002722392 001__ 2722392
002722392 005__ 20240501043213.0
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002722392 0247_ $$2DOI$$9bibmatch$$a10.1007/JHEP12(2020)075
002722392 037__ $$9arXiv$$aarXiv:2006.04820$$chep-ph
002722392 037__ $$9arXiv:reportnumber$$aDESY-19-234
002722392 037__ $$9arXiv:reportnumber$$aCERN-TH-2020-091
002722392 037__ $$9arXiv:reportnumber$$aINR-TH-2020-001
002722392 035__ $$9arXiv$$aoai:arXiv.org:2006.04820
002722392 035__ $$9Inspire$$aoai:inspirehep.net:1800405$$d2024-04-30T21:47:35Z$$h2024-05-01T02:00:12Z$$mmarcxml$$ttrue$$uhttps://inspirehep.net/api/oai2d
002722392 035__ $$9Inspire$$a1800405
002722392 041__ $$aeng
002722392 100__ $$aSibiryakov, Sergey$$msergey.sibiryakov@cern.ch$$tGRID:grid.425051.7$$tGRID:grid.9132.9$$tGRID:grid.5333.6$$uMoscow, INR$$uCERN$$uEPFL, Lausanne, LPTP$$vInstitute for Nuclear Research, Russian Academy of Sciences, 60th October Anniversary Prospect, 7a, 117312 Moscow, Russia$$vTheoretical Physics Department, CERN, Geneva, Switzerland$$vInstitute of Physics, LPTP, Ecole Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, Switzerland
002722392 245__ $$9arXiv$$aBBN constraints on universally-coupled ultralight scalar dark matter
002722392 269__ $$c2020-06-08
002722392 260__ $$c2020
002722392 300__ $$a34 p
002722392 500__ $$9arXiv$$a23 pages + appendices and bibliography, 6 figures, v2: typos
corrected, expanded discussion around eq. 4.5, published version
002722392 520__ $$9arXiv$$aUltralight scalar dark matter can interact with all massive Standard Model particles through a universal coupling. Such a coupling modifies the Standard Model particle masses and affects the dynamics of Big Bang Nucleosynthesis. We model the cosmological evolution of the dark matter, taking into account the modifications of the scalar mass by the environment as well as the full dynamics of Big Bang Nucleosynthesis. We find that precision measurements of the helium-4 abundance set stringent constraints on the available parameter space, and that these constraints are strongly affected by both the dark matter environmental mass and the dynamics of the neutron freeze-out. Furthermore, we perform the analysis in both the Einstein and Jordan frames, the latter of which allows us to implement the model into numerical Big Bang Nucleosynthesis codes and analyze additional light elements. The numerical analysis shows that the constraint from helium-4 dominates over deuterium, and that the effect on lithium is insufficient to solve the lithium problem. Comparing to several other probes, we find that Big Bang Nucleosynthesis sets the strongest constraints for the majority of the parameter space.
