SUSY24: The 31st International Conference on Supersymmetry and Unification of Fundamental Interactions

10 Jun 2024, 10:00 → 14 Jun 2024, 18:10 Europe/Madrid

IFT (Madrid, Spain)

Luis Ibanez, Sven Heinemeyer (CSIC (Madrid, ES))

The Conferences on Supersymmetry and Unification of Fundamental Interactions (SUSY) are among the largest international events where particle physicists come together to discuss innovative ideas pertaining to fundamental interactions among elementary particles.

The aim of the SUSY conference is to review and discuss recent research related to supersymmetric theories and all other approaches to physics beyond the Standard Model in all aspects, including formal theory, phenomenology, experiment, astrophysics, cosmology, etc.

The Institute of Theoretical Physics (IFT, Madrid) is responsible for organising the 31st International Conference on Supersymmetry and Unification of Fundamental Interactions (SUSY 2024).

Registration will open on 15/02 and close on 31/05. Abstract submission is extended until the 13 of May. 

WARNING:  Please be wary of fraudulent/phishing emails offering to book accommodation for the conference. We have not organized central reservations/bookings nor partnered with any companies for this. Any email of this kind you receive is spam. And of course in case of any doubts, please contact us directly!

 

 

Please contact susy24madrid@gmail.com in case of questions.

posterFinalSUSY24.pdf

Monday, 10 June

Plenaries

1 SUSY: Where are we

Speaker: Stephen Frederick King (Southampton University)

2 SUSY searches at ATLAS

Speaker: Joaquin Hoya (Argonne National Laboratory (US))

3 SUSY searches at CMS

Speaker: Malgorzata Kazana (NCBJ Warsaw (PL))

11:40 Coffee Break

Plenaries

4 Entanglement and collider physics

Speaker: Alan Barr (University of Oxford (GB))

5 SM (icluding top quark) measurements at LHC

Speaker: James Ferrando (Lancaster University (GB))

13:10 Lunch

Alternatives to SUSY / Non-SUSY BSM

Dark matter, astroparticles and gravitational waves

Flavour physics and neutrinos

Higgs: theory and experiment

16:40 Coffee Break

Alternatives to SUSY / Non-SUSY BSM

Dark matter, astroparticles and gravitational waves

Higgs: theory and experiment

SUSY, strings and QFT

19:00 Reception

Tuesday, 11 June

Plenaries

6 Measurements on SM Higgs at ATLAS and CMS

Speaker: Javier Cuevas (Universidad de Oviedo (ES))

7 Searches for non-SM Higgs at CMS

Speaker: Alexis Kalogeropoulos (The State University of New York SUNY (US))

8 Searches for non-SM Higgs at ATLAS

Speaker: Weitao Wang (University of Iowa (US))

11:40 Coffee Break

Plenaries

9 BSM Higgs physics - theory

Speaker: Georg Ralf Weiglein (Deutsches Elektronen-Synchrotron (DE))

10 Status of Flavour Physics and Anomalies

Speaker: Wolfgang Altmannshofer (UC Santa Cruz)

13:10 Lunch

Alternatives to SUSY / Non-SUSY BSM

Dark matter, astroparticles and gravitational waves

Higgs: theory and experiment

Joint Session: Flavour/Neutrinos/Dark Matter

16:40 Coffee Break

Roundtable: The future of particle physics

Carlos Wagner (Argonne National Laboratory)
Marcela Carena (Fermilab)
Karl Jakobs (Freiburg)
Greg Landsberg (Brown Univ.)
Antonio Delgado (Notre Dame)

Wednesday, 12 June

Plenaries

11 Overview: direct DM searches

Speaker: Wolfgang Rau

12 Overview: indirect DM searches

Speaker: Prof. Michele Doro (University of Padova)

13 Talk 1: DM theo/pheno/ALPS

Speaker: Geraldine Servant (Deutsches Elektronen-Synchrotron (DE))

11:40 Coffee Break

Plenaries

14 Talk 2: DM theo/pheno/ALPS

Speaker: Riccardo Catena (Chalmers University of Technology, Göteborg, Sweden)

15 Exotics at A/C

Dark sectors, ALPs, Long Lived

13:10 Lunch

15:00 Excursion / Social Event

Thursday, 13 June

Plenaries

16 Talk on GW exp + phenomenological implications

Speaker: Bruce Allen (Max Planck Society/Albert Einstein Institute Hannover)

17 FOEWPT in the early universe

Speaker: Michael Ramsey-Musolf (U. Massachusetts Amherst)

18 Highlights in Cosmology

Speaker: Dr Vivian Poulin (LUPM, CNRS & U. de Montpellier, France)

11:40 Coffee Break

Plenaries

19 Neutrino physics: exp. Status and phenomenological implications

Speaker: Prof. Concepcion Gonzalez-Garcia (YITP, Stony Brook and ICREA, U. Barcelona)

