New Solar Opacities, Abundances, Helioseismology, and Neutrino Fluxes

Bahcall, John N.; Serenelli, Aldo; Basu, Sarbani

doi:10.1086/428929

Cited by 649 publications

(816 citation statements)

References 20 publications

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“…This result is in good agreement with the prediction from the BS05(OP) SSM of 5.69 × 10 6 cm −2 s −1 [46], to within the theoretical uncertainty of ±16%. It is also in good agreement with the BS05(AGS,OP) model prediction of 4.51×10 6 cm −2 s −1 ± 16% [46], which was constructed assuming a lower heavyelement abundance in the Sun's surface.…”

Section: A Unconstrained Fitsupporting

confidence: 90%

Low-energy-threshold analysis of the Phase I and Phase II data sets of the Sudbury Neutrino Observatory

Aharmim¹,

Stonehill²,

Leslie³

et al. 2010

Phys. Rev. C

235

197

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Results are reported from a joint analysis of Phase I and Phase II data from the Sudbury Neutrino Observatory. The effective electron kinetic energy threshold used is T eff = 3.5 MeV, the lowest analysis threshold yet achieved with water Cherenkov detector data. In units of 10 6 cm −2 s −1 , the total flux of active-flavor neutrinos from 8 B decay in the Sun measured using the neutral current (NC) reaction of neutrinos on deuterons, with no constraint on the 8 B neutrino energy spectrum, is found to be NC = 5.140 +0.160 −0.158 (stat) +0.132 −0.117 (syst). These uncertainties are more than a factor of 2 smaller than previously published results. Also presented are the spectra of recoil electrons from the charged current reaction of neutrinos on deuterons and the elastic scattering of electrons. A fit to the Sudbury Neutrino Observatory data in which the free parameters directly describe the total 8 B neutrino flux and the energy-dependent ν e survival probability provides a measure of the total 8

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Section: A Unconstrained Fitsupporting

confidence: 90%

Low-energy-threshold analysis of the Phase I and Phase II data sets of the Sudbury Neutrino Observatory

Aharmim¹,

Stonehill²,

Leslie³

et al. 2010

Phys. Rev. C

235

197

View full text Add to dashboard Cite

show abstract

“…(59) For the density profile in the solar vicinity we take the helioseismological model of [92] for the solar interior, the chromosphere model of [93] and the corona model of [94] for the surrounding region. We add to these density profiles a constant galactic density of ρ g = 10 −24 g cm −3 .…”

Section: Solar System To Galaxymentioning

confidence: 99%

Models off(R)cosmic acceleration that evade solar system tests

2007

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We study a class of metric-variation f (R) models that accelerates the expansion without a cosmological constant and satisfies both cosmological and solar-system tests in the small-field limit of the parameter space. Solar-system tests alone place only weak bounds on these models, since the additional scalar degree of freedom is locked to the high-curvature general-relativistic prediction across more than 25 orders of magnitude in density, out through the solar corona. This agreement requires that the galactic halo be of sufficient extent to maintain the galaxy at high curvature in the presence of the low-curvature cosmological background. If the galactic halo and local environment in f (R) models do not have substantially deeper potentials than expected in ΛCDM, then cosmological field amplitudes |fR| 10 −6 will cause the galactic interior to evolve to low curvature during the acceleration epoch. Viability of large-deviation models therefore rests on the structure and evolution of the galactic halo, requiring cosmological simulations of f (R) models, and not directly on solar-system tests. Even small deviations that conservatively satisfy both galactic and solar-system constraints can still be tested by future, percent-level measurements of the linear power spectrum, while they remain undetectable to cosmological-distance measures. Although we illustrate these effects in a specific class of models, the requirements on f (R) are phrased in a nearly model-independent manner.

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“…17 Summing over capture rates from the various elements in the Sun (the main contributions are from the CNO elements) using a standard solar model [47], we obtain (taking the couplings to protons and neutrons to be the same). We have assumed that the DM velocity distribution follows the Standard Halo Model -since, for high-mass WIMPs, only the low-velocity part of the distribution can be captured by scattering events, modifications that affect the low-velocity distribution will alter the capture rate.…”

Section: Jhep07(2015)133mentioning

confidence: 99%

Signatures of large composite Dark Matter states

Hardy

Lasenby

March-Russell

et al. 2015

J. High Energ. Phys.

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Abstract:We investigate the interactions of large composite dark matter (DM) states with the Standard Model (SM) sector. Elastic scattering with SM nuclei can be coherently enhanced by factors as large as A 2 , where A is the number of constituents in the composite state (there exist models in which DM states of very large A 10 8 may be realised). This enhancement, for a given direct detection event rate, weakens the expected signals at colliders by up to 1/A. Moreover, the spatially extended nature of the DM states leads to an additional, characteristic, form factor modifying the momentum dependence of scattering processes, altering the recoil energy spectra in direct detection experiments. In particular, energy recoil spectra with peaks and troughs are possible, and such features could be confirmed with only O(50) events, independently of the assumed halo velocity distribution. Large composite states also generically give rise to low-energy collective excitations potentially relevant to direct detection and indirect detection phenomenology. We compute the form factor for a generic class of such excitations -quantised surface modes -finding that they can lead to coherently-enhanced, but generally sub-dominant, inelastic scattering in direct detection experiments. Finally, we study the modifications to capture rates in astrophysical objects that follow from the elastic form factor, as well as the effects of inelastic interactions between DM states once captured. We argue that inelastic interactions may lead to the DM collapsing to a dense configuration at the centre of the object.

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New Solar Opacities, Abundances, Helioseismology, and Neutrino Fluxes

Cited by 649 publications

References 20 publications

Low-energy-threshold analysis of the Phase I and Phase II data sets of the Sudbury Neutrino Observatory

Low-energy-threshold analysis of the Phase I and Phase II data sets of the Sudbury Neutrino Observatory

Models off(R)cosmic acceleration that evade solar system tests

Signatures of large composite Dark Matter states

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