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  • 151.
    Kopp, Michael
    et al.
    Nordita SU Stockholm Univ, Hannes Alfvens Vag 12, SE-10691 Stockholm, Sweden..
    Fragkos, Vasileios
    Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden..
    Pikovski, Igor
    Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden.;Stevens Inst Technol, Dept Phys, Hoboken, NJ 07030 USA..
    Nonclassicality of axionlike dark matter through gravitational self-interactions2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 106, no 4, article id 043517Article in journal (Refereed)
    Abstract [en]

    Axionlike particles (ALPs) are promising dark matter candidates. They are typically described by a classical field, motivated by large phase space occupation numbers. Here we show that such a description is accompanied by a quantum effect: squeezing due to gravitational self-interactions. For a typical QCD axion today, the onset of squeezing is reached on mu s scales and grows over millennia. Thus within the usual models based on the classical Schrodinger-Poisson equation, a type of Gross-Pitaevskii equation, any viable ALP is nonclassical. We also show that squeezing may be relevant on the scales of other self -gravitating systems such as galactic haloes, or solitonic cores. Conversely, our results highlight the incompleteness and limitations of the classical single field description of ALPs.

  • 152.
    Kuhnel, Florian
    et al.
    KTH, School of Engineering Sciences (SCI), Physics, Theoretical Particle Physics. Stockholm Univ, Sweden.
    Freese, Katherine
    Constraints on primordial black holes with extended mass functions2017In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 95, no 8, article id 083508Article in journal (Refereed)
    Abstract [en]

    Constraints on primordial black holes in the range 10(-18) M circle dot to 10(3) M circle dot are reevaluated for a general class of extended mass functions. Whereas previous work has assumed that PBHs are produced with one single mass, instead there is expected to be a range of masses even in the case of production from a single mechanism; constraints therefore change from previous literature. Although tightly constrained in the majority of cases, it is shown that, even under conservative assumptions, primordial black holes in the mass range 10(-10) M circle dot to 10(-8) M circle dot could still constitute the entirety of the dark matter. This stresses both the importance for a comprehensive reevaluation of all respective constraints that have previously been evaluated only for a monochromatic mass function and the need to obtain more constraints in the allowed mass range.

  • 153.
    Kuhnel, Florian
    et al.
    KTH, School of Engineering Sciences (SCI), Physics, Theoretical Particle Physics. AlbaNova University Center, Sweden.
    Ohlsson, Tommy
    KTH, School of Engineering Sciences (SCI), Physics, Theoretical Particle Physics. AlbaNova University Center, Sweden; University of Iceland, Iceland.
    Signatures of compact halos of sterile-neutrino dark matter2017In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 96, no 10, article id 103020Article in journal (Refereed)
    Abstract [en]

    We investigate compact halos of sterile-neutrino dark matter and examine observable signatures with respect to neutrino and photon emission. Primarily, we consider two cases: primordial black-hole halos and ultracompact minihalos. In both cases, we find that there exists a broad range of possible parameter choices such that detection in the near future with x-ray and gamma-ray telescopes might be well possible. In fact, for energies above 10 TeV, the neutrino telescope IceCube would be a splendid detection machine for such macroscopic dark-matter candidates.

  • 154.
    Litsa, Aliki
    et al.
    Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden..
    Freese, Katherine
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden.;Univ Texas Austin, Dept Phys, Austin, TX 78722 USA.;Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden..
    Sfakianakis, Evangelos, I
    Barcelona Inst Sci & Technol BIST, Inst Fis Altes Energies IFAE, Campus UAB, Barcelona 08193, Spain.;Nikhef, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands.;Leiden Univ, Inst Lorentz Theoret Phys, NL-2333 CA Leiden, Netherlands..
    Stengel, Patrick
    Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, AlbaNova, S-10691 Stockholm, Sweden.;Scuola Int Super Avanzati SISSA, Via Bonomea 265, I-34136 Trieste, Italy.;Ist Nazl Fis Nucl, Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy.;Inst Fundamental Phys Universe IFPU, Via Beirut 2, I-34151 Trieste, Italy..
    Visinelli, Luca
    Ist Nazl Fis Nucl, Lab Nazl Frascati, CP 13, I-100044 Frascati, Italy.;Shanghai Jiao Tong Univ, Tsung Dao Lee Inst TDLI, Shanghai 200240, Peoples R China..
    Large density perturbations from reheating to standard model particles due to the dynamics of the Higgs boson during inflation2021In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 104, no 12, article id 123546Article in journal (Refereed)
    Abstract [en]

    Cosmic microwave background observations are used to constrain reheating to standard model (SM) particles after a period of inflation. As a light spectator field, the SM Higgs boson acquires large field values from its quantum fluctuations during inflation, gives masses to SM particles that vary from one Hubble patch to another, and thereby produces large density fluctuations. We consider both perturbative and resonant decay of the inflaton to SM particles. For the case of perturbative decay from coherent oscillations of the inflaton after high scale inflation, we find strong upper bounds on the reheat temperature for the inflaton decay into heavy SM particles. The strongest bounds arise in the case of reheating to top quarks where we find Treh less than or similar to Oo1012 thorn GeV for an inflaton mass of 1013 GeV. For the case of resonant particle production (preheating) to (Higgsed) SM gauge bosons, we find temperature fluctuations larger than observed in the cosmic microwave background for a range of gauge coupling that includes those found in the SM and conclude that such preheating cannot be the main source of reheating the Universe after inflation.

  • 155.
    Manenti, Laura
    et al.
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Mishra, Umang
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Bruno, Gianmarco
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Roberts, Henry
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Oikonomou, Panos
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Pasricha, Renu
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Sarnoff, Isaac
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Weston, James
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Arneodo, Francesco
    New York Univ Abu Dhabi, Div Sci, Abu Dhabi, U Arab Emirates.;New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates..
    Di Giovanni, Adriano
    New York Univ Abu Dhabi, Ctr Astro Particle & Planetary Phys CAP3, Abu Dhabi, U Arab Emirates.;Gran Sasso Sci Inst GSSI, Via Iacobucci 2, I-67100 Laquila, Italy.;Ist Nazl Fis Nucl INFN, Lab Nazl Gran Sasso, I-67100 Laquila, Italy..
    Millar, Alexander John
    Stockholm Univ, Dept Phys, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden.; S-10691 Stockholm, Sweden.;Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.;Nordita SU.
    Mora, Knut Dundas
    Columbia Univ, Phys Dept, New York, NY 10027 USA..
    Search for dark photons using a multilayer dielectric haloscope equipped with a single-photon avalanche diode2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 105, no 5, article id 052010Article in journal (Refereed)
    Abstract [en]

    We report the results of the search for dark photons with mass around 1.5 eV/c(2) using a multilayer dielectric haloscope equipped with an affordable and commercially available photosensor. The multilayer stack, which enables the conversion of dark photons (DP) to Standard Model photons, is made of 23 bilayers of alternating SiO2 and Si3N4 thin films with linearly increasing thicknesses through the stack (a configuration known as a "chirped stack"). The thicknesses have been chosen according to an optimization algorithm in order to maximize the DP-photon conversion in the energy region where the photosensor sensitivity peaks. This prototype experiment, dubbed "MuDHI" (Multilayer Dielectric Haloscope Investigation) by the authors of this paper, has been designed, developed, and run at the Astroparticle Laboratory of New York University Abu Dhabi, which marks the first time a dark matter experiment has been operated in the Middle East. No significant signal excess is observed, and the method of maximum log likelihood is used to set exclusion limits at 90% confidence level on the kinetic mixing coupling constant between dark photons and ordinary photons.

  • 156.
    Manikandan, Sreenath K.
    et al.
    Nordita SU;Stockholm Univ, Hannes Alfvens Vag 12, SE-10691 Stockholm, Sweden..
    Rajeev, Karthik
    Indian Assoc Cultivat Sci, Sch Phys Sci, Kolkata 700032, India.;Indian Inst Technol, Dept Phys, Mumbai 400076, Maharashtra, India..
    New kind of echo from quantum black holes2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 105, no 6, article id 064024Article in journal (Refereed)
    Abstract [en]

    We propose that a quantum black hole can produce a new kind of late-time gravitational echoes, facilitated by a near-horizon process analogous to Andreev reflection in condensed matter systems. In comparison to the traditional echo scenarios where the near-horizon region is treated as an ordinary reflector, we argue that, consequent to near-horizon gravitational scattering, this region is better described by an Andreev reflector. Such interactions lead to a novel contribution to gravitational echoes with a characteristic phase difference, an effect which is analogous to how Andreev reflections lead to propagating particlelike and holelike components with a relative phase in certain condensed matter scenarios. Moreover, this novel contribution to the echo signal encodes information about the "near-horizon quantum state," hence offering a possible new window to probe the quantum nature of black holes.