20 Quantum technologies for fundamental physics

Speaker: Diego Blas (UAB/IFAE)

13:10 Lunch

Alternatives to SUSY / Non-SUSY BSM

Dark matter, astroparticles and gravitational waves

Flavour physics and neutrinos

Higgs: theory and experiment

16:40 Coffee Break

Cosmology and modified gravity

21 Curvature Perturbations Protected Against One Loop

I examine one-loop corrections from small-scale curvature perturbations to the superhorizon-limit ones in single-field inflation models, which have recently caused controversy. I consider the case where the Universe experiences transitions of slow-roll (SR) → intermediate period → SR. The intermediate period can be an ultra-slow-roll period or a resonant amplification period, either of which enhances small-scale curvature perturbations. I assume that the superhorizon curvature perturbations are conserved at least during each of the SR periods. Within this framework, I show that the superhorizon curvature perturbations during the first and the second SR periods coincide at one-loop level in the slow-roll limit.

Speaker: Keisuke Inomata (Jonhs Hopkins University)

22 CMB hotspots from tachyonic instability of the Higgs potential

At high energies, such as during inflation, the quartic coupling of the Standard Model (SM) Higgs potential runs negative, according to current measurements. This can lead the potential into a tachyonic regime, where the square of the mass of the SM Higgs becomes negative. This tachyonic instability can exponentially enhance Higgs particle production via Hubble-induced effects and via the dynamics of the Higgs field itself. Furthermore the enhanced Higgs particle production can draw energy out of the Higgs field and produce stabilizing thermal corrections.

The early produced Higgs particles would then modify the curvature perturbations of the early universe which in turn can cause hot or cold spots on the cosmic microwave background (CMB).
The aim of our work is to look into this enhanced Higgs particle production and calculate the temperature of the CMB hotspots, as well as looking into CMB hotspots from other sources such as primordial black holes.

Speaker: Julia Ziegler (Hamburg University)

23 Modular Stabilization and Modular Inflation

We propose a new classes of inflation models based on the modular symmetry, where modulus field $\tau$ serves as the inflaton. We make a connection between modular inflation and modular stabilization, and the modulus field rolls towards fixed point after inflation. We find the modular symmetry strongly constraints the possible shape of the potential and find some parameter space where the inflation predictions agree with cosmic microwave background observations. The tensor to scalar ratio is predicted to be smaller than $10^{-6}$ in our models, while the running of spectral index is in order of $10^{-4}$.

Speaker: Wenbin Zhao (Bethe Center for Theoretical Physics, University of Bonn)

24 Understanding the reheating dynamics and Baryogenesis

In this study, we explore the evolution of a system composed of an unstable scalar field ($\phi$), and radiation in the context of non-standard cosmology where initially the Universe is dominated by the energy density of $\phi$. Later, the unstable $\phi$ with decay width $\Gamma_\phi$ decays into radiation and we focus on two relevant quantities: the maximum radiation temperature $T_{max}$ and the temperature when the universe is dominated by the radiation (reheating temperature) $T_{RH}$. For a given universe's initial Hubble scale ($H_I$) we compare our numerical results from the Boltzmann equations with approximate results in two regimes: $H_I > \Gamma_\phi$ and $H_I < \Gamma_\phi$. Building upon our understanding of the system’s evolution during reheating, we further discuss the viability of Baryogenesis in this scenario.

Speaker: Gabriel Aragão (UFABC)

Higgs: theory and experiment

Joint Session: Flavour/Neutrinos/Dark Matter

SUSY, strings and QFT

21:00 Social Dinner

Friday, 14 June

Dark matter, astroparticles and gravitational waves

Flavour physics and neutrinos

Higgs: theory and experiment

SUSY, strings and QFT

11:40 Coffee Break

Cosmology and modified gravity

25 Dark Radiation Isocurvature from Cosmological Phase Transitions

Cosmological first order phase transitions are typically associated with physics beyond the Standard Model, and thus of great theoretical and observational interest. Models of phase transitions where the energy is mostly converted to dark radiation can be constrained through limits on the dark radiation energy density (parameterized by $\Delta N_{\rm eff}$). However, the current constraint ($\Delta N_{\rm eff} < 0.3$) assumes the perturbations are adiabatic. We point out that a broad class of non-thermal first order phase transitions that start during inflation but do not complete until after reheating leave a distinct imprint in the scalar field from bubble nucleation. Dark radiation inherits the perturbation from the scalar field when the phase transition completes, leading to large-scale isocurvature that would be observable in the CMB. We perform a detailed calculation of the isocurvature power spectrum and derive constraints on $\Delta N_{\rm eff}$ based on CMB+BAO data. For a reheating temperature of $T_{\rm rh}$ and a nucleation temperature $T_*$, the constraint is approximately $\Delta N_{\rm eff}\lesssim 10^{-5} (T_*/T_{\rm rh})^{-4}$, which can be much stronger than the adiabatic result. We also point out that since perturbations of dark radiation have a non-Gaussian origin, searches for non-Gaussianity in the CMB could place a stringent bound on $\Delta N_{\rm eff}$ as well.

