arXiv subjects

Colin D. Froggatt

Publications and source records attributed to Colin D. Froggatt.

15 recordsLinked to original sources

arXiv2026

Dark Matter as Screened Ordinary Matter

We look at our since long studied model for dark matter as being pearls of a speculated new vacuum containing highly compressed ordinary matter, with so much ordinary in it that the content of ordinary matter in the dark matter pearls dominate. Most dark matter models have the dark matter consisting mainly of new-physics-matter such as WIMPs being supersymmetric partners of possibly known particles or, as in Maxim Khlopovs model, a doubly negatively charged new-physics-particle with a helium nucleus attached. But usually the new-physics matter makes up weight-wise the major content. It is only in our model that the ordinary matter content in the dark matter dominates. We here expose some weak phenomenological evidence that, in truth, dark matter should be of the type with a dominant component of ordinary matter (weight-wise), thus favoring as the typical example our previously so much studied vacuum type 2 model. The main such evidence is that we manage a fit to data in which the 3.5 keV X-rays, presumed to result from dark matter, come both from collisions of dark matter with dark matter and from dark matter with ordinary matter! Both mechanisms are of so similar an order of magnitude that they are both seen, indicating that their similarity is due to a significant similarity between dark with ordinary matter. The fact that the amounts of ordinary and dark matter only deviate by a factor 6 points in the same direction. Using the information obtained from this fitting, we develop our speculation that the main content weight-wise of dark matter is ordinary matter to the very DAMA experiment. Actually we found three spots on the sky in which we fit the observed production of 3.5 keV X-rays with ordinary plus dark scattering.

hep-ph↗

arXiv2024

Domain Walls and Hubble Constant Tension

We present the idea that replacing the cosmological constant $Λ$ in the $Λ$CDM model by a distribution of walls, with very low tension compared to what one would expect from new physics, could help explaining the tension in the Hubble constant fits in the Standard Cosmological Model. Using parameters from our model for dark matter as macroscopic pearls, we can get a promising order of magnitude for the correction to the Hubble constant estimated from observations of the cosmic microwave background. Our model is on the borderline of failing by predicting too large extra fluctuations as a function of direction in the cosmological microwave background radiation. However, imagining the bubbles in the voids to have come from more somewhat smaller big bubbles also occurring outside the big voids may help. We estimate that, in order to have big volumes of the new vacuum in intergalactic space, a very high temperature is needed and that such regions would be likely to get cooled, freeze and shrink down to the degenerate form of dark matter if hitting some ordinary matter, as is likely in the denser parts of the Universe. We also review our model for dark matter, and develop the understanding of the stopping of the dark matter particles in the shielding of say the DAMA-LIBRA underground experiment and the counting rate this experiment observes. We manage to obtain a consistent fit with a mass $M = 2 \cdot 10^{-18}$kg = $10^9$GeV and radius $R = 10^{-10}$m for the dark matter pearls, corresponding to a tension in the domain wall of $S= (8 {\rm MeV})^3$.

astro-ph.CO↗

arXiv2023

Our Dark Matter Stopping in the Earth

We have worked for some time on a model for dark matter, in which dark matter consists of small bubbles of a new speculated type of vacuum, which are pumped up by some ordinary matter such as diamond, so as to resist the pressure of the domain wall separating the two vacua. Here we put forward thoughts on, how such macroscopic pearls would have their surrounding dust cleaned off passing through the atmosphere and the Earth, and what their distribution would be as a function of the depth of their stopping point and the distribution of the radiation emitted from them. In our model we assume that they radiate 3.5 keV electrons and photons, after having been excited during their passage into the Earth. The purpose of such an estimation of the radiation distribution is to explain the truly mysterious fact that, among all the underground experiments seeking dark matter colliding with the Earth material, only the DAMA-LIBRA experiment has seen any evidence of dark matter. This is an experiment based on solid NaI scintillators and is rather deep at 1400 m. It is our point that we can arrange the main radiation to appear in the relatively deep DAMA- LIBRA site, and explain that the dark matter pearls cannot stop in a fluid, such as xenon in the xenon based experiments.