  • 157. Maria Ezquiaga, Jose
    et al.
    Garcia-Bellido, Juan
    Zumalacarregui, Miguel
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Field redefinitions in theories beyond Einstein gravity using the language of differential forms2017In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 95, no 8, article id 084039Article in journal (Refereed)
    Abstract [en]

    We study the role of field redefinitions in general scalar-tensor theories. In particular, we first focus on the class of field redefinitions linear in the spin-2 field and involving derivatives of the spin-0 mode, generically known as disformal transformations. We start by defining the action of a disformal transformation in the tangent space. Then, we take advantage of the great economy of means of the language of differential forms to compute the full transformation of Horndeski's theory under general disformal transformations. We obtain that Horndeski's action maps onto itself modulo a reduced set of non-Horndeski Lagrangians. These new Lagrangians are found to be invariant under disformal transformation that depend only in the first derivatives of the scalar. Moreover, these combinations of Lagrangians precisely appear when expressing in our basis the constraints of the recently proposed extended scalar-tensor theories. These results allow us to classify the different orbits of scalar-tensor theories invariant under particular disformal transformations, namely, the special disformal, kinetic disformal, and disformal Horndeski orbits. In addition, we consider generalizations of this framework. We find that there are possible well-defined extended disformal transformations that have not been considered in the literature. However, they generically cannot link Horndeski theory with extended scalar-tensor theories. Finally, we study further generalizations in which extra fields with different spin are included. These field redefinitions can be used to connect different gravity theories such as multiscalar-tensor theories, generalized Proca theories, and bigravity. We discuss how the formalism of differential forms could be useful for future developments in these lines.

  • 158.
    Marsh, David J.E.
    et al.
    Department of Physics, King's College London, Strand, London WC2R 2LS, United Kingdom, Strand.
    McDonald, Jamie I.
    Centre for Cosmology, Particle Physics and Phenomenology (CP3), Universitè Catholique de Louvain, Chemin du cyclotron 2, Louvain-la-Neuve B-1348, Belgium, Chemin du cyclotron 2.
    Millar, Alexander J.
    NORDITA SU; The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden, AlbaNova; Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, 10691 Stockholm, Sweden, Roslagstullsbacken 23; Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA.
    Schütte-Engel, Jan
    Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA; Illinois Center for Advanced Studies of the Universe, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
    Axion detection with phonon-polaritons revisited2023In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 107, no 3, article id 035036Article in journal (Refereed)
    Abstract [en]

    In the presence of a background magnetic field, axion dark matter induces an electric field and can thus excite phonon-polaritons in suitable materials. We revisit the calculation of the axion-photon conversion power output from such materials, accounting for finite volume effects, and material losses. Our calculation shows how phonon-polaritons can be converted to propagating photons at the material boundary, offering a route to detecting the signal. Using the dielectric functions of GaAs, Al2O3, and SiO2, a fit to our loss model leads to a signal of lower magnitude than previous calculations. We demonstrate how knowledge of resonances in the dielectric function can directly be used to calculate the sensitivity of any material to axion dark matter. We argue that a combination of low losses encountered at O(1) K temperatures and near future improvements in detector dark count allow one to probe the QCD axion in the mass range ma≈100 meV. This provides further impetus to examine novel materials and further develop detectors in the THz regime. We also discuss possible tuning methods to scan the axion mass.

  • 159. Millar, Alexander J.
    et al.
    Lawson, Matthew
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden..
    Marvinney, Claire
    Univ Calif Berkeley, Dept Nucl Engn, Berkeley, CA 94720 USA..
    Searching for dark matter with plasma haloscopes2023In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 107, no 5, article id 055013Article in journal (Refereed)
    Abstract [en]

    We summarize the recent progress of the Axion Longitudinal Plasma Haloscope (ALPHA) Consortium, a new experimental collaboration to build a plasma haloscope to search for axions and dark photons. The plasma haloscope is a novel method for the detection of the resonant conversion of light dark matter to photons. ALPHA will be sensitive to QCD axions over almost a decade of parameter space, potentially discovering dark matter and resolving the strong CP problem. Unlike traditional cavity haloscopes, which are generally limited in volume by the Compton wavelength of the dark matter, plasma haloscopes use a wire metamaterial to create a tuneable artificial plasma frequency, decoupling the wavelength of light from the Compton wavelength and allowing for much stronger signals. We develop the theoretical foundations of plasma haloscopes and discuss recent experimental progress. Finally, we outline a baseline design for ALPHA and show that a full-scale experiment could discover QCD axions over almost a decade of parameter space.

  • 160.
    Millar, Alexander
    et al.
    Stockholm Univ, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, S-10691 Stockholm, Sweden.;Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.;Nordita SU.
    Raffelt, Georg
    Werner Heisenberg Inst, Max Planck Inst Phys, Fohringer Ring 6, D-80805 Munich, Germany..
    Stodolsky, Leo
    Werner Heisenberg Inst, Max Planck Inst Phys, Fohringer Ring 6, D-80805 Munich, Germany..
    Vitagliano, Edoardo
    Werner Heisenberg Inst, Max Planck Inst Phys, Fohringer Ring 6, D-80805 Munich, Germany..
    Neutrino mass from bremsstrahlung endpoint in coherent scattering on nuclei2018In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 98, no 12, article id 123006Article in journal (Refereed)
    Abstract [en]

    We calculate the coherent bremsstrahlung process nu + N -> N + nu + gamma off a nucleus H with the aim of revealing the neutrino mass via the photon endpoint spectrum. Unfortunately, the large required power of a monochromatic neutrino source and/or large detector mass make it difficult to compete with traditional electron-spectrum endpoint measurements in nuclear beta decay. Our neutral-current process distinguishes between Dirac and Majorana neutrinos, but the change of the photon spectrum is of the order of m(nu)/E-nu and thus very small, despite the final-state neutrino coming to rest at the photon endpoint. So the "Dirac-Majorana confusion theorem" remains intact even if E-nu >> m(nu) my applies only for the initial state.

  • 161.
    Musaeus, Jørgen
    et al.
    School of Mathematics and Maxwell Institute for Mathematical Sciences, University of Edinburgh, Peter Guthrie Tait Road, Edinburgh EH9 3FD, United Kingdom, Peter Guthrie Tait Road.
    Obers, Niels A.
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm University, Hannes Alfvéns väg 12, SE-106 91 Stockholm, Sweden, Hannes Alfvéns väg 12; Niels Bohr International Academy, The Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, DK-2100 Copenhagen Ø, Denmark.
    Oling, Gerben
    School of Mathematics and Maxwell Institute for Mathematical Sciences, University of Edinburgh, Peter Guthrie Tait Road, Edinburgh EH9 3FD, United Kingdom, Peter Guthrie Tait Road.
    Setting the connection free in the Galilei and Carroll expansions of gravity2024In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 109, no 10, article id 104040Article in journal (Refereed)
    Abstract [en]

    We obtain a Palatini-type formulation for the Galilei and Carroll expansions of general relativity, where the connection is promoted to a variable. Known versions of these large and small speed of light expansions are derived from the Einstein-Hilbert action and involve dynamical Newton-Cartan or Carroll geometry, along with additional gauge fields at subleading orders. The corresponding Palatini actions that we obtain in this paper are derived from an appropriate expansion of the Einstein-Palatini action, and the connection variable reduces to the Galilei- or Carroll-adapted connection on shell. In particular, we present the Palatini form for the next-to-leading-order Galilean action and recover the known equations of motion. We also compute the leading-order Palatini-type action for the Carrollian case and show that, while it depends on the connection variable, it reduces on shell to the known action of electric Carroll gravity, which only depends on extrinsic curvature.

  • 162. Nersisyan, Henrik
    et al.
    Akrami, Yashar
    Amendola, Luca
    Koivisto, Tomi S.
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Rubio, Javier
    Solomon, Adam R.
    Instabilities in tensorial nonlocal gravity2017In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 95, no 4, article id 043539Article in journal (Refereed)
    Abstract [en]

    We discuss the cosmological implications of nonlocal modifications of general relativity containing tensorial structures. Assuming the presence of standard radiation-and matter-dominated eras, we show that, except in very particular cases, the nonlocal terms contribute a rapidly growing energy density. These models therefore generically do not have a stable cosmological evolution.

  • 163.
    Niedermann, Florian
    et al.
    NORDITA SU, Hannes Alfvens Vag 12, SE-10691 Stockholm, Sweden.;Stockholm Univ, Hannes Alfvens Vag 12, SE-10691 Stockholm, Sweden..
    Sloth, Martin S.
    Univ Southern Denmark, Ctr Cosmol & Particle Phys Phenomenol, CP3 Origins, Campusvej 55, DK-5230 Odense M, Denmark..
    Hot new early dark energy2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 105, no 6, article id 063509Article in journal (Refereed)
    Abstract [en]

    New early dark energy (NEDE) makes the cosmic microwave background consistent with a higher value of the Hubble constant inferred from supernovae observations. It is a better alternative to the old EDE model because it explains naturally the decay of the extra energy component in terms of a vacuum first order phase transition that is triggered by a subdominant scalar field at zero temperature. With hot NEDE, we introduce a new mechanism to trigger the phase transition. It relies on thermal corrections that subside as a subdominant radiation fluid in a dark gauge sector cools. We explore the phenomenology of hot NEDE and identify the strong supercooled regime as the scenario favored by phenomenology. In a second step, we propose different microscopic embeddings of hot NEDE. This includes the (non-)Abelian dark matter model, which has the potential to also resolve the LSS tension through interactions with the dark radiation fluid. We also address the coincidence problem generically present in EDE models by relating NEDE to the mass generation of neutrinos via the inverse seesaw mechanism. We finally propose a more complete dark sector model, which embeds the NEDE field in a larger symmetry group and discuss the possibility that the hot NEDE field is central for spontaneously breaking lepton number symmetry.

