Bulletin of the American Physical Society
APS April Meeting 2023
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session B11: Particle Astrophysics |
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Sponsoring Units: DPF Chair: Sekhar Chivukula, University of California, San Diego Room: Marquette II - 2nd Floor |
Saturday, April 15, 2023 10:45AM - 10:57AM |
B11.00001: New Constraints on Dark Matter and Cosmic Neutrino Profiles through Gravity Jason Arakawa, Yu-Dai Tsai, Marianna Safronova, Joshua Eby, Davide Farnocchia We derive purely gravitational constraints on dark matter and cosmic neutrino profiles in the solar system using asteroid (101955) Bennu. We focus on Bennu because of its extensive tracking data and high-fidelity trajectory modeling resulting from the OSIRIS-REx mission. We find that the local density of dark matter is bound by ρDM < 3.3 × 10-15 kg/m ≅ 6 × 106 ρavg,DM in the vicinity of ~ 1.1 au (where ρavg,DM ≅ 0.3 GeV/cm3). We show that high-precision tracking data of solar system objects can constrain cosmic neutrino overdensities relative to the Standard Model prediction at a level comparable to the existing bounds from KATRIN and other previous laboratory experiments. These local bounds have interesting implications for existing and future direct-detection experiments. Our constraints apply to all dark matter candidates but are particularly meaningful for scenarios including solar halos, stellar basins, and axion miniclusters, which predict overdensities in the solar system. Furthermore, Bennu can also set a constraint on ρDM if a DM-SM long-range fifth force with a strength αD times stronger than gravity exists. These constraints can be improved in the future as the accuracy of tracking data improves, observational arcs increase, and more missions visit asteroids. |
Saturday, April 15, 2023 10:57AM - 11:09AM |
B11.00002: A signal from stimulated decays of axion dark matter in the Milky Way Takuya Okawa, Bhupal Dev, Francesc Ferrer In the presence of radio waves having a wavelength equivalent to half of an axion mass, an axion undergoes a stimulated decay and emits two photons. Those two photons travel in opposite directions along the background radiation fields, and thus, the radio image and its counterimage of background fields would be enhanced. Assuming all the dark matter consists of axions, the radio signals from decays of an axion in the Milky Way stimulated by galactic, extragalactic, and CMB photons are computed. We also consider what could affect the signal: the time evolution of the flux from supernova remnants, the free-free absorption with Galactic electrons, the formation of dilute axion stars, and the mass segregation between dilute axion stars and ordinary stars. The resulting signal turns out to be bright enough to be detected by the first phase of the Square Kilometer Array for the axion-photon coupling gaγ ∼ 2-3 × 10-11 GeV-1 and an axion mass ma ∼ 10-6 eV. |
Saturday, April 15, 2023 11:09AM - 11:21AM |
B11.00003: Modelling uncertainties for neutrino propagation using nuPyProp DIKSHA GARG The interaction probability of neutrinos with matter is low, owing to their charge neutrality and their weak interactions. This means they can travel cosmological distances to reach Earth largely unhindered, pointing back to their origins. Terrestrial, sub-orbital and orbital neutrino detectors can be designed to detect signals from the extensive air showers induced by charged leptons that come from ultra-high-energy neutrinos that have propagated through the Earth. An important feature in neutrino detection is the neutrino flux sensitivity of detectors. This flux sensitivity can be estimated using the nuPyProp simulation package, which propagates neutrinos (muon-neutrino, tau-neutrino) through the Earth to produce the corresponding charged leptons (muons and tau-leptons), which provides the input to extensive air shower simulations, such that what is in nuSpaceSim. In this talk, we quantify the uncertainties in the charged lepton exit probabilities and spectra that come from weak, electromagnetic and Earth density models using nuPyProp. Some of the parameters and models that we vary are: the local water depths, tau depolarization and photo-nuclear electromagnetic energy loss. The largest uncertainty comes from the photo-nuclear electromagnetic energy loss models, with some cases seeing a 20-50% difference between models. This work highlights the usefulness of nuPyProp in quantifying the small and large uncertainties due to input models in the determination of neutrino flux sensitivities of detectors. |
Saturday, April 15, 2023 11:21AM - 11:33AM |
B11.00004: Gamma rays run on time Felipe José Llanes Estrada, Gloria Tejedor-García, Daniel Beltrán Martínez Although absorption and refraction of radiation appear together in physical phenomena, this is not the case for γ rays travelling cosmic distances, that are absorbed but not refracted by the scarce matter and radiation. |
Saturday, April 15, 2023 11:33AM - 11:45AM |