hep-ph↗

arXiv2023

Domain Walls of Low Tension in Cosmology

In the present article we put up for discussion the idea of there existing several versions, phases, of the vacuum, in the spirit in which we have long worked on this idea, namely the Multiple Point Criticality Principle, which also says that these different vacuum phases have the same energy density. We mention that we indeed predicted the Higgs mass to be 135 plus minus 10 GeV, which when measured turned out to be 125 GeV, using the assumption of this Multiple Point Criticality Principle. We consider the possibility that there is one type of vacuum in the galaxy clusters (the usual vacuum) and another type of vacuum in the voids. The hope that there could indeed be such a low tension S of the domain wall between these two phases, that it would not totally upset cosmology is based on our dark matter model. In this model dark matter consists of pearls or bubbles of a new vacuum phase, with ordinary matter inside it under very high pressure. The order of magnitude of cubic root S of order MeV or 100 MeV could make such domain walls astronomically viable. We successfully estimate the order of magnitude of the variations in the fine structure constant in different places astronomically, but the similar variations in proton mass over electron mass should have been much bigger than seen experimentally in our model. The Universe s surprisingly early galaxies seen by JWST, James Webb telescope, may agree well with our model. Replacing the usual cosmological constant by domain walls in the standard cosmological model would lead to a cubic root of the tension being cubic root of S of order 30 MeV.

astro-ph.CO↗

arXiv2023

Dusty Dark Matter Bubbles of a New Vacuum stopped in Earth and Radiating 3.5 keV X-rays

We continue our work on a proposal for what dark matter could be, namely that the dark matter consists of essentially macroscopic objects built from ordinary matter. The only element of new physics is that there should exist several types or phases of vacuum. Then the dark matter particles are bubbles of a new type of vacuum filled with ordinary matter - say diamond - under high pressure and the whole bubble is supposedly contaminated by the materials in the extra galactic or intragalactic space able to form dust. The dust has a lower than dimension 3 structure and may well be long chains of atoms. We begin speculations on identifying the phase transition between the vacua, which we require in our model, with a (second order?) transition revealed in the Columbia plot with quark masses as axes. In the corner of small quark masses there is a true phase transition as temperature is raised, while outside this region there is instead no genuine phase transition under variation of the temperature but rather only a crossover.

hep-ph↗

arXiv2023

Dusty Dark Matter Pearls Developed

We briefly review and update our earlier published model for dark matter consisting of nanometer size bubbles of a new speculated vacuum phase in which some ordinary material, e.g. carbon, is present under high pressure caused by the surface tension of the domain wall surrounding the bubble. These bubbles or pearls are surrounded by dust grains, and it is one of the new points of the present article that this dust grain rather than being a three dimensional blob of ordinary matter is a lower dimensional object of some lower Hausdorff dimension. We make several order of magnitude fits and find rather good agreement for our model. However, we must imagine that the very high - 3.5 kev - homolumo gap assumed present in the highly compressed medium inside the bubble has influenced the neighboring dust, so as to make it significantly harder than usual dust. This is to ensure that we obtain the correct order of magnitude for the velocity in the region where the ratio cross section over mass falls drastically.The dark matter pearls loose their dust when impacting the Earth and the shielding. They must reach down with their terminal velocity through the shielding to the Dama observatory in less than a year, so that there is no problem in obtaining the seasonal variation effect the Dama experiment has observed. This is easier to achieve with a sufficiently high pearl mass and this mass is not so strongly restricted once the dust grain is lower dimensional.

physics.gen-ph↗

arXiv2022

Nano meter Size Dirty Dark Matter Pearls, electron-signal, IMP or SIDM, not WIMP

Through several articles we have developed a model for dark matter as consisting of bubbles of a new (speculated) type of vacuum, starting from cm-sized pearls or balls down to atomic size ones and now we believe they have nanometer sizes. In the latest development of our model we have the bubbles of the new vacuum imbedded in dust grains very similar to the grains present in interstellar and intergalactic space anyway, although the presence of the bubble with a very large homolumo gap in its single electron spectrum influences the dust grain material so as to become denser and harder. We have earlier explained how our dark matter particles get stopped in the shielding, so that normally expected nucleonic collisions are not observable. The signal of the dark matter in the underground experiments rather becomes decays of excited particles actually with the energy of the homolumo gap, which is also equal to the photon energy of the X-ray line presumably observed astronomically from galaxy clusters etc. A new calculation here is a fitting of the velocity dependence of the dark matter self-interaction as estimated by Correa [15], using deviations from the only gravitationally interacting dark matter in dwarf galaxies. Let us stress that apart from the speculated new vacuum we have no new physics, and if the couplings in the Standard Model were adjusted to make degenerate vacua as speculated according to our Multiple Point Principle (MPP) we would only need the Standard Model, so dark matter would not require new physics.

astro-ph.HE↗

arXiv2021

Dark Matter Macroscopic Pearls, 3.55 keV X-ray line, How big ?