  • 164.
    Niemi, Lauri
    et al.
    Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland.;Univ Helsinki, Helsinki Inst Phys, POB 64, FI-00014 Helsinki, Finland..
    Schicho, Philipp
    Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland.;Univ Helsinki, Helsinki Inst Phys, POB 64, FI-00014 Helsinki, Finland..
    Tenkanen, Tuomas
    Nordita SU.
    Singlet-assisted electroweak phase transition at two loops2021In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 103, no 11, article id 115035Article in journal (Refereed)
    Abstract [en]

    We investigate the electroweak phase transition in the real-singlet extension of the Standard Model at two-loop level, building upon existing one-loop studies. We calculate the effective potential in the high-temperature approximation and detail the required resummations at two-loop order. In typical strongtransition scenarios, we find deviations of order 20%-50% from one-loop results in transition strength and critical temperature for both one- and two-step phase transitions. For extremely strong transitions, the discrepancy with one-loop predictions is even larger, presumably due to sizable scalar couplings in the tree-level potential. Along the way, we obtain a dimensionally reduced effective theory applicable for nonperturbative lattice studies of the model.

  • 165. O'Hare, C. A. J.
    et al.
    Caputo, A.
    Millar, Alexander
    he Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova, 10691 Stockholm, Sweden;Nordita SU.
    Vitagliano, E.
    Axion helioscopes as solar magnetometers2020In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 102, no 4, article id 043019Article in journal (Refereed)
    Abstract [en]

    Axion helioscopes search for solar axions and axionlike particles via inverse Primakoff conversion in strong laboratory magnets pointed at the Sun. Anticipating the detection of solar axions, we determine the potential for the planned next-generation helioscope, the International Axion Observatory (IAXO), to measure or constrain the solar magnetic field. To do this we consider a previously neglected component of the solar axion flux at sub-keV energies arising from the conversion of longitudinal plasmons. This flux is sensitively dependent to the magnetic field profile of the Sun, with lower energies corresponding to axions converting into photons at larger solar radii. If the detector technology eventually installed in IAXO has an energy resolution better than 200 eV, then solar axions could become an even more powerful messenger than neutrinos of the magnetic field in the core of the Sun. For energy resolutions better than 10 eV, IAXO could access the inner 70% of the Sun and begin to constrain the field at the tachocline: the boundary between the radiative and convective zones. The longitudinal plasmon flux from a toroidal magnetic field also has an additional 2% geometric modulation effect which could be used to measure the angular dependence of the magnetic field.

  • 166.
    Ong, Yen Chin
    et al.
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Yao, Yuan
    Yangzhou Univ, Coll Phys Sci & Technol, Ctr Gravitat & Cosmol, Yangzhou 225009, Jiangsu, Peoples R China..
    Generalized uncertainty principle and white dwarfs redux: How the cosmological constant protects the Chandrasekhar limit2018In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 98, no 12, article id 126018Article in journal (Refereed)
    Abstract [en]

    It was previously argued that generalized uncertainty principle (GUP) with a positive parameter removes the Chandrasekhar limit. One way to restore the limit is by taking the GUP parameter to be negative. In this work we discuss an alternative method that achieves the same effect: by including a cosmological constant term in the GUP (known as "extended GUP" in the literature). We show that an arbitrarily small but nonzero cosmological constant can restore the Chandrasekhar limit. We also remark that if the extended GUP is correct, then the existence of white dwarfs gives an upper bound for the cosmological constant, which-while still large compared to observation-is approximately 86 orders of magnitude smaller than the natural scale.

  • 167.
    Porter, T. A.
    et al.
    Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.;Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA..
    Rowell, G. P.
    Univ Adelaide, Sch Phys Sci, Adelaide, SA 5000, Australia..
    Johannesson, Guolaugur
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland..
    Moskalenko, I. V.
    Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.;Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA..
    Galactic PeVatrons and helping to find them: Effects of galactic absorption on the observed spectra of very high energy gamma-ray sources2018In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 98, no 4, article id 041302Article in journal (Refereed)
    Abstract [en]

    Identification of the cosmic-ray (CR) "PeVatrons," which are sources capable of accelerating particles to similar to 10(15) eV energies and higher, may lead to resolving the long-standing question of the origin of the spectral feature in the all-particle CR spectrum known as the "knee." Because CRs with these energies are deflected by interstellar magnetic fields identification of individual sources and determination of their spectral characteristics is more likely via very high energy gamma-ray emissions, which provide the necessary directional information. However, pair production on the interstellar radiation field (ISRF) and cosmic microwave background (CMB) leads to steepening of the high energy tails of gamma-ray spectra, and should be corrected for to enable true properties of the spectrum at the source to be recovered. Employing recently developed three-dimensional ISRF models this paper quantifies the pair-absorption effect on spectra for sources in the Galactic center (GC) direction at 8.5 and 23.5 kpc distances, with the latter corresponding to the far side of the Galactic stellar disc where it is expected that discrimination of spectral features >10 TeV is possible by the forthcoming Cherenkov Telescope Array (CTA). The estimates made suggest spectral cutoffs could be underestimated by factors of a few in the energy range so far sampled by TeV gamma-ray telescopes. As an example to illustrate this, the recent HESS measurements of diffuse gamma-ray emissions possibly associated with injection of CRs nearby Sgr A* are ISRF corrected, and estimates of the spectral cutoff are reevaluated. It is found that it could be higher by up to a factor of similar to 2, indicating that these emissions may be consistent with a CR accelerator with a spectral cutoff of at least 1 PeV at the 95% confidence level.

  • 168.
    Raikwal, Deepak
    et al.
    Harish-Chandra Research Institute, A CI of Homi Bhabha National Institute, Chhatnag Road, Jhunsi, Prayagraj - 211019, Chhatnag Road, Jhunsi; Homi Bhabha National Institute, Anushakti Nagar, Mumbai 400094, India, Anushakti Nagar.
    Choubey, Sandhya
    KTH, School of Engineering Sciences (SCI), Physics.
    Earth tomography with the ICAL detector at INO2024In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 109, no 7, article id 073011Article in journal (Refereed)
    Abstract [en]

    Observing matter effects in atmospheric neutrinos traveling through the entire mantle and core of the Earth is a promising way of enhancing our understanding of Earth's density structure. In that context we study the prospects of Earth tomography with the ICAL detector at the India-based Neutrino Observatory. While this experiment is smaller in size in comparison to some of the other larger detectors being proposed, it is the only planned neutrino experiment with charge-identification sensitivity. In particular, ICAL can see matter effects separately in neutrinos and antineutrinos. This has been seen to enhance ICAL's sensitivity to earth matter effects and hence the mass ordering sensitivity for both normal and inverted mass orderings. It is therefore pertinent to see if the ICAL sensitivity to earth tomography is competitive or better with respect to other experiments, especially for the inverted mass ordering, where other experiments suffer reduced sensitivity. We present the sensitivity of ICAL to earth tomography by taking into consideration both the Earth's mass constraint as well as the hydrostatic equilibrium constraints.

  • 169.
    Raikwal, Deepak
    et al.
    Harish-Chandra Research Institute, A CI of Homi Bhabha National Institute, Chhatnag Road, Jhunsi, Prayagraj-211019, India, Chhatnag Road, Jhunsi; Homi Bhabha National Institute, Anushakti Nagar, Mumbai 400094, India.
    Choubey, Sandhya
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. The Oskar Klein Centre, AlbaNova University Center, Roslagstullsbacken 21, SE-106 91 Stockholm, Sweden, Roslagstullsbacken 21.
    Ghosh, Monojit
    Center of Excellence for Advanced Materials and Sensing Devices, Ruder Bošković Institute, 10000 Zagreb, Croatia.
    Comprehensive study of Lorentz invariance violation in atmospheric and long-baseline experiments2023In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 107, no 11, article id 115032Article in journal (Refereed)
    Abstract [en]

    In this paper, we have presented a comprehensive study of Lorentz invariance violation (LIV) in the context of the atmospheric neutrino experiment ICAL and the long-baseline experiments T2HK and DUNE. Our study consists of the full parameter space of the LIV parameters, i.e., six CPT-violating LIV parameters (aαβ) and six CPT-conserving LIV parameters (cαβ). In this study, our objective is to calculate the upper bound on all the LIV parameters with respect to the individual experiments as well as their combination. Our results show that DUNE gives the best sensitivity for the parameters aee, aeμ, aeτ, and aμτ in its 7 years of running, whereas ICAL gives the best sensitivity on aμμ, aμτ, cee, cμμ, cττ, and cμτ in its 10 years of running. For aττ, the sensitivities of DUNE and ICAL are almost same. The combination of T2HK, DUNE, and ICAL gives the best sensitivity for aeμ and aee with respect to all the existing bounds in the literature. For the CPT-even diagonal parameters cee and cμμ, our work provides the first-ever bounds.

