Exponential Inflation Research Articles

The labor of assetization: producing ‘hypergrowth’ inside a tech startup

Abstract Venture capitalists maximize profits not by ‘squeezing’ efficiencies out of established companies, but instead by promoting ceaseless experimentation aimed at helping startups achieve ‘hypergrowth’. To date, there is limited empirical evidence of both how startups achieve hypergrowth, and the impact of these practices on organizations and workers. This article draws on 19 months of participant-observation research inside a venture-backed startup I call AllDone to trace the links between the institution of venture capital and the organization of work. Although AllDone executives engaged in cost-cutting strategies common to other financialized firms, they also developed distinctive corporate strategies and organizational structures. Each of the company’s three work teams was organized to perform interdependent functions in support of venture capital’s imperative for rapid and exponential asset value inflation. I conclude with a discussion of the article’s implications for research on venture capital, startup work, and the relationship between financialization and work more broadly.

MATHEMATICAL ANALYSIS OF COSMOLOGICAL MODELS WITH LINEARLY VARYING DECELERATION PARAMETER

Bianchi type-V is investigated using a decaying cosmological constant with perfect fluid. The study solves Einstein field equations by assuming that the deceleration parameter q is functionally connected to the Hubble parameter H, which yields the scale factor a. As cosmic time t increases, the cosmological model experiences exponential inflation. The physical characteristics and behavior of the cosmological model are also covered.

Exponential authorship inflation in neuroscience and psychology from the 1950s to the 2020s.

How many researchers does it take to publish an article in top journals in neuroscience and psychology? Manually coding 42,580 articles spanning 1879-2021 from 32 journals, we examined the evolution of authorship size and its rate of change. Moreover, we assessed the driving forces behind these changes. We found that, starting from the 1950s but not earlier, the average authorship size per article in neuroscience and psychology has increased exponentially, growing by 50% and 31% over the last decade and reaching a record high of 10.4 and 4.8 authors in 2021, respectively. Single-authored articles have become a rarity today, particularly in primary research articles: 1.7% in neuroscience and 2.2% in psychology in 2019-2021 (vs. 5.7% and 11.2% in review articles). With the withering of sole authors rises a new type of authorship, group authors (e.g., a consortium). Group authorship was rare before 2000, but in 2019-2021, it appeared in 4.1% of articles in neuroscience, mostly in genetics, neuroimaging, and disease-outnumbering single-authored articles for the first time-and 0.7% in psychology, mostly in developmental and clinical research. The exponential inflation in authorship size could not be attributed to behaviors of professional editors in profit-oriented journals but aligns with a hybrid epistemic-behavioral-cultural account-an account that integrates multidimensional factors, including increased research complexity, the benefits of collaboration, the rise of government-funded research, changing norms in authorship practices, and biased incentives in evaluation. These findings suggest troubling implications for research reproducibility, innovations, equity/diversity, and ethics, calling for policy deliberations to address potential negative ramifications. (PsycInfo Database Record (c) 2023 APA, all rights reserved).

Supplemental Material for Exponential Authorship Inflation in Neuroscience and Psychology From the 1950s to the 2020s

Supplemental Material for Exponential Authorship Inflation in Neuroscience and Psychology From the 1950s to the 2020s

Stability investigations of isotropic and anisotropic exponential inflation in the Starobinsky–Bel–Robinson gravity

In this paper, we would like to examine whether a novel Starobinsky–Bel–Robinson (SBR) gravity model admits stable exponential inflationary solutions with or without spatial anisotropies. As a result, we are able to derive an exact de Sitter inflationary to this SBR model. Furthermore, we observe that an exact Bianchi type I inflationary solution does not exist in the SBR model. However, we find that a modified SBR model, in which the sign of coefficient of [Formula: see text] term is flipped from positive to negative, can admit the corresponding Bianchi type I inflationary solution. Unfortunately, stability analysis using the dynamical system approach indicates that both of these inflationary solutions turn out to be unstable. Interestingly, we show that a stable de Sitter inflationary solution can be obtained in the modified SBR gravity.

Cosmological solutions with time-delay

We introduce a time-delay function in bulk viscosity cosmology. Even for bulk viscosity functions where closed-form solutions are known, because of the time-delay term, the exact solutions are lost. Therefore in order to study the cosmological evolution of the resulting models we perform a detailed analysis of the stability of the critical points, which describe de Sitter solutions, by using Lindstedt’s method. We find that for the stability of the critical points it depends also on the time-delay parameter, where a critical time-delay value is found which plays the role of a bifurcation point. For time-delay values near the critical value, the cosmological evolution has a periodic evolution, this oscillating behavior is because of the time-delay function. We find a new behavior near the exponential expansion point, which can be seen also as an alternative way to exit the exponential inflation.

