The Impact of Neutrino Magnetic Moments on the Evolution of Massive Stars

Heger, Alexander; Friedland, Alexander; Giannotti, Maurizio; Cirigliano, Vincenzo

doi:10.1088/0004-637x/696/1/608

Cited by 52 publications

(48 citation statements)

References 67 publications

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“…Sufficiently large axion-photon coupling is shown to eliminate the blue loop stage of the evolution, leaving one without an explanation for the existence of Cepheid stars in a broad range of pulsation periods. This is the second time massive stars are used to constrain particle physics beyond the Standard Model and, as in the case of neutrino magnetic moment [48], axion is also capable of qualitatively changing the stellar evolution. The same astrophysical argument could be used for constraining other types of new physics, e.g., millicharge particles, as will be explored elsewhere.…”

Section: Discussionmentioning

confidence: 99%

“…The effect of the axion is pronounced at moderate temperatures and densities, ordinarily the domain of photoproduction (γe − → e − νν); for higher temperatures, it is overtaken by the SM pair production (e + e − → νν), while for higher densities, the SM plasmon decay dominates (cf. [47,48]). If the axion is to have an impact on the evolution of a star, it needs to be in this region.…”

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confidence: 99%

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Constraining the Axion-Photon Coupling with Massive Stars

2013

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We point out that stars in the mass window ∼ 8−12M can serve as sensitive probes of the axionphoton interaction, gAγγ. Specifically, for these stars axion energy losses from the helium-burning core would shorten and eventually eliminate the blue loop phase of the evolution. This would contradict observational data, since the blue loops are required, e.g., to account for the existence of Cepheid stars. Using the MESA stellar evolution code, modified to include the extra cooling, we conservatively find gAγγ 0.8 × 10 −10 GeV −1 , which compares favorably with the existing bounds.

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Section: Discussionmentioning

confidence: 99%

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confidence: 99%

Constraining the Axion-Photon Coupling with Massive Stars

2013

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“…(Duez, Mathis & Turck-Chièze, 2010) Therefore, a clear signature of magnetic interaction seems difficult to achieve. Nevertheless, more and more works are dedicated to this kind of interaction for the Sun with the hope of detection of a signal in BOREXINO (Das, Pulido & Picariello, 2009), and with important consequences for more massive stars (Heger et al, 2009). …”

Section: Secondary Effects Of the Neutrino Propertiesmentioning

confidence: 99%

Solar neutrinos, helioseismology and the solar internal dynamics

Turck‐Chièze¹,

Couvidat²

2011

Rep. Prog. Phys.

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Abstract. Neutrinos are fundamental particles ubiquitous in the Universe and whose properties remain elusive despite more than 50 years of intense research activity. This review illustrates the importance of solar neutrinos in Astrophysics, Nuclear Physics, and Particle Physics. After a description of the historical context, we remind the reader of the noticeable properties of these particles and of the stakes of the solar neutrino puzzle. The Standard Solar Model triggered persistent efforts in fundamental Physics to predict the solar neutrino fluxes, and its constantly evolving predictions have been regularly compared to the detected neutrino signals. Anticipating that this standard model could not reproduce the internal solar dynamics, a Seismic Solar Model was developed which enriched theoretical neutrino flux predictions with in situ observation of acoustic and gravity waves propagating in the Sun. This seismic model contributed to the stabilization of the neutrino flux predictions. This review reminds the main historical steps, from the pioneering Homestake mine experiment and the GALLEX-SAGE experiments capturing the first pp neutrinos. It emphasizes the importance of the Superkamiokande and SNO detectors. Both experiments demonstrated that the solar-emitted electronic neutrinos are partially transformed into other neutrino flavors before reaching the Earth. This sustained experimental effort opens the door to Neutrino Astronomy, with long-base lines and underground detectors. The success of BOREXINO in detecting the 7 Be neutrino signal alone instills confidence in the physicists ability to detect each neutrino source separately. It justifies the building of a new generation of detectors to measure the entire solar neutrino spectrum with greater detail, as well as supernova neutrinos. A coherent picture emerged from neutrino physics and helioseismology. Today, new paradigms take shape in these two fields: the neutrinos are massive particles, but their masses are still unknown, and the research on the solar interior is focusing on the dynamical aspects and on signature of dark matter. The magnetic moment of the neutrino begins to be an actor of stellar evolution. The third part of the review is dedicated to this prospect. The understanding of the crucial role of both rotation and magnetism in solar physics benefit from SoHO, SDO, and PICARD space observations, and from new prototype like GOLF-NG. The magnetohydrodynamical view of the solar interior is a new way of understanding the impact of the Sun on the Earth environment and climate. For now, the particle and stellar challenges seem decoupled, but this is only a superficial appearance. The development of asteroseismology -with the COROT and KEPLER spacecrafts-and of neutrino physics will both contribute to improvements in our understanding of, for instance, supernova explosions. This shows the far-reaching impact of Neutrino and Stellar Astronomy.