  • 170.
    Rydving, Erik
    et al.
    KTH, School of Engineering Sciences (SCI), Mathematics (Dept.), Mathematics (Div.).
    Aurell, Erik
    KTH, School of Electrical Engineering and Computer Science (EECS), Computer Science, Computational Science and Technology (CST).
    Pikovski, Igor
    Stevens Inst Technol, Dept Phys, Hoboken, NJ 07030 USA.;Stockholm Univ, Dept Phys, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden..
    Do Gedanken experiments compel quantization of gravity?2021In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 104, no 8, article id 086024Article in journal (Refereed)
    Abstract [en]

    Whether gravity is quantized remains an open question. To shed light on this problem, various Gedanken experiments have been proposed. One popular example is an interference experiment with a massive system that interacts gravitationally with another distant system, where an apparent paradox arises: even for spacelike separation the outcome of the interference experiment depends on actions on the distant system, leading to a violation of either complementarity or no-signaling. A recent resolution shows that the paradox is avoided when quantizing gravitational radiation and including quantum fluctuations of the gravitational field. Here we show that the paradox in question can also be resolved without considering gravitational radiation, relying only on the Planck length as a limit on spatial resolution. Therefore, in contrast to conclusions previously drawn, we find that the necessity for a quantum field theory of gravity does not follow from so far considered Gedanken experiments of this type. In addition, we point out that in the common realization of the setup the effects are governed by the mass octopole rather than the quadrupole. Our results highlight that no Gedanken experiment to date compels a quantum field theory of gravity, in contrast to the electromagnetic case.

  • 171.
    Sarin, Nikhil
    et al.
    Nordita SU; Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Clayton, Vic 3800, Australia.;Stockholm Univ, NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden.;Stockholm Univ, Dept Phys, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden..
    Lasky, Paul D.
    Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Clayton, Vic 3800, Australia..
    Vivanco, Francisco Hernandez
    Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Clayton, Vic 3800, Australia..
    Stevenson, Simon P.
    Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Hawthorn, Vic 3122, Australia..
    Chattopadhyay, Debatri
    Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Hawthorn, Vic 3122, Australia.;Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales..
    Smith, Rory
    Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Clayton, Vic 3800, Australia..
    Thrane, Eric
    Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.;OzGrav ARC Ctr Excellence Gravitat Wave Discovery, Clayton, Vic 3800, Australia..
    Linking the rates of neutron star binaries and short gamma-ray bursts2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 105, no 8, article id 083004Article in journal (Refereed)
    Abstract [en]

    Short gamma-ray bursts are believed to be produced by both binary neutron star (BNS) and neutron star-black hole (NSBH) mergers. We use current estimates for the BNS and NSBH merger rates to calculate the fraction of observable short gamma-ray bursts produced through each channel. This allows us to constrain merger rates of a BNS to R-BNS = 384(-213)(+431) Gpc(-3) yr(-1) (90% credible interval), a 16% decrease in the rate uncertainties from the second Laser Interferometer Gravitational Wave Observatory (LIGO)-Virgo Gravitational-Wave Transient Catalog. Assuming a top-hat emission profile with a large Lorentz factor, we constrain the average opening angle of gamma-ray burst jets produced in BNS mergers to approximate to 15 degrees. We also measure the fraction of BNS and NSBH mergers that produce an observable short gamma-ray burst to be 0.02(-0.01)(+0.02) and 0.01 +/- 0.01, respectively, and find that greater than or similar to 40% of BNS mergers launch jets (90% confidence). We forecast constraints for future gravitational-wave detections given different modeling assumptions, including the possibility that BNS and NSBH jets are different. With 24 BNS and 55 NSBH observations, expected within six months of the LIGO-Virgo-Kamioka Gravitational Wave Detector network operating at design sensitivity, it will be possible to constrain the fraction of BNS and NSBH mergers that launch jets with 10% precision. Within a year of observations, we can determine whether the jets launched in NSBH mergers have a different structure than those launched in BNS mergers and rule out whether greater than or similar to 80% of binary neutron star mergers launch jets. We discuss the implications of future constraints on understanding the physics of short gamma-ray bursts and binary evolution.

  • 172.
    Schneider, Aurel
    et al.
    Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland.
    Schaeffer, Timothée
    Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland.
    Giri, Sambit K.
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Cosmological forecast of the 21-cm power spectrum with the halo model of reionization2023In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 108, no 4, article id 043030Article in journal (Refereed)
    Abstract [en]

    The 21-cm power spectrum of reionization is a promising probe for cosmology and fundamental physics. Exploiting this new observable, however, requires fast predictors capable of efficiently scanning the very large parameter space of cosmological and astrophysical uncertainties. In this paper, we introduce the halo model of reionization (HMreio), a new analytical tool that combines the halo model of the cosmic dawn with the excursion-set bubble model for reionization, assuming an empirical correction factor to deal with overlapping ionization bubbles. First, HMreio is validated against results from the well-known seminumerical code 21 cmfast, showing a good overall agreement for wave-modes of k≲1 h/Mpc. Based on this result, we perform a Monte-Carlo Markov-Chain (MCMC) forecast analysis assuming mock data from 1000-hour observations with the low-frequency part of the Square Kilometre Array (SKA) observatory. We simultaneously vary the six standard cosmological parameters together with seven astrophysical parameters quantifying the abundance and spectral properties of sources. Depending on the assumed theory error, we find very competitive constraints on cosmological parameters. In particular, it will be possible to conclusively test current cosmological tensions related to the Hubble parameter (H0-tension) and the matter clustering amplitude (S8-tension). Furthermore, the sum of the neutrino masses can be strongly constrained, making it possible to determine the neutrino mass hierarchy at the ∼90 percent confidence level. However, these goals can only be achieved if the current modeling uncertainties are substantially reduced to below ∼3 percent.

  • 173.
    Schober, Jennifer
    et al.
    EPFL, Lab Astrophys, CH-1290 Sauverny, Switzerland..
    Rogachevskii, lgor
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Ben Gurion Univ Negev, Dept Mech Engn, POB 653, IL-84105 Beer Sheva, Israel.;Stockholm Univ, S-10691 Stockholm, Sweden..
    Brandenburg, Axel
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, S-10691 Stockholm, Sweden.;Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden.;Ilia State Univ, Sch Nat Sci & Med, GE-0194 Tbilisi, Georgia.;Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.;Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA..
    Dynamo instabilities in plasmas with inhomogeneous chiral chemical potential2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 105, no 4, article id 043507Article in journal (Refereed)
    Abstract [en]

    We study the dynamics of magnetic fields in chiral magnetohydrodynamics, which takes into account the effects of an additional electric current related to the chiral magnetic effect in high-energy plasmas. We perform direct numerical simulations, considering weak seed magnetic fields and inhomogeneities of the chiral chemical potential mu(5) with a zero mean. We demonstrate that a small-scale chiral dynamo can occur in such plasmas if fluctuations of mu(5) are correlated on length scales that are much larger than the scale on which the dynamo growth rate reaches its maximum. Magnetic fluctuations grow by many orders of magnitude due to the small-scale chiral dynamo instability. Once the nonlinear backreaction of the generated magnetic field on fluctuations of mu(5) sets in, the ratio of these scales decreases and the dynamo saturates. When magnetic fluctuations grow sufficiently to drive turbulence via the Lorentz force before reaching maximum field strength, an additional mean-field dynamo phase is identified. The mean magnetic field grows on a scale that is larger than the integral scale of turbulence after the amplification of the fluctuating component saturates. The growth rate of the mean magnetic field is caused by a magnetic alpha effect that is proportional to the current helicity. With the onset of turbulence, the power spectrum of mu(5) develops a universal k(-1) scaling independently of its initial shape, while the magnetic energy spectrum approaches a k(-3) scaling.

  • 174.
    Sharma, Ramkishor
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. IUCAA, Post Bag 4,Pune Univ Campus, Pune 411007, Maharashtra, India.;.
    Constraining models of inflationary magnetogenesis with NANOGrav data2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 105, no 4, article id L041302Article in journal (Refereed)
    Abstract [en]

    Generation of magnetic field during inflation can explain its presence over a wide range of scales in the Universe. In [Sharma et al Phys. Rev. D 96, 083511 (2017)], we proposed a model to generate these fields during inflation. These fields have nonzero anisotropic stress which lead to the generation of a stochastic background of gravitational waves (GW) in the early universe. Here we show that for a scenario of magnetogenesis where reheating takes place around QCD epoch, this stochastic GW background lies in the 95% confidence region of the stochastic common spectrum process probed by NANOGrav collaboration. This is the case when the generated electromagnetic field (EM) energy density is 3%-10% of the background energy density at the end of reheating. For this case, the values of magnetic field strength B-0 similar to (0.7-1.4) x 10(-11) G and its coherence length similar to 3 kpc at the present epoch. These values are for the models in which EM fields are of nonhelical nature. For the helical nature of the fields, these values are B-0 similar to (2.1-3.8) x 10(-10) G and its coherence length similar to 90 kpc.