B11.00005: The Surface Array of IceCube-Gen2 Frank G Schroeder IceCube-Gen2, the next generation extension of the IceCube Neutrino Observatory at the South Pole, will feature a Surface Array on top of the enlarged Optical Array deep in the ice and also an even larger Radio Array for neutrino astronomy at the highest energies. The Surface Array will cover the footprint of the Optical Array in a similar way as IceTop covers the surface above IceCube’s current cubic-kilometer in-ice array, but being an order of magnitude larger in size and thus extending to higher energies. Detecting cosmic-ray air showers, the surface array will support neutrino astronomy by providing a veto for downgoing events and by measuring atmospheric backgrounds more accurately. Furthermore, IceCube-Gen2 will constitute a unique laboratory for the particle physics in cosmic-ray air showers because of the combination of a surface array that measures the electromagnetic shower particles and low-energy muons and a deep array that measures TeV to PeV muons produced in the same shower. In addition to the larger size, several improvements are made to the detector design compared to IceTop, e.g., the new surface detectors will be elevated to avoid snow coverage. Most importantly, a combination of scintillation detectors and radio antennas will increase the measurement accuracy for the cosmic-ray air showers detected by the surface array making IceCube-Gen2 the most accurate cosmic-ray detector for the energy range of the Galactic-to-extragalactic transition between around 100 PeV and a few EeV. Beyond the astrophysics of the most energetic Galactic cosmic rays, also important particle physics questions will be targeted, such as the cosmic-ray muon puzzle or the production of prompt leptons at PeV energies. |
Saturday, April 15, 2023 11:45AM - 11:57AM |
B11.00006: Collisional flavor instability in dense neutrino gases Huaiyu Duan, Zewei Xiong, Meng-Ru Wu, Lucas Johns Although the charged-current neutrino processes tend to destroy the flavor coherence among the weak-interaction states of a single neutrino and thus damp its flavor oscillation, they can lead for flavor instability in a dense neutrino gas such as that inside a core-collapse supernova or the black hole accretion disk formed in a compact binary merger. There exist two types of collisional flavor instability in a homogeneous and isotropic neutrino gas which can be identified by the dependence of their real frequencies on the neutrino density. The instability transitions from one type to the other and exhibits a resonance-like behavior in the region where the net electron lepton number of the neutrino gas is negligible. We show that the neutrino gas in the black hole accretion disk is susceptible to the collision-induced flavor conversion where the neutrino densities are the highest. As a result, large amounts of heavy-lepton flavor neutrinos can be produced through flavor conversion, which can have important ramifications in the subsequent evolution of the remnant. |
Saturday, April 15, 2023 11:57AM - 12:09PM |
B11.00007: NGC 1068 and Neutrino Self-Interactions Jeffrey M Hyde Recently IceCube announced the observation of high-energy neutrinos from the active galaxy NGC 1068. Due to the potential for scattering between signal neutrinos and cosmic background neutrinos, this observation is an opportunity to probe possible neutrino self-interactions mediated by a massive scalar. I will present bounds derived from this result and discuss the potential of future IceCube observations to extend them. |
Saturday, April 15, 2023 12:09PM - 12:21PM |
B11.00008: Forward production of prompt neutrinos in the atmosphere and at the LHC Yu Seon Jeong, Weidong Bai, Milind Diwan, Maria V Garzelli, Karan Kumar, Mary H Reno The atmospheric neutrino flux at very high energies is dominated by prompt neutrinos, mostly contributed by the decays of charmed hadrons produced in the forward direction by cosmic ray interactions with air nuclei. Theoretical predictions of the prompt atmospheric neutrino flux have large uncertainties mainly related with charm hadron production. Two ongoing forward experiments and the proposed Forward Physics Facility at the LHC can detect prompt neutrinos from the charm hadrons produced in the forward direction. We will present the kinematic regions relevant to the prompt atmospheric neutrino flux in terms of collider kinematic variables, the collision energy sqrt{s} and the charm hadron's center-of-mass rapidity y, and discuss implications of the forward experiments at the LHC on the theoretical predictions of the prompt atmospheric neutrino flux. |
Saturday, April 15, 2023 12:21PM - 12:33PM |
B11.00009: Reaching Critical Thresholds in Cosmology with CMB-S4 Sara M Simon The cosmic microwave background (CMB) offers an unparalleled opportunity to advance our understanding of the fundamental physics of the universe. The CMB carries information about the earliest moments in the universe that could constrain inflationary models and quantum gravity. It also acts as a backlight to the formation of structure in the universe, giving us information about dark energy, dark matter, neutrinos, and particles beyond the standard model. With ~500,000 polarization-sensitive detectors, CMB-S4 will measure the CMB with unprecedented sensitivity and reach critical thresholds in these areas of discovery. Observations with CMB-S4 will also open a new observational window of the time-varying millimeter sky. I will give an overview of the science achievable with CMB-S4 and the latest project status. |
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