We study the 3.55 keV X-ray suspected to arise from dark matter in our model of dark matter consisting of a bubble of a new phase of the vacuum, the surface tension of which keeps ordinary matter under high pressure inside the bubble. We consider two versions of the model: Old large pearls model : We worked for a long time on a pearl picture with pearl / bubbles of cm-size adjusted so that the impacts of them on earth could be identified with events of the mysterious type that happened in Tunguska in 1908. We fit both the very frequency, the 3.55 keV, and the overall intensity of the X-ray line coming from the center of the Milky Way and from galaxy clusters with one parameter in the model in which this radiation comes from collisions of pearls. New small pearl model: Our latest idea is to let the pearls be smaller than atoms but bigger than nuclei so as to manage to fit the 3.5 keV X-rays coming from the Tycho supernova remnant in which Jeltema and Profumo observed this line. Further we also crudely fit the DAMA-LIBRA observation with the small pearls, and even see a possibility for including the electron-recoil-excess seen by the Xenon1T experiment as being due to de-excitation via electron emission of our pearls. The important point of even our small size pearl model is that the cross section of our "macroscopic" pearls is so large that the pearls interact several times in the shielding but, due to their much larger mass than the typical nuclei, are {\bf not stopped by only a few interactions}. Nevertheless only a minute fraction of the relatively strongly interacting pearls reach the 1400 m down to the DAMA experiment, but due to the higher cross section we can fit the data anyway.

hep-ph↗

arXiv2020

The 3.5 keV line from non-perturbative Standard Model dark matter balls

Our earlier put forward model of dark matter, consisting of cm-size pearls with ordinary matter inside under high pressure and with a mass of order $1.4 *10^8$ kg, is used to explain the mysterious 3.5 keV X-ray line from the galactic center and various galaxies and galaxy clusters. The pearls are bubbles of a new type of vacuum and thus surrounded by a surface tension providing the high pressure. We have two rather successful order of magnitude numerical results: 1) the X-ray energy of 3.5 keV comes out as the homolumo-gap or rather as the energy due to screening of electrons in the high pressure ordinary matter inside the pearls, and is well fitted. %predicted correctly to within a factor %{\bf tbc 2} %3; %$40 \%$; 2) Using the fitting of Cline and Frey for dark matter radiation arising from collisions or annihilations of dark matter particles we fit the overall intensity of the radiation in our pearl model. We find that a pearl of the minimal size required just by stability, as used in our previous work \cite{Tunguska}, is inconsistent with the observed frequency and intensity of the 3.5 keV line. However the predictions of our model are very sensitive to the radius of the pearls and an excellent fit to both experimental quantities is obtained for a pearl of radius of 2.8 cm.

hep-ph↗

arXiv2019

Anomalies from Non-Perturbative Standard Model Effects

We interpret anomalies, deviations, from the standard model as being in fact due to effects not given by perturbation, because the top Yukawa coupling is after all so large that not by perturbation effects become important. Most of the anomalies found have the character of signaling violation of lepton universality. There are four lepton universality violating anomalies known at present, which we shall fit with one overall scale parameter to order of magnitude accuracy. One can look at the picture that we have found - due to the rather strong top Yukawa coupling - as a new sector of strongly interacting particles analogous to quantum color dynamics inside the standard model! In addition we treat what is presumably also an anomaly: the experimental value of the direct charge conjugation parity violation parameter epsilon prime over epsilon turns out to be a factor 2 or more larger than the standard model prediction,but fit our model. However if we include in our anomaly model such processes not involving leptons (but only quarks), it seems superficially that we obtain very large - and unacceptable - anomalies in meson zero meson zero bar etc. mixing. To rescue our model from this falsification, we think of the interacting quarks as provided with clouds (on half terra electron volt scale) of, and that too strongly interacting such clouds cannot penetrate into each other. Thereby the interactions and thus the resulting anomalies are damped. Even with such a crutch for our theory we only barely manage to avoid an overlarge anomaly in the indirect charge conjugation parity violation parameter epsilon. Our modified model also predicts an anomalous contribution to the meson long to meson short mass difference of the same order of magnitude as the experimental value, which is consistent with the deviation from the standard model lattice value.