  • 175.
    Sharma, Ramkishor
    et al.
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Hannes Alfvens vag 12, S-10691 Stockholm, Sweden.;Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden..
    Brandenburg, Axel
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Hannes Alfvens vag 12, S-10691 Stockholm, Sweden.;Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden.;Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.;Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.;Ilia State Univ, Sch Nat Sci & Med, 3-5 Cholokashvili Ave, Tbilisi 0194, Georgia..
    Low frequency tail of gravitational wave spectra from hydromagnetic turbulence2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 106, no 10, article id 103536Article in journal (Refereed)
    Abstract [en]

    Hydrodynamic and magnetohydrodynamic turbulence in the early Universe can drive gravitational waves (GWs) and imprint their spectrum onto that of GWs, which might still be observable today. We study the production of the GW background from freely decaying magnetohydrodynamic turbulence from helical and nonhelical initial magnetic fields. To understand the produced GW spectra, we develop a simple model on the basis of the evolution of the magnetic stress tensor. We find that the GW spectra obtained in this model reproduce those obtained in numerical simulations if we consider the detailed time evolution of the low frequency tail of the stress spectrum from numerical simulations. We also show that the shapes of the produced GW frequency spectra are different for helical and nonhelical cases for the same initial magnetic energy spectra. Such differences can help distinguish helical and nonhelical initial magnetic fields from a polarized background of GWs-especially when the expected circular polarization cannot be detected directly.

  • 176. Singh, B.
    et al.
    Erni, W.
    Krusche, B.
    Steinacher, M.
    Walford, N.
    Liu, H.
    Liu, Z.
    Liu, B.
    Shen, X.
    Wang, C.
    Zhao, J.
    Albrecht, M.
    Erlen, T.
    Fink, M.
    Heinsius, F. H.
    Held, T.
    Holtmann, T.
    Jasper, S.
    Keshk, I.
    Koch, H.
    Kopf, B.
    Kuhlmann, M.
    Kuemmel, M.
    Leiber, S.
    Mikirtychyants, M.
    Musiol, P.
    Mustafa, A.
    Pelizaeus, M.
    Pychy, J.
    Richter, M.
    Schnier, C.
    Schroeder, T.
    Sowa, C.
    Steinke, M.
    Triffterer, T.
    Wiedner, U.
    Ball, M.
    Beck, R.
    Hammann, C.
    Ketzer, B.
    Kube, M.
    Mahlberg, P.
    Rossbach, M.
    Schmidt, C.
    Schmitz, R.
    Thoma, U.
    Urban, M.
    Walther, D.
    Wendel, C.
    Wilson, A.
    Bianconi, A.
    Bragadireanu, M.
    Caprini, M.
    Pantea, D.
    Patel, B.
    Czyzycki, W.
    Domagala, M.
    Filo, G.
    Jaworowski, J.
    Krawczyk, M.
    Lisowski, E.
    Lisowski, F.
    Michalek, M.
    Poznanski, P.
    Plazek, J.
    Korcyl, K.
    Kozela, A.
    Kulessa, P.
    Lebiedowicz, P.
    Pysz, K.
    Schaefer, W.
    Szczurek, A.
    Fiutowski, T.
    Idzik, M.
    Mindur, B.
    Przyborowski, D.
    Swientek, K.
    Biernat, J.
    Kamys, B.
    Kistryn, S.
    Korcyl, G.
    Krzemien, W.
    Magiera, A.
    Moskal, P.
    Pyszniak, A.
    Rudy, Z.
    Salabura, P.
    Smyrski, J.
    Strzempek, P.
    Wronska, A.
    Augustin, I.
    Boehm, R.
    Lehmann, I.
    Marinescu, D. Nicmorus
    Schmitt, L.
    Varentsov, V.
    Al-Turany, M.
    Belias, A.
    Deppe, H.
    Veis, N. Divani
    Dzhygadlo, R.
    Ehret, A.
    Flemming, H.
    Gerhardt, A.
    Goetzen, K.
    Gromliuk, A.
    Gruber, L.
    Karabowicz, R.
    Kliemt, R.
    Krebs, M.
    Kurilla, U.
    Lehmann, D.
    Loechner, S.
    Luehning, J.
    Lynen, U.
    Orth, H.
    Patsyuk, M.
    Peters, K.
    Saito, T.
    Schepers, G.
    Schmidt, C. J.
    Schwarz, C.
    Schwiening, J.
    Taeschner, A.
    Traxler, M.
    Ugur, C.
    Voss, B.
    Wieczorek, P.
    Wilms, A.
    Zuehlsdorf, M.
    Abazov, V.
    Alexeev, G.
    Arefiev, V. A.
    Astakhov, V.
    Barabanov, M. Yu.
    Batyunya, B. V.
    Davydov, Y.
    Dodokhov, V. Kh.
    Efremov, A.
    Fechtchenko, A.
    Fedunov, A. G.
    Galoyan, A.
    Grigoryan, S.
    Koshurnikov, E. K.
    Lobanov, Y. Yu.
    Lobanov, V. I.
    Makarov, A. F.
    Malinina, L. V.
    Malyshev, V.
    Olshevskiy, A. G.
    Perevalova, E.
    Piskun, A. A.
    Pocheptsov, T.
    Pontecorvo, G.
    Rodionov, V.
    Rogov, Y.
    Salmin, R.
    Samartsev, A.
    Sapozhnikov, M. G.
    Shabratova, G.
    Skachkov, N. B.
    Skachkova, A. N.
    Strokovsky, E. A.
    Suleimanov, M.
    Teshev, R.
    Tokmenin, V.
    Uzhinsky, V.
    Vodopianov, A.
    Zaporozhets, S. A.
    Zhuravlev, N. I.
    Zinchenko, A.
    Zorin, A. G.
    Branford, D.
    Glazier, D.
    Watts, D.
    Boehm, M.
    Britting, A.
    Eyrich, W.
    Lehmann, A.
    Pfaffinger, M.
    Uhlig, F.
    Dobbs, S.
    Seth, K.
    Tomaradze, A.
    Xiao, T.
    Bettoni, D.
    Carassiti, V.
    Ramusino, A. Cotta
    Dalpiaz, P.
    Drago, A.
    Fioravanti, E.
    Garzia, I.
    Savrie, M.
    Akishina, V.
    Kisel, I.
    Kozlov, G.
    Pugach, M.
    Zyzak, M.
    Gianotti, P.
    Guaraldo, C.
    Lucherini, V.
    Bersani, A.
    Bracco, G.
    Macri, M.
    Parodi, R. F.
    Biguenko, K.
    Brinkmann, K. T.
    Di Pietro, V.
    Diehl, S.
    Dormenev, V.
    Drexler, P.
    Doern, M.
    Etzelmller, E.
    Galuska, M.
    Gutz, E.
    Hahn, C.
    Hayrapetyan, A.
    Kesselkaul, M.
    Koehn, W.
    Kuske, T.
    Lange, J. S.
    Liang, Y.
    Metag, V.
    Moritz, M.
    Nanova, M.
    Nazarenko, S.
    Novotny, R.
    Quagli, T.
    Reiter, S.
    Riccardi, A.
    Rieke, J.
    Rosenbaum, C.
    Schmidt, M.
    Schnell, R.
    Stenzel, H.
    Thoering, U.
    Ullrich, T.
    Wagner, M. N.
    Wasem, T.
    Wohlfahrt, B.
    Zaunick, H. G.
    Tomasi-Gustafsson, E.
    Ireland, D.
    Rosner, G.
    Seitz, B.
    Deepak, P. N.
    Kulkarni, A.
    Apostolou, A.
    Babai, M.
    Kavatsyuk, M.
    Lemmens, P. J.
    Lindemulder, M.
    Loehner, H.
    Messchendorp, J.
    Schakel, P.
    Smit, H.
    Tiemens, M.
    Van derweele, J. C.
    Veenstra, R.
    Vejdani, S.
    Dutta, K.
    Kalita, K.
    Kumar, A.
    Roy, A.
    Sohlbach, H.
    Bai, M.
    Bianchi, L.
    Buescher, M.
    Cao, L.
    Cebulla, A.
    Dosdall, R.
    Gillitzer, A.
    Goldenbaum, F.
    Grunwald, D.
    Herten, A.
    Hu, Q.
    Kemmerling, G.
    Kleines, H.
    Lai, A.
    Lehrach, A.
    Nellen, R.
    Ohm, H.
    Orfanitski, S.
    Prasuhn, D.
    Prencipe, E.
    Puetz, J.
    Ritman, J.
    Schadmand, S.
    Sefzick, T.
    Serdyuk, V.
    Sterzenbach, G.
    Stockmanns, T.
    Wintz, P.
    Wuestner, P.
    Xu, H.
    Zambanini, A.
    Li, S.
    Li, Z.
    Sun, Z.
    Rigato, V.
    Isaksson, L.
    Achenbach, P.
    Corell, O.
    Denig, A.
    Distler, M.
    Hoek, M.
    Karavdina, A.
    Lauth, W.
    Merkel, H.
    Mueller, U.
    Pochodzalla, J.
    Sanchez, S.
    Schlimme, S.
    Sfienti, C.
    Thiel, M.
    Ahmadi, H.
    Ahmed, S.
    Bleser, S.
    Capozza, L.
    Cardinali, M.
    Dbeyssi, A.
    Deiseroth, M.
    Feldbauer, F.
    Fritsch, M.
    Froerllich, B.
    Kang, D.
    Khaneft, D.
    Klasen, R.
    Leithoff, H. H.
    Lin, D.
    Maas, F.
    Maldaner, S.
    Martinez, M.
    Michel, M.
    Mora Esp, M. C.
    Morales, C. Morales
    Motzko, C.
    Nerling, F.
    Noll, O.
    Pfloeger, S.
    Pitka, A.
    Pineiro, D. Rodriguez
    Sanchez-Lorente, A.
    Steinen, M.
    Valente, R.
    Weber, T.
    Zambrana, M.
    Zimmermann, I.
    Fedorov, A.
    Korjik, M.
    Missevitch, O.
    Boukharov, A.
    Malyshev, O.
    Marishev, I.
    Balanutsa, V.
    Balanutsa, P.
    Chernetsky, V.
    Demekhin, A.
    Dolgolenko, A.
    Fedorets, P.
    Gerasimov, A.
    Goryachev, V.
    Chandratre, V.
    Datar, V.
    Dutta, D.
    Jha, V.
    Kumawat, H.
    Mohanty, A. K.
    Parmar, A.
    Roy, B.
    Sonika, G.
    Fritzsch, C.
    Grieser, S.
    Hergemoeller, A. K.
    Hetz, B.
    Huesken, N.
    Khoukaz, A.
    Wessels, J. P.
    Khosonthongkee, K.
    Kobdaj, C.
    Limphirat, A.
    Srisawad, P.
    Yan, Y.
    Barnyakov, A. Yu.
    Barnyakov, M.
    Beloborodov, K.
    Blinov, V. E.
    Bobrovnikov, V. S.
    Kuyanov, I. A.
    Martin, K.
    Onuchin, A. P.
    Serednyakov, S.
    Sokolov, A.
    Tikhonov, Y.
    Blinov, A. E.
    Kononov, S.
    Kravchenko, E. A.
    Atomssa, E.
    Kunne, R.
    Ma, B.
    Marchand, D.
    Ramstein, B.
    van de Wiele, J.
    Wang, Y.
    Boca, G.
    Costanza, S.
    Genova, P.
    Montagna, P.
    Rotondi, A.
    Abramov, V.
    Belikov, N.
    Bukreeva, S.
    Davidenko, A.
    Derevschikov, A.
    Goncharenko, Y.
    Grishin, V.
    Kachanov, V.
    Kormilitsin, V.
    Levin, A.
    Melnik, Y.
    Minaev, N.
    Mochalov, V.
    Morozov, D.
    Nogach, L.
    Poslavskiy, S.
    Ryazantsev, A.
    Ryzhikov, S.
    Semenov, P.
    Shein, I.
    Uzunian, A.
    Vasiliev, A.
    Yakutin, A.
    Roy, U.
    Yabsley, B.
    Belostotski, S.
    Gavrilov, G.
    Izotov, A.
    Manaenkov, S.
    Miklukho, O.
    Veretennikov, D.
    Zhdanov, A.
    Bäck, Torbjörn
    KTH, School of Engineering Sciences (SCI), Physics, Nuclear Physics.
    Cederwall, Bo
    KTH, School of Engineering Sciences (SCI), Physics, Nuclear Physics.
    Makonyi, K.
    Preston, M.
    Tegner, P. E.
    Woelbing, D.
    Rai, A. K.
    Godre, S.
    Calvo, D.
    Coli, S.
    De Remigis, P.
    Filippi, A.
    Giraudo, G.
    Lusso, S.
    Mazza, G.
    Mignone, M.
    Rivetti, A.
    Wheadon, R.
    Amoroso, A.
    Bussa, M. P.
    Busso, L.
    De Mori, F.
    Destefanis, M.
    Fava, L.
    Ferrero, L.
    Greco, M.
    Hu, J.
    Lavezzi, L.
    Maggiora, M.
    Maniscalco, G.
    Marcello, S.
    Sosio, S.
    Spataro, S.
    Balestra, F.
    Iazzi, F.
    Introzzi, R.
    Lavagno, A.
    Olave, J.
    Birsa, R.
    Bradamante, F.
    Bressan, A.
    Martin, A.
    Calen, H.
    Andersson, W. Ikegami
    Johansson, T.
    Kupsc, A.
    Marciniewski, P.
    Papenbrock, M.
    Pettersson, J.
    Schoenning, K.
    Wolke, M.
    Galnander, B.
    Diaz, J.
    Chackara, V. Pothodi
    Chlopik, A.
    Kesik, G.
    Melnychuk, D.
    Slowinski, B.
    Trzcinski, A.
    Wojciechowski, M.
    Wronka, S.
    Zwieglinski, B.
    Buehler, P.
    Marton, J.
    Steinschaden, D.
    Suzuki, K.
    Widmann, E.
    Zmeskal, J.
    Semenov-Tian-Shansky, K. M.
    Feasibility study for the measurement of pi N transition distribution amplitudes at (P)over-barANDA in (P)over-barp -> J/psi pi(0)2017In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 95, no 3, article id 032003Article in journal (Refereed)
    Abstract [en]