Speaker: Mitchell Weikert (Rutgers University)

26 Cold dark matter particle mass, size, and properties and axion-like dark radiation in ΛCDM cosmology

A new theory is presented to estimate the mass, size, lifetime, and other properties of cold dark matter particles (CDM) within the ΛCDM cosmology. Using Illustris simulations, we demonstrate the existence of mass and energy cascade that facilitates the formation of hierarchical structures. A scale-independent rate of cascade $\varepsilon_u\approx 10^{-7}m^2/s^3$ can be identified. The energy cascade leads to universal scaling laws on relevant scales r, i.e. a two-thirds law for kinetic energy ($v_r^2\propto \varepsilon_u^{2/3} r^{2/3}$) and a four-thirds law for DM halo density ($\rho_r\propto \varepsilon_u^{2/3}G^{-1}r^{-4/3}$), where G is the gravitational constant. For cold and collisionless dark matter that interacts via gravity only, these scaling laws can be extended down to the smallest scale, that is, a free streaming scale. For standard WIMPs, that scale is about Earth's mass. For superheavy dark matter particles of mass $10^{12}$GeV, the free streaming mass can be comparable to the particle mass such that quantum effects can be important on that scale. Combined with the uncertainty principle and virial theorem, three constants ($\varepsilon_u$, $\hbar$, and G) dominate the physics on that scale, so that the properties of CDM can be estimated. We estimate a mass $m_X=(\varepsilon_u\hbar^5G^{-4})^{1/9}=10^{12}$GeV, a size $l_X=(\varepsilon_u^{-1}\hbar G)^{1/3}=10^{-13}$m, and a lifetime $\tau_X=c^2/\varepsilon_u=10^{16}$ years for CDM particles. Here, $\hbar$ is the Planck constant and c is the speed of light. The typical energy on that scale $E_X=(\varepsilon_u^5\hbar^7G^{-2})^{1/9}=10^{-9}$eV suggests a “dark radiation” field to provide a viable mechanism for the energy dissipation during gravitational collapsing of CDM. If existing, the “dark radiation" should be produced around $t_X=(\varepsilon_u^{-5}\hbar^2G^2)^{1/9}=10^{-6}$s (quark epoch) with mass of $10^{-9}$eV, a GUT scale decay constant $10^{16}$GeV, or an effective axion-photon coupling $10^{-18}$GeV$^{-1}$, such that the axion particle can be a very promising candidate for “dark radiation". The energy density of “dark radiation” is estimated to be about 1% of the cosmic microwave background (CMB). This work suggests a heavy dark matter scenario created during inflationary epoch along with a light axion-like dark radiation field. Potential extension to self-interacting dark matter is also presented. More details can be found at arXiv:2202.07240.

Speaker: Zhijie (Jay) Xu (Pacific Northwest National Lab)

27 A minimal solution to the axion isocurvature problem from a non-minimal coupling

The main limitation for pre-inflationary breaking of Peccei-Quinn (PQ) symmetry is the upper bound on the Hubble rate during inflation from axion isocurvature fluctuations. This leads to a tension between high scale inflation and QCD axions with Grand Unified Theory (GUT) scale decay constants, which reduces the potential for a detection of tensor modes at next generation CMB experiments. We propose a mechanism that excplicitly breaks PQ symmetry via non-minimal coupling to gravity, that lifts the axion mass above the Hubble scale during inflation and has negligible impact on today's axion potential. The initially heavy axion gets trapped at an intermediate minimum during inflation given by the phase of the non-minimal coupling, before it moves to its true CP-conserving minimum after inflation. During this stage it undergoes coherent oscillations around an adiabatically decreasing minimum, which slightly dilutes the axion energy density, while still being able to explain the observed dark matter relic abundance. This scenario can be tested by the combination of next generation CMB surveys like CMB-S4 and LiteBIRD with haloscopes such as ABRACADABRA or CASPEr-Electric.

Speaker: Maximilian Berbig (IFIC & University of Valencia)

Higgs: theory and experiment

Joint Session: Flavour/Neutrinos/Dark Matter

SUSY, strings and QFT

13:10 Lunch

Plenaries

28 Beyond the Standard Model Physics at colliders

Speaker: Benjamin Fuks

29 (g-2)_mu theory status

Speaker: Gilberto Colangelo

30 Swampland: review and phenomenological implications

Speaker: Alvaro Herraez Escudero (D)

16:40 Coffee Break

Plenaries

31 SUSY in Future Experiments

Speaker: Jenny List (Deutsches Elektronen-Synchrotron (DE))

32 What comes beyond the Standard Model?