arXiv subjects

Maurice H. P. M. van Putten

Publications and source records attributed to Maurice H. P. M. van Putten.

At least 37 records · Page 2Linked to original sources

arXiv2022

Self-similar galaxy dynamics below the de Sitter scale of acceleration

Radial accelerations $α$ in galaxy dynamics are now observed over an extended range in redshift that includes model calculations on galactic distributions of cold dark matter (CDM) in $Λ$CDM. In a compilation of data of the {\em Spitzer} Photometry and Accurate Rotation Curves (SPARC) catalogue, the recent sample of Genzel et al.(2017) and the McMaster Unbiased Galaxy Simulations 2, we report on effective self-similarity in the variable $ζ= a_N/a_{dS}$, given by the Newtonian acceleration $a_N$ based on baryonic matter content over the de Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light and $H$ is the Hubble parameter. SPARC, MUG2 and theory satisfy ${a_N}/α \simeq 2.1\,ζ^\frac{1}{2}$ $(ζ<<1)$. At $ζ=1$ in transition to Newtonian gravity ($ζ>>1$), however, there is a $6σ$ gap between SPARC and MUGS2. This poses a novel challenge to CDM in $Λ$CDM against the apparent $C^0$ galaxy dynamics observed in SPARC. We attribute the latter to reduced inertia below the de Sitter scale of acceleration $(ζ< 1)$, based on a causality constraint imposed by the cosmological horizon ${\cal H}$.

astro-ph.GA↗

arXiv2022

Central engine of GRB170817A: Neutron star versus Kerr black hole based on multimessenger calorimetry and event timing

The central engine of GRB170817A post-merger to GW170817 is probed by GW-calorimetry and event timing, applied to a post-merger descending chirp which can potentially break the degeneracy in spin-down of a neutron star or black hole remnant by the relatively large energy reservoir in the angular momentum, $E_J$, of the latter according to the Kerr metric. This analysis derives from model-agnostic spectrograms with equal sensitivity to ascending and descending chirps generated by time-symmetric butterfly matched filtering. The sensitivity was calibrated by response curves generated by software injection experiments. The statistical significance for candidate emission from the central engine of GRB170817A is expressed by probabilities of false alarm (PFA; type I errors) derived from an event-timing analysis. PDFs were derived for start-time $t_s$, identified via high-resolution image analyses of the available spectrograms. For merged (H1,L1)-spectrograms of the LIGO detectors, a PFA $p_1$ derives from causality in $t_s$ given GW170817-GRB17081A. A statistically independent confirmation is presented in individual H1 and L1 analyses, in a second PFA $p_2$ of consistency in their respective observations of $t_s$. A combined PFA derives from their product since mean and (respectively) difference in timing are statistically independent. Applied to GW170817-GRB170817A, PFAs of event timing in $t_s$ produce $p_1=8.3\times 10^{-4}$ and $p_2=4.9\times 10^{-5}$ of a post-merger output ${\cal E}_{GW}\simeq 3.5\%M_\odot c^2$ ($p_1p_2=4.1\times 10^{-8}$, equivalent $Z$-score 5.48). ${\cal E}_{GW}$ exceeds $E_J$ of the hyper-massive neutron star in the immediate aftermath of GW170817, yet it is consistent with $E_J$ rejuvenated in delayed gravitational collapse to a Kerr black hole. Similar emission may be expected from energetic core-collapse supernovae producing black holes. (Abbr.)

