Muonic boson limits: Supernova redux

Caputo, Andrea; Raffelt, Georg; Vitagliano, Edoardo

doi:10.1103/PhysRevD.105.035022

Muonic boson limits: Supernova redux

Andrea Caputo
(
- Tel Aviv U. and
- Weizmann Inst.
)
,
Georg Raffelt
(
- Munich, Max Planck Inst.
)
,
Edoardo Vitagliano
(
- UCLA
)

Sep 7, 2021

30 pages

Published in:

Phys.Rev.D 105 (2022) 3, 035022

Published: Feb 1, 2022

e-Print:

2109.03244 [hep-ph]

DOI:

10.1103/PhysRevD.105.035022 (publication)

Report number:

MPP-2021-154

View in:

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Abstract: (APS)

We derive supernova (SN) bounds on muon-philic bosons, taking advantage of the recent emergence of muonic SN models. Our main innovations are to consider scalars

ϕ

in addition to pseudoscalars

a

and to include systematically the generic two-photon coupling

G_{γ γ}

implied by a muon triangle loop. This interaction allows for Primakoff scattering and radiative boson decays. The globular-cluster bound

G_{γ γ} < 0.67 \times 10^{- 10} {GeV}^{- 1}

carries over to the muonic Yukawa couplings as

g_{a} < 3.1 \times 10^{- 9}

and

g_{ϕ} < 4.6 \times 10^{- 9}

for

m_{a, ϕ} ≲ 100 keV

, so SN arguments become interesting mainly for larger masses. If bosons escape freely from the SN core the main constraints originate from SN 1987A

γ

rays and the diffuse cosmic

γ

-ray background. The latter allows at most

10^{- 4}

of a typical total SN energy of

E_{SN} ≃ 3 \times 10^{53} erg

to show up as

γ

rays, for

m_{a, ϕ} ≳ 100 keV

implying

g_{a} ≲ 0.9 \times 10^{- 10}

and

g_{ϕ} ≲ 0.4 \times 10^{- 10}

. In the trapping regime the bosons emerge as quasi-thermal radiation from a region near the neutrino sphere and match

L_{ν}

for

g_{a, ϕ} ≃ 10^{- 4}

. However, the

2 γ

decay is so fast that all the energy is dumped into the surrounding progenitor-star matter, whereas at most

10^{- 2} E_{SN}

may show up in the explosion. To suppress boson emission below this level we need yet larger couplings,

g_{a} ≳ 2 \times 10^{- 3}

and

g_{ϕ} ≳ 4 \times 10^{- 3}

. Muonic scalars can explain the muon magnetic-moment anomaly for

g_{ϕ} ≃ 0.4 \times 10^{- 3}

, a value hard to reconcile with SN physics despite the uncertainty of the explosion-energy bound. For generic axionlike particles, this argument covers the “cosmological triangle” in the

G_{a γ γ} - m_{a}

parameter space.

Note:

30 pages, 12 figures; minor changes on the text and references, published version

two-photon: coupling
boson: radiative decay
magnetic moment: anomaly
muon: magnetic moment
loop integral
neutrino: sphere
coupling: Yukawa
axion-like particles
supernova
background

References(113)

Figures(14)

Seminars

[1]

Muon creation and effects in supernovae

R. Bollig

[2]

Muon Creation in Supernova Matter Facilitates Neutrino-driven Explosions

R. Bollig
(
- Garching, Max Planck Inst. and
- Munich, Tech. U.
)
,
H. -Th. Janka
(
- Garching, Max Planck Inst.
)
,
A. Lohs
(
- Darmstadt, GSI
)
,
G. Martinez-Pinedo
(
- Darmstadt, Tech. U. and
- Darmstadt, GSI
)
,
C.J. Horowitz
(
- Indiana U.
)

et al.

- Phys.Rev.Lett. 119 (2017) 24, 242702
•
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•
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[3]

Muons in Supernovae: Implications for the Axion-Muon Coupling

- Phys.Rev.Lett. 125 (2020) 5, 051104,
- Phys.Rev.Lett. 126 (2021) 18, 189901 (erratum)
•
e-Print:
- 2005.07141
•
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[3]

Muons in Supernovae: Implications for the Axion-Muon Coupling

- Phys.Rev.Lett. 125 (2020) 5, 051104,
- Phys.Rev.Lett. 126 (2021) 18, 189901 (erratum)
•
e-Print:
- 2005.07141
•
DOI:
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[3]

Muons in Supernovae: Implications for the Axion-Muon Coupling

- Phys.Rev.Lett. 125 (2020) 5, 051104,
- Phys.Rev.Lett. 126 (2021) 18, 189901 (erratum)
•
e-Print:
- 2005.07141
•
DOI:
- 10.1103/PhysRevLett.125.051104