Estimating Analytical Errors of Glomerular Filtration Rate Measurement.

Few studies are available on how to optimize time points for sampling and how to estimate effects of analytical uncertainty when glomerular filtration rate (GFR) is calculated. We explored the underlying regression mathematics of how analytical variation of a kidney filtration marker affects 1-compartment, slope-and-intercept GFR calculations, using 2 or 3 time points following a bolus injection, and used this to examine the results from 731 routine 3-point iohexol plasma clearance measurements. GFR calculations inflated analytical uncertainty if the time points were taken too late after the bolus injection and too close after each other. The uncertainty in GFR calculation was, however, the same as the analytical uncertainty if optimal time points were used. The middle of the 3 samples was of little value. The first sample should be taken as early as possible after the distribution phase. Sampling before the patient specific half-life of the kidney filtration marker resulted in an exponential error inflation whereas no error inflation was seen when sampling occurred later than 2 half-lives. Theoretical GFR uncertainty could be lowered 2.6-fold if individually optimized time points for sampling had been used in our 731 clearance measurements. Using Taylor expansions to approximate the moments of transformed random variables, the uncertainty of an individual GFR measurement could be calculated in a simple enough way to be applicable by laboratory software. We provide a theoretical foundation to select patient-optimal time points that may both limit errors and allow calculation of GFR uncertainty.

Generalizing the constant-roll condition in scalar inflation

In this work, we generalize the constant-roll condition for minimally coupled canonical scalar field inflation. Particularly, we shall assume that the scalar field satisfies the condition [Formula: see text], and we derive the field equations under this assumption. We call the framework extended constant-roll framework. Accordingly, we calculate the inflationary indices and the corresponding observational indices of inflation. In order to demonstrate the inflationary viability, we choose three potentials that are problematic in the context of slow-roll dynamics, namely, chaotic, linear power-law and exponential inflation, and by choosing a simple power-law form for the smooth function [Formula: see text], we show that in the extended constant-roll framework, the models are compatible with the latest 2018 Planck constraints on inflation. We also justify appropriately why we called this new framework extended constant-roll framework, and we show that the condition [Formula: see text] is equivalent to the condition [Formula: see text], with the latter condition being a simple generalization of the constant-roll condition. Finally, we examine an interesting physical situation, in which a general extended constant-roll scalar field model is required to satisfy the cosmological tracker condition used in quintessence models. In contrast to the slow-roll and ordinary constant-roll cases, in which case the tracker condition is not compatible with neither the slow-roll or the ordinary constant-roll conditions, the extended constant-roll condition can be compatible with the tracker condition. This feature leads to a new inflationary phenomenological framework, the essential features of which we develop in brief. The main feature of the new theoretical framework is that the function [Formula: see text] and the potential [Formula: see text] are no longer free to choose, but these are directly functionally related.

Reheating in small-field inflation on the brane: the swampland criteria and observational constraints in light of the PLANCK 2018 results

We study cosmological inflation and its dynamics in the framework of the Randall–Sundrum II brane model. In particular, we analyze in detail four representative small-field inflationary potentials, namely Natural inflation, Hilltop inflation, Higgs-like inflation, and Exponential SUSY inflation, each characterized by two mass scales. We constrain the parameters for which a viable inflationary Universe emerges using the latest PLANCK results. Furthermore, we investigate whether or not those models in brane cosmology are consistent with the recently proposed Swampland Criteria, and give predictions for the duration of reheating as well as for the reheating temperature after inflation. Our results show that (i) the distance conjecture is satisfied, (ii) the de Sitter conjecture and its refined version may be avoided, and (iii) the allowed range for the five-dimensional Planck mass, M_5, is found to be 10^5,text {TeV}lesssim M_5lesssim 10^{12},text {TeV}. Our main findings indicate that non-thermal leptogenesis cannot work within the framework of RS-II brane cosmology, at least for the inflationary potentials considered here.

Asymptotic de Sitter inflation in different geometric backgrounds

In this paper, we will show that a power law asymptotic de Sitter inflation will be established for all values of Hankel indices [Formula: see text] that relate to the different background spacetimes of the universe in their evolution. First, we calculate the relations for the Hubble, deceleration, slow roll and the equation of state parameters in terms of the Hankel function index [Formula: see text]. We then show that the obtained relations and figures correspond to the conventional limit conditions for pure de Sitter inflation. As an important result, power law quasi-de Sitter inflation is more likely to occur after exponential pure de Sitter inflation. Also, in the proposed model, the universe can always be in the accelerating expansion phase for all values of index [Formula: see text].