astro-ph.HE↗

arXiv2022

On the mass-function of GWTC-2 binary black hole systems and their progenitors

The distribution of LIGO black hole binaries (BBH) shows an intermediate-mass range consistent with the Salpeter Initial Mass Function (IMF) in black hole formation by core-collapse supernovae, subject to preserving binary association. They are effectively parameterized by mean mass $μ$ with Pearson correlation coefficient $r = 0.93\,\pm\,0.06$ of secondary to primary masses with mean mass-ratio $\bar{q}\simeq 0.67$, $q=M_2/M_1$, consistent with the paucity of intermediate-mass X-ray binaries. The mass-function of LIGO BBHs is well-approximated by a broken power-law with a tail $μ\gtrsim 31.4M_\odot$ {in the mean binary mass $μ=\left(M_1+M_2\right)/2$}. Its power-law index $α_{B,true}=4.77\pm 0.73$ inferred from the tail of the observed mass-function is found to approach the upper bound $2α_S=4.7$ of the uncorrelated binary initial mass-function, defined by the Salpeter index $α_S=2.35$ of the Initial Mass Function of stars. The observed low scatter in BBH mass ratio $q$ evidences equalizing mass-transfer in binary evolution prior to BBH formation. At the progenitor redshift $z^\prime$, furthermore, the power-law index satisfies $α_B^\prime>α_B$ in a flat $Λ$CDM background cosmology. The bound $α_{B,true}^\prime \lesssim 2α_S$ hereby precludes early formation at arbitrarily high redshift $z^\prime \gg1$, that may be made more precise and robust with extended BBH surveys from upcoming LIGO O4-5 observations.

astro-ph.HE↗

arXiv2019

Prospects for multi-messenger extended emission from core-collapse supernovae in the Local Universe

Multi-messenger emissions from SN1987A and GW170817/GRB170817A suggest a Universe rife with multi-messenger transients associated with black holes and neutron stars. For LIGO-Virgo, soon to be joined by KAGRA, these observations promise unprecedented opportunities to probe the central engines of core-collapse supernovae (CC-SNe) and gamma-ray bursts. Compared to neutron stars, central engines powered by black hole-disk or torus systems may be of particular interest to multi-messenger observations by the relatively large energy reservoir $E_J$ of angular momentum, up to 29\% of total mass in the Kerr metric. These central engines are expected from relatively massive stellar progenitors and compact binary coalescence involving a neutron star. We review prospects of multi-messenger emission by catalytic conversion of $E_J$ by a non-axisymmetric disk or torus. Observational support for this radiation process is found in a recent identification of ${\cal E}\simeq (3.5\pm1)\%M_\odot c^2$ in Extended Emission to GW170817 at a significance of 4.2\,$σ$ concurrent with GRB170817A. A prospect on similar emissions from nearby CC-SNe justifies the need for all-sky blind searches of long duration bursts by heterogeneous computing.

astro-ph.HE↗

arXiv2019

Multi-messenger Extended Emission from the compact remnant in GW170817

GW170817/GRB170817A probably marks a double neutron star coalescence. Extended Emission $t_s\simeq (0.67\pm0.03)$\,s post-merger shows an estimated energy output ${\cal E}\simeq (3.5\pm1)\%M_\odot c^2$ determined by response curves to power-law signal injections, where $c$ is the velocity of light. It provides calorimetric evidence for a rotating black hole of $\sim 3M_\odot$, inheriting the angular momentum $J$ of the merged hyper-massive neutron star in the immediate aftermath of GW170817 following core-collapse about or prior to $t_s$. Core collapse greatly increases the central energy reservoir to $E_J\lesssim 1M_\odot c^2$, accounting for ${\cal E}$ even at modest efficiencies in radiating gravitational waves through a non axisymmetric thick torus. The associated multi-messenger output in ultra-relativistic outflows and sub-relativistic mass-ejecta is consistent with observational constraints from the GRB-afterglow emission of GRB170817A and accompanying kilonova.

astro-ph.HE↗

arXiv2019

On the stability of corotating and counter rotating P-type orbits around stellar binaries: a numerical study