    The exclusive charmonium production process in (P) over barp annihilation with an associated pi 0 meson (p) over barp -> J/psi pi(0) is studied in the framework of QCD collinear factorization. The feasibility of measuring this reaction through the J/psi -> e(+) e(-) decay channel with the AntiProton ANnihilation at DArmstadt ((P) over bar ANDA) experiment is investigated. Simulations on signal reconstruction efficiency as well as the background rejection from various sources including the (P) over barp -> pi(+)pi(-)pi(0) and (p) over barp -> J/psi pi(0)pi(0) reactions are performed with PANDAROOT, the simulation and analysis software framework of the (P) over bar ANDA experiment. It is shown that the measurement can be done at (P) over bar ANDA with significant constraining power under the assumption of an integrated luminosity attainable in four to five months of data taking at the maximum design luminosity.

  • 177.
    Smail, R. E.
    et al.
    CSSM, Department of Physics, University of Adelaide, Adelaide, South Australia 5005, Australia.
    Batelaan, M.
    CSSM, Department of Physics, University of Adelaide, Adelaide, South Australia 5005, Australia.
    Horsley, R.
    School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom.
    Nakamura, Y.
    RIKEN Center for Computational Science, Kobe, Hyogo 650-0047, Japan.
    Perlt, H.
    Institut für Theoretische Physik, Universität Leipzig, 04103 Leipzig, Germany.
    Pleiter, Dirk
    KTH, School of Electrical Engineering and Computer Science (EECS), Computer Science, Computational Science and Technology (CST). KTH, School of Electrical Engineering and Computer Science (EECS), Centres, Centre for High Performance Computing, PDC.
    Rakow, P. E.L.
    Theoretical Physics Division, Department of Mathematical Sciences, University of Liverpool, Liverpool L69 3BX, United Kingdom.
    Schierholz, G.
    Deutsches Elektronen-Synchrotron DESY, Notkestraße 85, 22607 Hamburg, Germany.
    Stüben, H.
    Universität Hamburg, Regionales Rechenzentrum, 20146 Hamburg, Germany.
    Young, R. D.
    CSSM, Department of Physics, University of Adelaide, Adelaide, South Australia 5005, Australia; Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
    Zanotti, J. M.
    CSSM, Department of Physics, University of Adelaide, Adelaide, South Australia 5005, Australia.
    Constraining beyond the standard model nucleon isovector charges2023In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 108, no 9, article id 094511Article in journal (Refereed)
    Abstract [en]

    At the TeV scale, low-energy precision observations of neutron characteristics provide unique probes of novel physics. Precision studies of neutron decay observables are susceptible to beyond the Standard Model (BSM) tensor and scalar interactions, while the neutron electric dipole moment, dn, also has high sensitivity to new BSM CP-violating interactions. To fully utilize the potential of future experimental neutron physics programs, matrix elements of appropriate low-energy effective operators within neutron states must be precisely calculated. We present results from the QCDSF/UKQCD/CSSM Collaboration for the isovector charges gT, gA and gS of the nucleon, ς and Ξ baryons using lattice QCD methods and the Feynman-Hellmann theorem. We use a flavor symmetry breaking method to systematically approach the physical quark mass using ensembles that span five lattice spacings and multiple volumes. We extend this existing flavor-breaking expansion to also account for lattice spacing and finite volume effects in order to quantify all systematic uncertainties. Our final estimates of the nucleon isovector charges are gT=1.010(21)stat(12)sys,gA=1.253(63)stat(41)sys and gS=1.08(21)stat(03)sys renormalized, where appropriate, at μ=2 GeV in the MS¯ scheme.