Ground deformation reveals the scale-invariant conduit dynamics driving explosive basaltic eruptions

The mild activity of basaltic volcanoes is punctuated by violent explosive eruptions that occur without obvious precursors. Modelling the source processes of these sudden blasts is challenging. Here, we use two decades of ground deformation (tilt) records from Stromboli volcano to shed light, with unprecedented detail, on the short-term (minute-scale) conduit processes that drive such violent volcanic eruptions. We find that explosive eruptions, with source parameters spanning seven orders of magnitude, all share a common pre-blast ground inflation trend. We explain this exponential inflation using a model in which pressure build-up is caused by the rapid expansion of volatile-rich magma rising from depth into a shallow (<400 m) resident magma conduit. We show that the duration and amplitude of this inflation trend scales with the eruption magnitude, indicating that the explosive dynamics obey the same (scale-invariant) conduit process. This scale-invariance of pre-explosion ground deformation may usher in a new era of short-term eruption forecasting.

A New Solution of Intermediate Cosmological Inflation with the Effect of Scalar Field

According to the inflationary model, the universe had a brief period of extraordinarily rapid expansion or inflation during which its diameter increased by a factor at least 1025 times larger than previously thought. In this work an analysis is given on inflationary universe, which expands at a rate intermediate between that of power-law and exponential inflation. We have examined the model of Barrow which is solved exactly and leaded to power law inflation. We have tested a new potential by applying the scalar field using the equation of motion and found some new interior solutions.&#x0D; The Chittagong Univ. J. Sci. 40(1) : 112-121, 2019

Exact and Slow-Roll Solutions for Exponential Power-Law Inflation Connected with Modified Gravity and Observational Constraints

We investigate the ability of the exponential power-law inflation to be a phenomenologically correct model of the early universe. We study General Relativity (GR) scalar cosmology equations in Ivanov–Salopek–Bond (or Hamilton–Jacobi like) representation where the Hubble parameter H is the function of a scalar field ϕ. Such approach admits calculation of the potential for given H(ϕ) and consequently reconstruction of f(R) gravity in parametric form. By this manner the Starobinsky potential and non-minimal Higgs potential (and consequently the corresponding f(R) gravity) were reconstructed using constraints on the model’s parameters. We also consider methods for generalising the obtained solutions to the case of chiral cosmological models and scalar-tensor gravity. Models based on the quadratic relationship between the Hubble parameter and the function of the non-minimal interaction of the scalar field and curvature are also considered. Comparison to observation (PLANCK 2018) data shows that all models under consideration give correct values for the scalar spectral index and tensor-to-scalar ratio under a wide range of exponential-power-law model’s parameters.

Signature flipping of isotropic homogeneous space-time with holographic dark energy in [formula omitted]gravity

Present investigation devoted to the dynamical study of isotropic and homogeneous FRW space-time filled with a Holographic dark energy fluid with cosmic string in the framework of numerous form of f(G)gravity models say linear, quadratic and inverse model. We determine the aspects of the model by considering the hybrid expansion law for the average scale factor that yields power and exponential inflation cosmologies, in its special cases. As per the observation, the model is singular and singularity observed at an initial epoch. The contribution of Gauss-Bonnet term in linear and quadratic model is just like as cosmological constant hence for whole expansion it is ΛCDMmodel which supports and resembles with the observational fact that the usual matter is about 4% and the dark energy occupies near about 73% of the energy also the results with several high precision observational experiments, especially the Wilkinson Microwave Anisotropic Probe (WMAP) satellite experiment.

Power spectrum of stochastic wave and diffusion equations in the warm inflation models

We discuss dissipative stochastic wave and diffusion equations resulting from an interaction of the inflaton with an environment in an external expanding homogeneous metric. We show that a diffusion equation well approximates the wave equation in a strong friction limit. We calculate the long wave power spectrum of the wave equation under the assumption that the perturbations are slowly varying in time and the expansion is almost exponential. Under the assumption that the noise has a form invariant under the coordinate transformations we obtain the power spectrum close to the scale invariant one. In the diffusion approximation we go beyond the slow variation assumption. We calculate the power spectrum exactly in models with exponential inflation and polynomial potentials and with power-law inflation and exponential potentials.