We here revisit the essential problem of dynamical stability of planetary orbits around stellar binaries. We build on the coplanar three-body system of the Dvorak(1986), extending his stability diagram to both corotation and counter rotation of P-type orbits. His stability diagram express the change of stability across the gap between upper(UCO) and lower(LCO) critical orbits. By radius, this gap has a width of about 8$\%$ in the corotation case and 24$\%$ in the counter rotation case. As the gap of the second lies below the first, counter rotation is more stable, yet by width it is more chaotic. The gap between UCO and LCO follows a transition radius $r^+_g = 2.39 + 2.53e - 1.40 e^2$ and $r^-_g = 0.92 - 2.47e$ for corotation and respectively, counter rotation of the third body (the planet). Our $r^+_g$ agrees with the same of Dvorak to within 0.35$\%$. As a result, we discover $r^+_g/r^-_g \lesssim 2.57$ for all $e$. Around dim binaries, therefore, a relatively close in habitable zone may still be populated with planets on counter rotating orbits. The accurate numerical results presented here based on adaptive integration using MATLAB ODE45 may also serve as a novel benchmark of accurate \textit{N}-body integrators of exosolar systems more generally.

astro-ph.EP↗

arXiv2019

Global climate by Rossby number in the Solar system planets

On the largest scales, planetary climates can be described by their Rossby number (\textit{Ro}). \textit{Ro} is in response to $Gr/Re^2$ , where Gr is the Grashof number and Re is the Reynolds number. We here simplify $Gr/Re^2$ as h, where $h=H/H_{Earth}$ with $H=gP/(2πV_e)$ for a planet with surface gravity \textit{g}, rotation period \textit{P} and equatorial velocity V\textsubscript{e}. Unlike \textit{h}, \textit{Ro} is difficult to obtain because of a large diversity in observation. We perform on an in-depth literature search on average (av) and maximum (mx) wind velocity for each planet in the Solar system by various observational methods and by altitude. We explore a correlation between \textit{Ro} and \textit{h} expressed as a power law with index $α$ based on wind velocities of planets in the Solar system. We obtain a correlation between \textit{Ro} and \textit{h} with $α=0.56$ (av) and $α=0.52$ (mx). Earth's $H=H_{Earth}$ ($h=1$) is primarily due to lunar tidal interaction, given our relatively distant habitable zone (HZ) to the Sun. Our positive correlation, therefore, suggests exoplanet-moon systems as the `go-to-place' in our searches for potentially advanced life in exosolar system.

astro-ph.EP↗

arXiv2019

de Sitter Swampland, $H_0$ tension & observation

Realising de Sitter vacua in string theory is challenging. For this reason it has been conjectured that de Sitter vacua inhabit the Swampland of inconsistent low-energy effective theories coupled to gravity. Since de Sitter is an attractor for $Λ$CDM, the conjecture calls $Λ$CDM into question. Reality appears sympathetic to this idea as local measurements of the Hubble constant $H_0$ are also at odds with $Λ$CDM analysis of Planck data. This tension suggests that the de Sitter state is unstable, thereby implying a turning point in the Hubble parameter. We present a model relieving this tension, which predicts a turning at small positive redshift $z_*$ that is dictated by present-day matter density $ω_m$. This feature is easily identified by homogeneous surveys covering redshifts $z \leq 0.1$. We comment on the implications for the Swampland program.

hep-th↗

arXiv2018

Observational evidence for Extended Emission to GW170817

The recent LIGO event GW170817 is the merger of a double neutron star system with an associated short GRB170817A with $2.9\pm0.3$\,s soft emission over 8-70\,keV. This association has a Gaussian equivalent level of confidence of 5.1$σ$. The merger produced a hyper-massive neutron star of stellar mass black hole with prompt or continuous energy output powering GRB170817A. {Here, we report on a possible detection of} Extended Emission (EE) in gravitational radiation {\em during} GRB170817A: a descending chirp with characteristic time scale $τ_s=3.01\pm0.2\,$s in a (H1,L1)-spectrogram up to 700\,Hz with {Gaussian equivalent level of confidence greater than 3.3$σ$ based on causality alone following edge detection applied to (H1,L1)-spectrograms merged by frequency coincidences. Additional confidence derives from the strength of this EE.} The observed frequencies below 1kHz indicate a hyper-massive magnetar rather than a black hole, spinning down by magnetic winds and interactions with dynamical mass ejecta.

