dashed lines correspond to the B¯ determined by (11) in Fig. 1. More details about the numerical simulations that lead to these two subfigures can be found in the Appendix.

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    • Figure 3
      Figure 3

      Suppression factor f(h) defined by Eq. (27). This factor describes the remaining portion of the nonthermal electrons at altitude h. The blue line corresponds to the initial kinetic energy ΔE≈2×102  eV which has been used in all our estimates throughout the text. For illustrative purposes we also presented the same suppression factor f(h) for other values of parameter ΔE. Suppression factor becomes essential for h≳4×104  km corresponding to low frequency emission as one can see from Fig. 4. In computing (27), we have used np(h)≈ne(h) above h0 where the profile of ne(h) is from [66] (the solar profiles needed in the numerical computations in this work are all from [66]).

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    • Figure 4
      Figure 4

      Frequency of the emission ν=ω/2π≈ωp/2π [i.e., Eq. (9)] as a function of height. Radio emission occurs at the altitudes above 104  km while the dominant portion of the AQN-annihilation events occur at lower altitudes h<2150  km as shown in Fig. 5.

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    • Figure 5
      Figure 5

      Left: mass fraction 1−ΔB/B being annihilated as a function of the altitude. This is plotted by taking the average of the mass loss profiles of the AQNs above B¯ (i.e., the AQNs that will generate radio emissions) where B¯ has been determined by (11). We see that the AQNs start to annihilate at about 2150 km. Right: luminosity per unit length as a function of the altitude where the energy is converted from the mass loss according to (6). This is plotted also by taking the average of the AQNs above B¯, then multiplied by the impact rate of these large AQNs.

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    • Figure 6
      Figure 6

      The blue points are extracted from Fig. 7 in [1] (132 MHz). Dividing the blue points by the corresponding bin width, we get the red points [i.e., the values of P(Δti) in (49)]. The red line is fitted by (50) with A=0.56  s−1, n≃1.5, λ≃0.0049  s−1.

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    • Figure 7
      Figure 7

      The red points are the same as those in Fig. 6 [i.e., the values of P(Δti) in (49)]. The solid line is fitted by the full expression of P(Δt) given by (43). The solid red line gives β=−0.9, t0=4000  s, λ0=0.5  s−1. Other choices around this group of parameters can also give similar result. For example, the solid black line corresponds to β=−0.6, t0=3000  s, λ0=0.2  s−1. In comparison, the dashed lines are the simplified P(Δt) given by (47), with the same group of parameters chosen correspondingly.

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    • Figure 8
      Figure 8

      Probability density distributions of the trajectory and impact properties for the Nimp=30457 impacting particles. The plots represent (a) the initial distance distribution of these impacting particles, (b) the impact parameter distribution, (c) the impact time distribution, and (d) the velocity distribution when they impact the Sun.

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