hep-ph↗

arXiv2016

Production and Decay of 750 Gev state of 6 top and 6 anti top quarks

Crude estimates are made of the branching ratios and pair production cross-section for our previously proposed bound state S of six top and six antitop quarks identified with the diphoton excess recently observed in ATLAS and CMS. We estimate the pair production cross section to be approximately 12 times that for fourth family quarks. Hence we predict $σ(pp \rightarrow SS + anything) \approx 2$ pb at 13 TeV and an increase by a factor 10 over the cross section at 8 TeV. Crude estimates of the main branching ratios relative to the diphoton decay give $Γ(S\rightarrow γ+γ) \propto 1$, $Γ(S\rightarrow t + \bar{t})\propto 378$, $Γ(S \rightarrow gluon+gluon)\propto 117$, $Γ(S\rightarrow Higgs+Higgs)\propto 15$, $Γ(S\rightarrow W+W)\propto 30$ and $Γ(S\rightarrow Z+Z) = 15$. These estimates are consistent with the LHC bounds at 8 TeV within a factor 1.25. We expect the $S \rightarrow γγ$ events to be produced together with another S resonance decaying typically into top-antitop or gluon-gluon jets.

hep-ph↗

arXiv2016

Dark Matter Balls Help Supernovae to Explode

As a solution to the well-known problem that the shock wave potentially responsible for the explosion of a supernova actually tends to stall, we propose a new energy source arising from our model for dark matter. Our earlier model proposed that dark matter should consist of cm-large white dwarf-like objects kept together by a skin separating two different sorts of vacua. These dark matter balls or pearls will collect in the middle of any star throughout its lifetime. At some stage during the development of a supernova the balls will begin to take in neutrons and then other surrounding material. By passing into a ball nucleons fall through a potential of order 10 MeV, causing a severe production of heat - of order 10 foe for a solar mass of material eaten by the balls. The temperature in the iron core will thereby be raised, splitting up the iron into smaller nuclei. This provides a mechanism for reviving the shock wave when it arrives and making the supernova explosion really occur. The onset of the heating due to the dark matter balls would at first stop the collapse of the supernova progenitor. This opens up the possibility of there being {\em two} collapses giving two neutrino outbursts, as apparently seen in the supernova SN1987A - one in Mont Blanc, and one 4 hours 43 minutes later in both IMB and Kamiokande.

astro-ph.HE↗

arXiv2006

Implementation of the Multiple Point Principle in the Two-Higgs Doublet Model of type II

The multiple point principle (MPP) is applied to the non--supersymmetric two-Higgs doublet extension of the Standard Model (SM). The existence of a large set of degenerate vacua at some high energy scale caused by the MPP results in a few relations between Higgs self-coupling constants which can be examined at future colliders. The numerical analysis reveals that these MPP conditions constrain the mass of the SM--like Higgs boson to lie below 180 GeV for a wide set of MPP scales $Λ$ and $\tanβ$.

hep-ph↗

arXiv2002

Neutrinos in the Family Replicated Gauge Group Model

We present a discussion of the neutrino mass problem in the anti-grand unification theory based on three family replicated copies of the Standard Model gauge group (SMG). We consider two versions of the theory, with and without right-handed neutrinos, and present order of magnitude fits to the 17 measured quark-lepton mass and mixing angle variables. In the model without right-handed neutrinos, based on the gauge group $SMG^3\times U(1)_f$ and an isotriplet Higgs, we obtain a good 4 parameter fit, but with a vacuum oscillation solution to the solar neutrino problem. In the second model, based on the gauge group $(SMG\times U(1)_{B-L})^3$, we obtain a good 5 parameter fit using the usual right-handed neutrino see-saw mechanism to generate an LMA-MSW solution to the solar neutrino problem. The CHOOZ mixing angle bound is easily satisfied in the first model and is close to the predicted value in the second model.

hep-ph↗

arXiv2001

Quark-Lepton Masses and the Neutrino Puzzle in the AGUT Model

We first discuss an approach to the fermion mass problem, according to which the whole of flavour mixing for quarks is determined by the mechanism responsible for generating the physical masses of the up and down quarks: the Lightest Flavour Mass Generation model. Then we consider fermion masses in the Anti-grand Unification Theory and, in particular, the neutrino mass and mixing problem.

hep-ph↗