002722392 540__ $$3preprint$$aCC-BY-4.0$$uhttp://creativecommons.org/licenses/by/4.0/
002722392 540__ $$3publication$$aCC-BY-4.0$$bSpringer$$fSCOAP3$$uhttp://creativecommons.org/licenses/by/4.0/
002722392 542__ $$3publication$$f© The Authors
002722392 595__ $$aCERN-TH
002722392 65017 $$2arXiv$$aastro-ph.CO
002722392 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
002722392 65017 $$2arXiv$$ahep-ph
002722392 65017 $$2SzGeCERN$$aParticle Physics - Phenomenology
002722392 690C_ $$aCERN
002722392 690C_ $$aARTICLE
002722392 700__ $$aSørensen, Philip$$jORCID:0000-0003-4780-9088$$mphilip.soerensen@desy.de$$tGRID:grid.9026.d$$tGRID:grid.7683.a$$uHamburg U., Inst. Theor. Phys. II$$uDESY$$vII. Institute of Theoretical Physics, Universität Hamburg, 22761 Hamburg, Germany$$vDESY, Notkestraße 85, 22607 Hamburg, Germany
002722392 700__ $$aYu, Tien-Tien$$jORCID:0000-0003-4708-809X$$mtientien@uoregon.edu$$tGRID:grid.170202.6$$uOregon U.$$vDepartment of Physics, Institute for Fundamental Science, University of Oregon, 97403 Eugene, USA
002722392 773__ $$c075$$pJHEP$$v2012$$y2020
002722392 8564_ $$82233261$$s22153$$uhttps://cds.cern.ch/record/2722392/files/He4_Dconstraints_paper_v2.png$$y00006 \small The numerical constraints on $^4$He (black, solid) and D (black, dashed) derived using {\tt AlterBBN} as compared to the constraints from the analytical approximation of the preceding section (red and orange regions). Again, red corresponds to underproduction of $^4$He and orange corresponds to its overproduction. Deuterium tends to be overproduced. The black dotted line delimits the region of parameters where the coupling becomes large at the scale factor $a_W=10^{-9.6}$ corresponding to the weak freeze-out, $\alpha(a_W)>1$. To the left of this line higher-order terms in the Taylor expansion of the function $\alpha(\phi)$ become important. The right panel zooms in to the region where the constraints exhibit oscillations. Here, the constraints should be taken with caution as they are sensitive to non-linear effects in $\alpha$.
002722392 8564_ $$82233262$$s32903$$uhttps://cds.cern.ch/record/2722392/files/He4_Dconstraints_zoom_paper_v2.png$$y00007 \small The numerical constraints on $^4$He (black, solid) and D (black, dashed) derived using {\tt AlterBBN} as compared to the constraints from the analytical approximation of the preceding section (red and orange regions). Again, red corresponds to underproduction of $^4$He and orange corresponds to its overproduction. Deuterium tends to be overproduced. The black dotted line delimits the region of parameters where the coupling becomes large at the scale factor $a_W=10^{-9.6}$ corresponding to the weak freeze-out, $\alpha(a_W)>1$. To the left of this line higher-order terms in the Taylor expansion of the function $\alpha(\phi)$ become important. The right panel zooms in to the region where the constraints exhibit oscillations. Here, the constraints should be taken with caution as they are sensitive to non-linear effects in $\alpha$.
002722392 8564_ $$82233263$$s6000$$uhttps://cds.cern.ch/record/2722392/files/baryonDensityPlot.png$$y00000 \small \textbf{Left:} The evolution of $ \Theta_{\rm SM} $ as a function of scale factor (solid line). The contribution of non-relativistic baryons $ \Theta_b \propto a^{-3} $ is displayed by the dashed line for reference. Notice the large contribution from the $e^+e^-$ plasma. For reference, we also show the total energy density $\rho_{\rm SM}$ (dotted line). Vertical lines mark the values of the scale factor corresponding to freeze-out of weak interactions ($a_{\rm W}$), the time when electrons become non-relativistic ($a_{e}$) and BBN ($a_{\rm BBN}$). \textbf{Right:} Map of the transition history of DM evolution for various points in parameter space. Each region is labeled with the regimes the field $\phi$ passes from the weak freeze-out to the present time. Example: $I\to H\to B$ refers to an evolution that starts out dominated by the induced mass, then transitions to being dominated by Hubble friction and finally by the bare mass, $m_\phi$. The gray-shaded region on the bottom left is excluded by the condition eq.~\ref{constr1}.