A Different Cosmology—Thoughts from Outside the Box

In this paper, we present a new cosmology based on the idea of a universe dominated by vacuum energy with time-varying curvature. In this model, the universe began with an exponential Plank era inflation before transitioning to a spacetime described by Einstein’s equations. While no explicit model of the Plank era is yet known, we do establish a number of properties that the vacuum of that time must have exhibited. In particular, we show that structures came into existence during that inflation that were later responsible for all cosmic structures. A new solution of Einstein’s equations incorporating time-varying curvature is presented which predicts that the scaling was initially power law with a parameter of y=1/2 before transitioning to an exponential acceleration of the present-day scaling. A formula relating the curvature to the vacuum energy density is also a part of the solution. A non-conventional model of nucleosynthesis provides a solution for the matter/antimatter asymmetry problem and a non-standard origin of the CMB. The CMB power spectrum is shown to be a consequence of uncertainties embedded during the initial inflation and the existence of superclusters. Using Einstein’s equations, we show that so-called dark matter is, in fact, vacuum energy. A number of other issues are discussed.

Reconstruction of general relativistic cosmological solutions in modified gravity theories

We study the special class of the exact solutions in cosmological models based on the Generalized Scalar-Tensor Gravity with non-minimal coupling of a scalar field to the Ricci scalar and to the Gauss-Bonnet scalar in 4D Friedmann universe corresponding to similar ones in GR. The parameters of cosmological perturbations in such models correspond to the case of Einstein gravity with a high precision. As the example of proposed approach, we obtain the exact solutions for the power-law and exponential power-law inflation.

Primordial perturbations and non-gaussianities in Hořava-Lifshitz gravity * * Partly supported by the Chinese National Youth Thou-sand Talents Program (71000-41180003)

We investigate primordial perturbations and non-gaussianities in the Hořava-Lifshitz theory of gravitation. In the UV limit, the scalar perturbation in the Hořava theory is naturally scale-invariant, ignoring the details of the expansion of the Universe. One may thus relax the exponential inflation and the slow-roll conditions for the inflaton field. As a result, it is possible that the primordial non-gaussianities, which are " slow-roll suppressed” in the standard scenarios, become large. We calculate the non-gaussianities from the bispectrum of the perturbation and find that the equilateral-type non-gaussianity is of the order of unity, while the local-type non-gaussianity remains small, as in the usual single-field slow-roll inflation model in general relativity. Our result is a new constraint on Hořava-Lifshitz gravity.

Oscillatory nature of the Okmok volcano's deformation

The time-dependent deformation of volcanic edifices can help one understand the dynamics of pre-eruptive overpressure build-up in magma chambers. Thus, geodetic time series recorded at the Okmok volcano, in Alaska, show a pattern of fast and short inflations — referred to as “pulses” — followed by either slower and longer deflations, or time intervals with no deformation. This pattern is superimposed onto a longer-period inflation. A rapid inflation occurred just before the 2008 eruption, which suggests that the underlying process may lead to eruptions. It is crucial to understand whether such a behavior is driven by external forcing, such as melt supply variations, or whether it can develop spontaneously within the volcano's plumbing system. Here we model the observed oscillations (2004–2008) as resulting from the hydraulic interaction between two shallow magma chambers fed by a deeper source region, a geometry that is consistent with geochemical, petrological, and geophysical data. The model shows that episodes of periodic fast inflations occur (i) when a viscosity gradient is present in the vertical pipe, for instance as the result of a temperature gradient; and (ii) when the flux supplying the shallower chamber lies between two bounds that we derive analytically. The deformation pulses observed at Okmok can, therewith, be fully explained by the internal variability of the magmatic system and do not require time-variable external forcing. The proposed model can also be seen as an improvement upon the classic hydraulic models regularly used to explain a commonly observed pattern of volcanic deformations, i.e. exponential inflation.

Exponential inflation with F(R) gravity

In this paper, we shall consider an exponential inflationary model in the context of vacuum $F(R)$ gravity. By using well-known reconstruction techniques, we shall investigate which $F(R)$ gravity can realize the exponential inflation scenario at leading order in terms of the scalar curvature, and we shall calculate the slow-roll indices and the corresponding observational indices, in the context of slow-roll inflation. We also provide some general formulas of the slow-roll and the corresponding observational indices in terms of the $e$-foldings number. In addition, for the calculation of the slow-roll and of the observational indices, we shall consider quite general formulas, for which it is not necessary for the assumption that all the slow-roll indices are much smaller than unity to hold true. Finally, we investigate the phenomenological viability of the model by comparing it with the latest Planck and BICEP2/Keck-Array observational data. As we demonstrate, the model is compatible with the current observational data for a wide range of the free parameters of the model.