  • 178.
    Soumya, C.
    et al.
    Inst Phys, Sachivalaya Marg, Bhubaneswar 751005, India..
    Ghosh, Monojit
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Raut, Sushant K.
    Inst for Basic Sci Korea, Ctr Theoret Phys Universe, Daejeon 34051, South Korea.;Korea Adv Inst Sci & Technol, Dept Phys, Daejeon 34141, South Korea..
    Sinha, Nita
    Inst Math Sci, Chennai 600113, Tamil Nadu, India..
    Mehta, Poonam
    Jawaharlal Nehru Univ, Sch Phys Sci, New Delhi 110067, India..
    Probing muonic charged current nonstandard interactions at decay-at-rest facilities in conjunction with T2HK2020In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 101, no 5, article id 055009Article in journal (Refereed)
    Abstract [en]

    The muon decay-at-rest (mu-DAR) facility provides us with an ideal platform to probe purely muonic charged-current nonstandard neutrino interactions (NSIs). We propose to probe this class of NSI effects using antineutrinos from a mu-DAR source in conjunction with neutrinos from the future Tokai to Kamioka superbeam experiment with megaton hyper Kamiokande detector (T2HK). Even though muonic NSIs are absent in neutrino production at T2HK, we show that our proposed hybrid setup comprising mu-DAR and T2HK helps in alleviating the parameter degeneracies that can arise in data. Analytic considerations reveal that the oscillation probability is most sensitive to the NSI parameter in the mu-e sector. For this parameter, we show that the mu-DAR setup can improve on the existing bounds down to around 0.01, especially when the data are combined with neutrino data from T2HK experiment due to the lifting of parameter degeneracies. The high precision with which mu-DAR can measure delta(CP) is shown to be robust even in the presence of the considered NSIs. Finally, we show that the combination of mu-DAR along with T2HK can also be used to put mild constraints on the NSI phase in the vicinity of the maximal CP-violating value, for the chosen benchmark value of epsilon(mu e)(mu e) = 0.01.

  • 179.
    Vagnozzi, Sunny
    et al.
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, Alballova Univ Ctr, Roslagstullsbacken 21A, SE-10691 Stockholm, SwedenStockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.;Univ Cambridge, Kavh Inst Cosmol KICC, Madingley Rd, Cambridge CB3 0HA, England.;Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England..
    Visinelli, Luca
    Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.;Uppsala Univ, Dept Phys & Astron, Lagerhyddsvagen 1, S-75120 Uppsala, Sweden.;Univ Amsterdam, Gravitat Astroparticle Phys Amsterdam GRAPPA, Inst Theoret Phys Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.;Univ Amsterdam, Delta Inst Theoret Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Hunting for extra dimensions in the shadow of M872019In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 100, no 2, article id 024020Article in journal (Refereed)
    Abstract [en]

    The Event Horizon Telescope has recently provided the first image of the dark shadow around the supermassive black hole M87*. The observation of a highly circular shadow provides strong limits on deviations of M87*'s quadrupole moment from the Kerr value. We show that the absence of such a deviation can be used to constrain the physics of extra dimensions of spacetime. Focusing on the Randall-Sundrum AdS(5) brane-world scenario, we show that the observation of M87*'s dark shadow sets the limit l less than or similar to 170 AU, where l is the AdS(5) curvature radius. This limit is among the first quantitative constraints on exotic physics obtained from the extraordinary first ever image of the dark shadow of a black hole.

  • 180.
    Vescovi, Edoardo
    Nordita SU ; Stockholm University, Roslagstullsbacken 23, Stockholm.
    Four-point function of determinant operators in N=4 SYM2021In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 103, no 10, article id 106001Article in journal (Refereed)
    Abstract [en]

    We calculate the four-point function of 1/2-BPS (Bogomolnyi-Prasad-Sommerfield) determinant operators in N=4 SYM (super Yang-Mills) at next-to-leading order at weak coupling. We use two complementary methods recently developed for a class of determinant three-point functions: one is based on Feynman diagrams and it extracts perturbative data at finite N, while the other one expresses a generic correlator of determinants as the zero-dimensional integral over an auxiliary matrix field. We generalize the latter approach to calculate one-loop corrections and we solve the four-point function in a semiclassical approach at large N. The results allow us to comment on the order of the phase transition that the four-point function is expected to exhibit in an exact integrability-based description.

  • 181.
    Visinelli, Luca
    Nordita SU.
    Light axion-like dark matter must be present during inflation2017In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 96, no 2, article id 023013Article in journal (Refereed)
    Abstract [en]

    Axion-like particles (ALPs) might constitute the totality of the cold dark matter (CDM) observed. The parameter space of ALPs depends on the mass of the particle m and on the energy scale of inflation HI, the latter being bound by the nondetection of primordial gravitational waves. We show that the bound on HI implies the existence of a mass scale mχ=10 neV-0.5 peV, depending on the ALP susceptibility χ, such that the energy density of ALPs of mass smaller than mχ is too low to explain the present CDM budget, if the ALP field has originated after the end of inflation. This bound affects ultra-light axions (ULAs), which have recently regained popularity as CDM candidates. Light (m<mχ) ALPs can then be CDM candidates only if the ALP field has already originated during the inflationary period, in which case the parameter space is constrained by the nondetection of axion isocurvature fluctuations. We comment on the effects on these bounds from additional physics beyond the standard model, besides ALPs.

  • 182.
    Visinelli, Luca
    et al.
    Nordita SU.
    Bolis, Nadia
    Fyzikalni Ustav Akad CR, Cent European Inst Cosmol & Fundamental Phys CEIC, Na Slovance 1999-2, CZ-18221 Prague 8, Czech Republic..
    Vagnozzi, Sunny
    Stockholm Univ, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, AlbaNova Univ Ctr, Roslagstullbacken 21A, SE-10691 Stockholm, Sweden..
    Brane-world extra dimensions in light of GW1708172018In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 97, no 6, article id 064039Article in journal (Refereed)
    Abstract [en]

    The search for extra dimensions is a challenging endeavor to probe physics beyond the Standard Model. The joint detection of gravitational waves (GW) and electromagnetic (EM) signals from the merging of a binary system of compact objects like neutron stars can help constrain the geometry of extra dimensions beyond our 3 + 1 spacetime ones. A theoretically well-motivated possibility is that our observable Universe is a 3 + 1-dimensional hypersurface, or brane, embedded in a higher 4 + 1-dimensional antide Sitter (AdS(5)) spacetime, in which gravity is the only force which propagates through the infinite bulk space, while other forces are confined to the brane. In these types of brane-world models, GW and EM signals between two points on the brane would, in general, travel different paths. This would result in a time lag between the detection of GW and EM signals emitted simultaneously from the same source. We consider the recent near-simultaneous detection of the GW event GW170817 from the LIGO/Virgo collaboration, and its EM counterpart, the short gamma-ray burst GRB170817A detected by the Fermi Gamma-ray Burst Monitor and the International Gamma-Ray Astrophysics Laboratory Anti-Coincidence Shield spectrometer. Assuming the standard.-cold dark matter scenario and performing a likelihood analysis which takes into account astrophysical uncertainties associated to the measured time lag, we set an upper limit of l less than or similar to 0.535 Mpc at 68% confidence level on the AdS(5) radius of curvature l. Although the bound is not competitive with current Solar System constraints, it is the first time that data from a multimessenger GW-EM measurement is used to constrain extra-dimensional models. Thus, our work provides a proof of principle for the possibility of using multimessenger astronomy for probing the geometry of our space-time.

  • 183.
    Visinelli, Luca
    et al.
    Nordita SU.
    Redondo, Javier
    Univ Zaragoza, Dept Fis Teor, C Pedro Cerbuna 12, E-50009 Zaragoza, Spain.;Max Planck Inst Phys & Astrophys, Foehringer Ring 6, D-80805 Munich, Germany..
    Axion miniclusters in modified cosmological histories2020In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 101, no 2, article id 023008Article in journal (Refereed)
    Abstract [en]

    If the symmetry breaking leading to the origin of the axion dark matter field occurs after the end of inflation and is never restored, then overdensities in the axion field collapse to form dense objects known in the literature as axion miniclusters. The estimates of the typical minicluster mass and radius strongly depend on the details of the cosmology at which the onset of axion oscillations begin. In this work we study the properties and phenomenology of miniclusters in alternative cosmological histories and find that they can change by many orders of magnitude. Our findings have direct implications on current and future experimental searches and, in the case of discovery, could be used to learn something about the universe expansion prior to big bang nucleosynthesis.

  • 184.
    Visinelli, Luca
    et al.
    Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Roslagstullsbacken 21A, SE-10691 Stockholm, Sweden..;Uppsala Univ, Dept Phys & Astron, Lagerhyddsvagen 1, S-75120 Uppsala, Sweden..
    Vagnozzi, Sunny
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Roslagstullsbacken 21A, SE-10691 Stockholm, Sweden.
    Cosmological window onto the string axiverse and the supersymmetry breaking scale2019In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 99, no 6, article id 063517Article in journal (Refereed)
    Abstract [en]

    In the simplest picture, the masses of string axions populating the axiverse depend on two parameters: the supersymmetry-breaking scale M-susy and the action S of the string instantons responsible for breaking the axion shift symmetry. In this work, we explore whether cosmological data can be used to probe these two parameters. Adopting string-inspired flat priors on log(10) M-susy and S and imposing that M-susy be sub-Planckian, we find S = 198 +/- 28. These bounds suggest that cosmological data complemented with string-inspired priors select a quite narrow axion mass range within the axiverse, log(10)(m(a)/eV) = -21.5(-2.3)(+1.3). We find that M-susy remains unconstrained due to a fundamental parameter degeneracy with S. We explore the significant impact of other choices of priors on the results, and we comment on similar findings in recent previous literature.

