Family-Patient Communication Questionnaire--Patient and Family Versions

Nakazato, Katsuharu; Shiozaki, Mariko; Hirai, Kei; Morita, Tatsuya; Tatara, Ryuhei; Ichihara, Kaori; Sato, Shinichi; Simizu, Megumi; Tsuneto, Satoru; Shima, Yasuo; Miyasita, Mitsunori

doi:10.1037/t69814-000

Cited by 2 publications

(4 citation statements)

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“…There are large uncertainties in these profiles, and we thus use four different profiles in order to estimate the systematic uncertainties in our resulting constraints. We choose the same profiles as in [20], and will refer to these as the "fiducial" [2], "Fischer, 11.8M " [46], "Fischer, 18M " [46], and "Nakazato, 13M " [47,48]. The profiles from [46] use the AGILE-BOLTZTRAN code [49][50][51][52][53], while the profile from [47,48] is based on a solution to a neutrino radiative hydrodynamical code before shock revival and a solution to the flux-limited diffusion equation after cooling has commenced.…”

Section: Supernova Temperature and Density Profilesmentioning

confidence: 99%

Supernova 1987A constraints on sub-GeV dark sectors, millicharged particles, the QCD axion, and an axion-like particle

Chang

Essig

McDermott

2018

J. High Energ. Phys.

464

432

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We consider the constraints from Supernova 1987A on particles with small couplings to the Standard Model. We discuss a model with a fermion coupled to a dark photon, with various mass relations in the dark sector; millicharged particles; dark-sector fermions with inelastic transitions; the hadronic QCD axion; and an axion-like particle that couples to Standard Model fermions with couplings proportional to their mass. In the fermion cases, we develop a new diagnostic for assessing when such a particle is trapped at large mixing angles. Our bounds for a fermion coupled to a dark photon constrain small couplings and masses 200 MeV, and do not decouple for low fermion masses. They exclude parameter space that is otherwise unconstrained by existing accelerator-based and direct-detection searches. In addition, our bounds are complementary to proposed laboratory searches for sub-GeV dark matter, and do not constrain several benchmark-model targets in parameter space for which the dark matter obtains the correct relic abundance from interactions with the Standard Model. For a millicharged particle, we exclude charges between 10 −9 − few ×10 −6 in units of the electron charge, also for masses 200 MeV; this excludes parameter space to higher millicharges and masses than previous bounds. For the QCD axion and an axion-like particle, we apply several updated nuclear physics calculations and include the energy dependence of the optical depth to accurately account for energy loss at large couplings. These corrections allow us to rule out a hadronic axion of mass between 0.1 and a few hundred eV, or equivalently to put a bound on the scale of Peccei-Quinn symmetry breaking between a few ×10 4 and 10 8 GeV, closing the hadronic axion window. For an axion-like particle, our bounds disfavor decay constants between a few ×10 5 GeV up to a few ×10 8 GeV, for a mass 200 MeV. In all cases, our bounds differ from previous work by more than an order of magnitude across the entire parameter space. We also provide estimated systematic errors due to the uncertainties of the progenitor.

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Section: Supernova Temperature and Density Profilesmentioning

confidence: 99%

Supernova 1987A constraints on sub-GeV dark sectors, millicharged particles, the QCD axion, and an axion-like particle

Chang

Essig

McDermott

2018

J. High Energ. Phys.

464

432

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“…2.2: the "fiducial model" described in Eq. (2.4), two obtained from the reference runs of [31], and one profile from [32,33]. We cut off each plot at R ν , which we define as the radius at which the temperature is T = 3 MeV for the profiles of Eq.…”

Section: Uncertainties Regarding the Explosion Of Sn1987amentioning

confidence: 99%

“…Our fiducial model, while convenient for analytic purposes, will inevitably mischaracterize the core collapse to some degree. To parameterize the uncertainties arising from the exact nature of the supernova explosion, we will also show bounds using numerical profiles from a variety of different sources [31][32][33]. The profile from [32,33] is the 13 solar mass progenitor at t = 1 sec post bounce and with a 100 msec shock revival time inserted by hand.…”

Section: Uncertainties Regarding the Explosion Of Sn1987amentioning

confidence: 99%

“…To parameterize the uncertainties arising from the exact nature of the supernova explosion, we will also show bounds using numerical profiles from a variety of different sources [31][32][33]. The profile from [32,33] is the 13 solar mass progenitor at t = 1 sec post bounce and with a 100 msec shock revival time inserted by hand. This work includes a solution to a neutrino radiative hydrodynamical code before shock revival and a solution to the flux-limited diffusion equation after cooling has commenced [33].…”

Section: Uncertainties Regarding the Explosion Of Sn1987amentioning

confidence: 99%

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Revisiting Supernova 1987A constraints on dark photons

Chang

Essig

McDermott

2017

J. High Energ. Phys.

291

440

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We revisit constraints on dark photons with masses below ∼ 100 MeV from the observations of Supernova 1987A. If dark photons are produced in sufficient quantity, they reduce the amount of energy emitted in the form of neutrinos, in conflict with observations. For the first time, we include the effects of finite temperature and density on the kineticmixing parameter, , in this environment. This causes the constraints on to weaken with the dark-photon mass below ∼ 15 MeV. For large-enough values of , it is well known that dark photons can be reabsorbed within the supernova. Since the rates of reabsorption processes decrease as the dark-photon energy increases, we point out that dark photons with energies above the Wien peak can escape without scattering, contributing more to energy loss than is possible assuming a blackbody spectrum. Furthermore, we estimate the systematic uncertainties on the cooling bounds by deriving constraints assuming one analytic and four different simulated temperature and density profiles of the proto-neutron star. Finally, we estimate also the systematic uncertainty on the bound by varying the distance across which dark photons must propagate from their point of production to be able to affect the star. This work clarifies the bounds from SN1987A on the dark-photon parameter space.

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Family-Patient Communication Questionnaire--Patient and Family Versions

Cited by 2 publications

References 0 publications

Supernova 1987A constraints on sub-GeV dark sectors, millicharged particles, the QCD axion, and an axion-like particle

Supernova 1987A constraints on sub-GeV dark sectors, millicharged particles, the QCD axion, and an axion-like particle

Revisiting Supernova 1987A constraints on dark photons

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