Members in the departments of physics and astronomy who work on dark matter and neutrino-related fields are invited to get together to discuss papers related to their field. Topics include: neutrinos, dark matter, BSM physics, fundamental symmetries, precision physics and more.
Contact Xiran Bai and Eleanor Graham for more information.
Ultra-relativistic heavy-ion collisions produce a hot and dense QCD matter, called Quark-Gluon Plasma (QGP). Unlike in ordinary matter, quarks and gluons are not confined within short distances but can roam freely over distances larger than the hadronic scale in the state of QGP. Understanding this novel state of matter offers a new way to learn how quarks and gluons bind to form stable particles like the proton.
Talia Weiss will lead a discussion on the paper “Anomalies in Particle Physics” found at https://arxiv.org/abs/2309.03870.pdf
See also: “The Era of Anomalies” found at https://physics.aps.org/articles/v13/79
Members in the departments of physics and astronomy who work on dark matter and neutrino-related fields are invited to get together to discuss papers related to their field. Topics include: neutrinos, dark matter, BSM physics, fundamental symmetries, precision physics and more.
Contact Xiran Bai and Eleanor Graham for more information.
Long-baseline neutrino oscillation experiments present some of the most compelling paths toward physics beyond the standard model. Measurement of the leptonic mixing matrix through oscillation and observation of the degree of leptonic CP violation demonstrates a proof of concept for understanding the difference between matter and anti-matter in the observable universe. State of the art experiments like NOvA and T2K are currently performing measurements of neutrino oscillation, but ultimately, will be statistically limited.
Eleanor Graham will lead a discussion on the paper “Synchronous Detection of Cosmic Rays and Correlated Errors in Superconducting Qubit Arrays” found at https://arxiv.org/pdf/2402.03208.pdf
Members in the departments of physics and astronomy who work on dark matter and neutrino-related fields are invited to get together to discuss papers related to their field. Topics include: neutrinos, dark matter, BSM physics, fundamental symmetries, precision physics and more.
Contact Xiran Bai and Eleanor Graham for more information.
In this talk, I’ll describe how we use solid-state spin ensembles, magnetic resonance, and quantum sensing techniques to search for axion dark matter in the third-generation CASPEr-e detector. Discovering and characterizing axion dark matter could resolve the longstanding Strong CP Problem, in addition to revealing the identity of dark matter. The Strong CP Problem stems from the puzzling lack of a CP-violating permanent electric dipole moment (EDM) in nucleons.
The matter inside of a neutron star (NS) exists in an ultra-dense, cold state that we are unable to reproduce in Earth-based laboratories. Hence the only way to understand how matter behaves in this environment, i.e. determining the Equation of State (EoS), is through observations of these objects. NSs in low-mass X-ray binaries, where matter is stripped from a stellar companion to form an accretion disk, provide a unique opportunity to learn more about accretion physics and properties of the compact object itself.
Members in the departments of physics and astronomy who work on dark matter and neutrino-related fields are invited to get together to discuss papers related to their field. Topics include: neutrinos, dark matter, BSM physics, fundamental symmetries, precision physics and more.
Contact Xiran Bai and Eleanor Graham for more information.
It was the best of times, it was the worst of times. Just as the classic English novel lends its title well to the spirit of understanding symmetries in the standard model (SM), the opening words also concisely sum up the status of beyond standard model (BSM) physics searches through tests of the fundamental symmetric matrices over the past few decades. Despite the identical mathematical formalism that generates these matrices in the SM, empirically the level of observed mixing within these two are dramatically different.