  • 185.
    Westernacher-Schneider, John Ryan
    et al.
    Univ Arizona, Dept Astron Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.;Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.;Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada.;Univ Copenhagen, Niels Bohr Inst, DARK, Lyngbyvej 2, DK-2100 Copenhagen, Denmark..
    O'Connor, Evan
    Stockholm Univ, Dept Astron, AlbaNova, S-10961 Stockholm, Sweden.;Stockholm Univ, Oskar Klein Ctr, AlbaNova, S-10961 Stockholm, Sweden..
    O'Sullivan, Erin
    Stockholm Univ, Oskar Klein Ctr, AlbaNova, S-10961 Stockholm, Sweden.;Stockholm Univ, Dept Phys, AlbaNova, S-10961 Stockholm, Sweden..
    Tamborra, Irene
    Univ Copenhagen, Niels Bohr Inst, DARK, Lyngbyvej 2, DK-2100 Copenhagen, Denmark.;Univ Copenhagen, Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark..
    Wu, Meng-Ru
    Univ Copenhagen, Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark.;Acad Sinica, Inst Phys, Taipei 11529, Taiwan.;Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan..
    Couch, Sean M.
    Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.;Michigan State Univ, Dept Computat Math Sci & Engn, E Lansing, MI 48824 USA.;Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA.;Michigan State Univ, Ctr Evolut Elements, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA..
    Malmenbeck, Felix
    KTH, School of Engineering Sciences (SCI), Physics.
    Multimessenger asteroseismology of core-collapse supernovae2019In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 100, no 12, article id 123009Article in journal (Refereed)
    Abstract [en]

    We investigate correlated gravitational wave and neutrino signals from rotating core-collapse supernovae with simulations. Using an improved mode identification procedure based on mode function matching, we show that a linear quadrupolar mode of the core produces a dual imprint on gravitational waves and neutrinos in the early post-bounce phase of the supernova. The angular harmonics of the neutrino emission are consistent with the mode energy around the neutrinospheres, which points to a mechanism for the imprint on neutrinos. Thus, neutrinos carry information about the mode amplitude in the outer region of the core, whereas gravitational waves probe deeper in. We also find that the best-fit mode function has a frequency bounded above by similar to 420 Hz, and yet the mode's frequency in our simulations is similar to 15% higher, due to the use of Newtonian hydrodynamics and a widely used pseudo-Newtonian gravity approximation. This overestimation is particularly important for the analysis of gravitational wave detectability and asteroseismology, pointing to limitations of pseudo-Newtonian approaches for these purposes, possibly even resulting in excitation of incorrect modes. In addition, mode frequency matching (as opposed to mode function matching) could be resulting in mode misidentification in recent work. Lastly, we evaluate the prospects of a multimessenger detection of the mode using current technology. The detection of the imprint on neutrinos is most challenging, with a maximum detection distance of similar to 1 kpc using the IceCube Neutrino Observatory. The maximum distance for detecting the complementary gravitational wave imprint is similar to 5 kpc using Advanced LIGO at design sensitivity.

  • 186.
    Winkler, Martin Wolfgang
    Nordita SU.
    Decay and detection of a light scalar boson mixing with the Higgs boson2019In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 99, no 1, article id 015018Article in journal (Refereed)
    Abstract [en]

    The simplest extension of the standard model consists in adding one singlet scalar field which mixes with the Higgs boson. O(GeV) masses of the new scalar carry strong motivation from relaxion, dark matter and inflation models. The decay of a GeV scalar is, however, notoriously difficult to address since, at this mass scale, the chiral expansion breaks down and perturbative QCD does not apply. Existing estimates of the GeV scalar decay rate disagree by several orders of magnitude. In this work, we perform a new dispersive analysis in order to strongly reduce these uncertainties and to address discrepancies in earlier results. We will update existing limits on light scalars and future experimental sensitivities which are in some cases strongly affected by the new-found decay rates. The meson form factors provided in this work, can be used to generalize our findings to non-universally coupled light scalars.

  • 187. Winkler, Martin Wolfgang
    et al.
    Freese, Katherine
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.
    Power spectrum of density perturbations in chain inflation2021In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 103, no 4, article id 043511Article in journal (Refereed)
    Abstract [en]

    Chain inflation is an alternative to slow roll inflation in which the Universe undergoes a series of transitions between different vacua. The density perturbations (studied in this paper) are seeded by the probabilistic nature of tunneling rather than quantum fluctuations of the inflaton. We find the scalar power spectrum of chain inflation and show that it is fully consistent with a Lambda CDM cosmology. In agreement with some of the previous literature (and disagreement with others), we show that 10(4) phase transitions per e-fold are required in order to agree with the amplitude of cosmic microwave background anisotropies within the observed range of scales. Interestingly, the amplitude of perturbations constrains chain inflation to a regime of highly unstable de Sitter spaces, which may be favorable from a quantum gravity perspective since the swampland conjecture on trans-Planckian censorship is automatically satisfied. We provide new analytic estimates for the bounce action and the tunneling rate in periodic potentials which replace the thin-wall approximation in the regime of fast tunneling. Finally, we study model implications and derive an upper limit of similar to 10(10) GeV on the axion decay constant in viable chain inflation with axions.

  • 188.
    Witte, Samuel J.
    et al.
    GRAPPA Inst, Inst Theoret Phys Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.;Univ Amsterdam, Delta Inst Theoret Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Baum, Sebastian
    Stanford Univ, Stanford Inst Theoret Phys, Dept Phys, Stanford, CA 94305 USA..
    Lawson, Matthew
    Stockholm Univ, Oskar Klein Ctr, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden..
    Marsh, M. C. David
    The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, SE-10691, Sweden.
    Millar, Alexander J.
    Stockholm Univ, Oskar Klein Ctr, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.;Nordita SU;Stockholm Univ, Roslagstullsbacken 23, S-10691 Stockholm, Sweden.;Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA..
    Salinas, Gustavo
    Stockholm Univ, Oskar Klein Ctr, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden..
    Transient radio lines from axion miniclusters and axion stars2023In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 107, no 6, article id 063013Article in journal (Refereed)
    Abstract [en]

    Gravitationally bound clumps of dark matter axions in the form of "miniclusters" or even denser "axion stars" can generate strong radio signals through axion-photon conversion when encountering highly magnetized neutron star magnetospheres. We systematically study encounters of axion clumps with neutron stars and characterize the axion infall, conversion and the subsequent propagation of the photons. We show that the high density and low escape velocity of the axion clumps lead to strong, narrow, and temporally characteristic transient radio lines with an expected duration varying from seconds to months. Our work comprises the first end-to-end modeling pipeline capable of characterizing the radio signal generated during these transient encounters, quantifying the typical brightness, anisotropy, spectral width, and temporal evolution of the radio flux. The methods developed here may prove essential in developing dedicated radio searches for transient radio lines arising from miniclusters and axion stars.

  • 189.
    Wu, Youjia
    et al.
    Univ Michigan, Leinweber Ctr Theoret Phys, Dept Phys, Ann Arbor, MI 48109 USA..
    Baum, Sebastian
    Stanford Univ, Stanford Inst Theoret Phys, Stanford, CA 94305 USA..
    Freese, Katherine
    KTH, Centres, Nordic Institute for Theoretical Physics NORDITA. Univ Texas, Dept Phys, Austin, TX 78712 USA.;Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, Dept Phys, AlbaNova, Roslagstullsbacken 21, S-10691 Stockholm, Sweden.;Stockholm Univ, .
    Visinelli, Luca
    Tsung Dao Lee Inst TDLI, 520 Shengrong Rd, Shanghai 201210, Peoples R China.;Shanghai Jiao Tong Univ, Sch Phys & Astron, 800 Dongchuan Rd, Shanghai 200240, Peoples R China..
    Yu, Hai -Bo
    Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA..
    Dark stars powered by self-interacting dark matter2022In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 106, no 4, article id 043028Article in journal (Refereed)
    Abstract [en]

    Dark matter annihilation might power the first luminous stars in the Universe. These types of stars, known as dark stars, could form in (10(6)-10(8)) M-? protohalos at redshifts z similar to 20, and they could be much more luminous and larger in size than ordinary stars powered by nuclear fusion. We investigate the formation of dark stars in the self-interacting dark matter (SIDM) scenario. We present a concrete particle physics model of SIDM that can simultaneously give rise to the observed dark matter density, satisfy constraints from astrophysical and terrestrial searches, and address the various small-scale problems of collisionless dark matter via the self-interactions. In this model, the power from dark matter annihilation is deposited in the baryonic gas in environments where dark stars could form. We further study the evolution of SIDM density profiles in the protohalos at z similar to 20. As the baryon cloud collapses due to the various cooling processes, the deepening gravitational potential can speed up gravothermal evolution of the SIDM halo, yielding sufficiently high dark matter densities for dark stars to form. We find that SIDM-powered dark stars can have similar properties, such as their luminosity and size, as dark stars predicted in collisionless dark matter models.

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