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“…This will lead to significant observable consequences for the stellar evolution theory (see Raffelt 1996Raffelt , 2000Raffelt , 2012, for very detailed reviews and Heger et al 2009, for a discussion of the impact on massive stars). Raffelt (1990) and then Raffelt & Weiss (1992) showed that the properties of red giants from the color-magnitude diagram (CMD) of Galactic globular clusters implied μ ν < ∼ 3 × 10 −12 μ B , where μ B = e /(2m e c) is the Bohr magneton.…”

Section: Introductionmentioning

confidence: 99%

Limits on the neutrino magnetic dipole moment from the luminosity function of hot white dwarfs

Bertolami

Miguel²

2014

A&A

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Context. Recent determinations of the white dwarf luminosity function (WDLF) from very large surveys have extended our knowledge of the WDLF to very high luminosities. This, together with the availability of new full evolutionary white dwarf models that are reliable at high luminosities, have opened the possibility of testing particle emission in the core of very hot white dwarfs, where neutrino processes are dominant. Aims. We use the available WDLFs from the Sloan Digital Sky Survey and the SuperCOSMOS Sky Survey to constrain the value of the neutrino magnetic dipole moment (μ ν ). Methods. We used a state-of-the-art stellar evolution code to compute a grid of white dwarf cooling sequences under the assumptions of different values of μ ν . Then we constructed theoretical WDLFs for different values of μ ν and performed a χ 2 -test to derive constraints on the value of μ ν . Results. We find that the WDLFs derived from the Sloan Digital Sky Survey and the SuperCOSMOS Sky Survey do not yield consistent results. The discrepancy between the two WDLFs suggests that the uncertainties are significantly underestimated. Consequently, we constructed a unified WDLF by averaging the SDSS and SSS and estimated the uncertainties by taking into account the differences between the WDLF at each magnitude bin. Then we compared all WDLFs with theoretical WDLFs. Comparison between theoretical WDLFs and both the SDSS and the averaged WDLF indicates that μ ν should be μ ν < 5 × 10 −12 e /(2m e c). In particular, a χ 2 -test on the averaged WDLF suggests that observations of the disk WDLF exclude values of μ ν > 5 × 10 −12 e /(2m e c) at more than a 95% confidence level, even when conservative estimates of the uncertainties are adopted. This is close to the best available constraints on μ ν from the physics of globular clusters. Conclusions. Our study shows that modern WDLFs, which extend to the high-luminosity regime, are an excellent tool for constraining the emission of particles in the core of hot white dwarfs. However, discrepancies between different WDLFs suggest there might be some relevant unaccounted systematic errors. A larger set of completely independent WDLFs, as well as more detailed studies of the theoretical WDLFs and their own uncertainties, is desirable to explore the systematic uncertainties behind this constraint. Once this is done, we believe the Galactic disk WDLF will offer constraints on the magnetic dipole moment of the neutrino similar to the best available constraints obtainable from globular clusters.

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The Impact of Neutrino Magnetic Moments on the Evolution of Massive Stars

Cited by 52 publications

References 67 publications

Constraining the Axion-Photon Coupling with Massive Stars

Constraining the Axion-Photon Coupling with Massive Stars

Solar neutrinos, helioseismology and the solar internal dynamics

Limits on the neutrino magnetic dipole moment from the luminosity function of hot white dwarfs

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