Constraining Neutrino Cooling Using the Hot White Dwarf Luminosity Function in the Globular Cluster 47 Tucanae

Hansen, Brad M. S.; Richer, Harvey B.; Kalirai, Jason; Goldsbury, Ryan; Frewen, Shane

doi:10.1088/0004-637x/809/2/141

Cited by 42 publications

(48 citation statements)

References 62 publications

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“…Our analysis strongly rules out that value, but we also find better fitting hydrogen layers at the thick end of the range usually considered by modelers . The 95% confidence range on f s in Hansen et al (2015, which is equivalent to our parameter n A ) was found to be < < f 0.6 1.7 s , which agrees with what we have found. The differences in these values can be attributed both to the inclusion of additional data in our analysis, and to different statistical assumptions made in fitting the models.…”

Section: Discussionsupporting

confidence: 91%

“…This data set is described in detail in Section 2. The analysis discussed in this paper complements the work in Hansen et al (2015). In that paper, similar white dwarf cooling models were fit to the ACS data shown as the surrounding annulus in Figure 1.…”

Section: Introductionmentioning

confidence: 65%

“…In Hansen et al (2015), the best-fitting hydrogen layer thickness was found to be =´-q 4 10 H 4 . Our analysis strongly rules out that value, but we also find better fitting hydrogen layers at the thick end of the range usually considered by modelers .…”

Section: Discussionmentioning

confidence: 99%

“…We would expect to draw data from our best-fitting model that differs at least as much as the real data do from that model 4.9% of the time. Hansen et al (2015) 0.025 Lawlor & MacDonald (2006) 0.078 Renedo et al (2010) 0.118 This work (MESA) 0.049…”

Section: Discussionmentioning

confidence: 99%

“…These models come from Fontaine et al (2001), Hansen et al (2015), Lawlor & MacDonald (2006), and Renedo et al (2010). The model from Hansen et al (2015) is more recent than the version fit in Goldsbury et al (2012), while the other models are the same. These models do not have any intrinsic parameters to be varied, and so the fits are only performed over the parameter space (with priors) defined by the four parameters in Table 2.…”

Section: Cooling Models From Other Groupsmentioning

confidence: 99%

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Constraining White Dwarf Structure and Neutrino Physics in 47 Tucanae

Goldsbury

Richer

Kalirai

et al. 2016

ApJ

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We present a robust statistical analysis of the white dwarf cooling sequence in 47 Tucanae. We combine Hubble Space Telescope UV and optical data in the core of the cluster, Modules for Experiments in Stellar Evolution (MESA) white dwarf cooling models, white dwarf atmosphere models, artificial star tests, and a Markov Chain Monte Carlo sampling method to fit white dwarf cooling models to our data directly. We use a technique known as the unbinned maximum likelihood to fit these models to our data without binning. We use these data to constrain neutrino production and the thickness of the hydrogen layer in these white dwarfs. The data prefer thicker hydrogen layers =´-q 3. 2 10 H 5 ( ) and we can strongly rule out thin layers = -q 10 H 6 ( ). The neutrino rates currently in the models are consistent with the data. This analysis does not provide a constraint on the number of neutrino species.

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Section: Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 65%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Cooling Models From Other Groupsmentioning

confidence: 99%

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Constraining White Dwarf Structure and Neutrino Physics in 47 Tucanae

Goldsbury

Richer

Kalirai

et al. 2016

ApJ

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New Target for Cosmic Axion Searches

Wallisch

2019

Cosmological Probes of Light Relics

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Future cosmic microwave background experiments have the potential to probe the density of relativistic species at the subpercent level. This sensitivity allows light thermal relics to be detected up to arbitrarily high decoupling temperatures. Conversely, the absence of a detection would require extra light species never to have been in equilibrium with the Standard Model. In this Letter, we exploit this feature to demonstrate the sensitivity of future cosmological observations to the couplings of axions to photons, gluons, and charged fermions. In many cases, the constraints achievable from cosmology will surpass existing bounds from laboratory experiments and astrophysical observations by orders of magnitude.

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How to rule out (g − 2)μ in $$ \textrm{U}{(1)}_{L_{\mu }-{L}_{\tau }} $$ with white dwarf cooling

Foldenauer,

Zink

2024

J. High Energ. Phys.

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In recent years, the gauge group $$ \textrm{U}{(1)}_{L_{\mu }-{L}_{\tau }} $$ U 1 L μ − L τ has received a lot of attention since it can, in principle, account for the observed excess in the anomalous muon magnetic moment (g − 2)μ, as well as the Hubble tension. Due to unavoidable, loop-induced kinetic mixing with the SM photon and Z, the $$ \textrm{U}{(1)}_{L_{\mu }-{L}_{\tau }} $$ U 1 L μ − L τ gauge boson A′ can contribute to stellar cooling via decays into neutrinos. In this work, we perform for the first time an ab initio computation of the neutrino emissivities of white dwarf stars due to plasmon decay in a model of gauged $$ \textrm{U}{(1)}_{L_{\mu }-{L}_{\tau }} $$ U 1 L μ − L τ . A key result is that current observations of the early-stage white dwarf neutrino luminosity at the 30% level exclude previously allowed regions of the parameter space favoured by a simultaneous explanation of the (g – 2)μ and H0 anomalies. In this work, we present the relevant white dwarf cooling limits over the entire A′ mass range. In particular, we have performed a rigorous computation of the luminosities in the resonant regime, where the A′ mass is comparable to the white dwarf plasma frequencies.

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Constraining Neutrino Cooling Using the Hot White Dwarf Luminosity Function in the Globular Cluster 47 Tucanae

Cited by 42 publications

References 62 publications

Constraining White Dwarf Structure and Neutrino Physics in 47 Tucanae

Constraining White Dwarf Structure and Neutrino Physics in 47 Tucanae

New Target for Cosmic Axion Searches

How to rule out (g − 2)μ in $$ \textrm{U}{(1)}_{L_{\mu }-{L}_{\tau }} $$ with white dwarf cooling

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