002722392 8564_ $$82233264$$s14915$$uhttps://cds.cern.ch/record/2722392/files/transitionsShort.png$$y00001 \small \textbf{Left:} The evolution of $ \Theta_{\rm SM} $ as a function of scale factor (solid line). The contribution of non-relativistic baryons $ \Theta_b \propto a^{-3} $ is displayed by the dashed line for reference. Notice the large contribution from the $e^+e^-$ plasma. For reference, we also show the total energy density $\rho_{\rm SM}$ (dotted line). Vertical lines mark the values of the scale factor corresponding to freeze-out of weak interactions ($a_{\rm W}$), the time when electrons become non-relativistic ($a_{e}$) and BBN ($a_{\rm BBN}$). \textbf{Right:} Map of the transition history of DM evolution for various points in parameter space. Each region is labeled with the regimes the field $\phi$ passes from the weak freeze-out to the present time. Example: $I\to H\to B$ refers to an evolution that starts out dominated by the induced mass, then transitions to being dominated by Hubble friction and finally by the bare mass, $m_\phi$. The gray-shaded region on the bottom left is excluded by the condition eq.~\ref{constr1}.
002722392 8564_ $$82233265$$s24294$$uhttps://cds.cern.ch/record/2722392/files/final_constraints_paper.png$$y00008 \small Summary of constraints on the scale of the universal quadratic coupling, $1/\Lambda$, as a function of scalar mass $m_\phi$. Only the case of positive coupling is shown. The bounds from the $^4\rm{He}$ and D abundances are shown in the red shaded region. Additional constraints come from supernova cooling and fifth-force searches (blue), superradiance (yellow), the deBroglie wavelength of the smallest dwarf galaxies along with bounds from Ly-$\alpha$ measurements (green), and Eridanus II (purple). The constraints from measurements of the binary pulsar orbital period are given in the yellow dots, corresponding to the resonant bands. Also shown are constraints inferred from the bounds on stochastic gravitational waves by Cassini (CAS) and Pulsar Timing Arrays (PTA). See text for more detail.
002722392 8564_ $$82233266$$s22683$$uhttps://cds.cern.ch/record/2722392/files/analyticHe4constraints_paper_v2.png$$y00004 \small {\bf Left:} BBN constraints on the scalar dark matter parameter space in the case of positive coupling $\alpha=+\phi^2/\Lambda^2$. The shaded region is excluded at 95\%CL. The red shading corresponds to underproduction of $^4$He while the orange shading corresponds to overproduction. Orange dashed line shows the constraint obtained in an analysis that neglects the induced dark matter mass and uses instantaneous weak freeze-out approximation. For the parameters to the left of the black dotted line the coupling $\alpha$ becomes non-perturbative at the time of weak freeze-out (scale factor $a_W=10^{-9.6}$). {\bf Right:} Parameter space of the model with negative coupling $\alpha=-\phi^2/\Lambda^2$. The blue shaded region corresponds to tachyonic instability during BBN. It is excluded unless the initial conditions for dark matter are extremely fine-tuned. The region above the green line admits spontaneous scalarization of neutron stars.
002722392 8564_ $$82233267$$s8015$$uhttps://cds.cern.ch/record/2722392/files/analyticHe4negconstraints_paper.png$$y00005 \small {\bf Left:} BBN constraints on the scalar dark matter parameter space in the case of positive coupling $\alpha=+\phi^2/\Lambda^2$. The shaded region is excluded at 95\%CL. The red shading corresponds to underproduction of $^4$He while the orange shading corresponds to overproduction. Orange dashed line shows the constraint obtained in an analysis that neglects the induced dark matter mass and uses instantaneous weak freeze-out approximation. For the parameters to the left of the black dotted line the coupling $\alpha$ becomes non-perturbative at the time of weak freeze-out (scale factor $a_W=10^{-9.6}$). {\bf Right:} Parameter space of the model with negative coupling $\alpha=-\phi^2/\Lambda^2$. The blue shaded region corresponds to tachyonic instability during BBN. It is excluded unless the initial conditions for dark matter are extremely fine-tuned. The region above the green line admits spontaneous scalarization of neutron stars.
002722392 8564_ $$82233268$$s12004$$uhttps://cds.cern.ch/record/2722392/files/evolutionPlotNegative.png$$y00002 \small {\bf Left:} Evolution of $\phi^2/\Lambda^2$ as a function of scale factor $a$ for the negative coupling and parameters $m_\phi=10^{-17}$ eV, $\Lambda=10^{17.3}$ GeV. The red-dashed curve shows the full numeric solution whereas the solid red curve shows the effective solution which patches together the oscillations with an exponential growth. {\bf Right:} Evolution of $ \phi^2/\Lambda^2$ as a function of scale factor $a$ for positive coupling and parameters $m_\phi=10^{-20}$ eV, $\Lambda=10^{17}$ GeV. The red-dashed curve shows the full numeric solution whereas the red solid curve gives the effective solution which patches together the slowly oscillating/frozen phase with a WKB-type solution in the intermediate regime. The pure WKB amplitude, neglecting Hubble friction, is shown in orange. The green curve shows the evolution of the $\phi$-field neglecting the induced mass.
002722392 8564_ $$82233269$$s40215$$uhttps://cds.cern.ch/record/2722392/files/evolutionPlotDetailed.png$$y00009 Same as fig.~\ref{fig:DM density} (right), but with transition times marked with vertical lines and the amplification function visualized by the red dashed line. The amplification function (gray, dashed), which takes values in the range between 1 and 2, is shown here with an artificial amplitude for visualization. The effective solution (red, solid) is the patching between the full numeric solution (red, dashed) and the WKB-amplitude (orange, solid) for the rapidly-oscillating regions.
002722392 8564_ $$82233270$$s2589038$$uhttps://cds.cern.ch/record/2722392/files/2006.04820.pdf$$yFulltext
002722392 8564_ $$82233271$$s35908$$uhttps://cds.cern.ch/record/2722392/files/evolutionPlotPostive.png$$y00003 \small {\bf Left:} Evolution of $\phi^2/\Lambda^2$ as a function of scale factor $a$ for the negative coupling and parameters $m_\phi=10^{-17}$ eV, $\Lambda=10^{17.3}$ GeV. The red-dashed curve shows the full numeric solution whereas the solid red curve shows the effective solution which patches together the oscillations with an exponential growth. {\bf Right:} Evolution of $ \phi^2/\Lambda^2$ as a function of scale factor $a$ for positive coupling and parameters $m_\phi=10^{-20}$ eV, $\Lambda=10^{17}$ GeV. The red-dashed curve shows the full numeric solution whereas the red solid curve gives the effective solution which patches together the slowly oscillating/frozen phase with a WKB-type solution in the intermediate regime. The pure WKB amplitude, neglecting Hubble friction, is shown in orange. The green curve shows the evolution of the $\phi$-field neglecting the induced mass.
002722392 8564_ $$82268800$$s2290031$$uhttps://cds.cern.ch/record/2722392/files/scoap3-fulltext.pdf$$yArticle from SCOAP3
002722392 8564_ $$82270127$$s23447$$uhttps://cds.cern.ch/record/2722392/files/final_constraints_superradiance.png$$y00008 \small Summary of constraints on the scale of the universal quadratic coupling, $1/\Lambda$, as a function of scalar mass $m_\phi$. Only the case of positive coupling is shown. The bounds from the $^4\rm{He}$ and D abundances are shown in the red shaded region. Additional constraints come from supernova cooling and fifth-force searches (blue), superradiance (yellow), the deBroglie wavelength of the smallest dwarf galaxies along with bounds from Ly-$\alpha$ measurements (green), and Eridanus II (purple). Above the black dotted lines, the induced mass from the black hole accretion disk exceeds $m_\phi$ and the dynamics of superradiance may be affected. The constraints from measurements of the binary pulsar orbital period are given in the yellow dots, corresponding to the resonant bands. Also shown are constraints inferred from the bounds on stochastic gravitational waves by Cassini (CAS) and Pulsar Timing Arrays (PTA). See text for more detail.
002722392 8564_ $$82334635$$s2290031$$uhttps://cds.cern.ch/record/2722392/files/scoap.pdf$$yArticle from SCOAP3
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