astro-ph.HE↗

arXiv2018

GPU-accelerated broadband analysis of multi-messenger GRB light curves

High-frequency multi-messenger observations provide a powerful probe of gamma-ray bursts (GRBs), pioneered by {\em BeppoSAX} in gamma-rays and LIGO-Virgo in gravitational waves. Identifying the central engines - magnetars or black holes - also promises to improve on GRBs as probes of cosmological evolution. THESEUS' design is ideally suited to pursue both science objectives. Here, we present a general-purpose {\em graphics processor units} (GPU)-accelerated broadband search algorithm for long duration ascending and descending chirps, post-merger or from core-collapse of massive stars, in electromagnetic and gravitational radiation. It implements butterfly filtering using banks of up to 8 million templates of 1 second duration at over one million correlations per second by heterogeneous computing using a dozen high-end GPUs. We demonstrate its application with the identification of broadband Kolmogorov spectra in long GRBs and the long duration ascending chirp in the merger GW170817. The first shows a noticeable absence of a high frequency bump, otherwise expected from newly formed magnetar central engines. The second illustrates the need for deep searches to identify GRB central engines in descending chirps in gravitational waves, post-merger or from nearby energetic core-collapse supernovae. A future catalogue of THESEUS' GRBs covering a broad range of redshifts may probe the nature of the cosmological vacuum and establish the de Sitter limit as a turning point in cosmological evolution.

astro-ph.IM↗

arXiv2017

Accelerated cosmological expansion without tension in the Hubble parameter

The $H_0$-tension problem poses a confrontation of dark energy driving late-time cosmological expansion measured by the Hubble parameter $H(z)$ over an extended range of redshifts $z$. Distinct values $H_0\simeq 73$ km\,s$^{-1}$Mpc$^{-1}$ and $H_0\simeq 68$ km\,s$^{-1}$Mpc$^{-1}$ obtain from surveys of the Local Universe and, respectively, $Λ$CBM analysis of the CMB. These are representative of accelerated expansion with $H^\prime(0)\simeq0$ by $Λ=ω_0^2$ and, respectively, $H^\prime(0)>0$ in $Λ$CDM, where $ω_0=\sqrt{1-q}H$ is a fundamental frequency of the cosmological horizon in a Friedmann-Robertson-Walker universe with deceleration parameter $q(z)=-1+(1+z)H^{-1}H^\prime(z)$. Explicit solutions $H(z)=H_0\sqrt{1+ω_m(6z+12z^2+12z^3+6z^4+(6/5)z^5)}$ and, respectively, $H(z)=H_0\sqrt{1-ω_m+ω_m(1+z)^3}$ are here compared with recent data on $H(z)$ over $0\lesssim z \lesssim2$. The first is found to be free of tension with $H_0$ from local surveys, while the latter is disfavored at $2.7σ$. A further confrontation obtains in galaxy dynamics by a finite sensitivity of inertia to background cosmology in weak gravity, putting an upper bound of $m\lesssim 10^{-30}$eV on the mass of dark matter. A $C^0$ onset to weak gravity at the de Sitter scale of acceleration $a_{dS}=cH(z)$, where $c$ denotes the velocity of light, can be seen in galaxy rotation curves covering $0\lesssim z \lesssim 2$. Weak gravity in galaxy dynamics hereby provides a proxy for cosmological evolution.

astro-ph.CO↗

arXiv2017

Evidence for galaxy dynamics tracing background cosmology below the de Sitter scale of acceleration

Galaxy dynamics probes weak gravity at accelerations below the de Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light and $H$ is the Hubble parameter. Low and high redshift galaxies hereby offer a novel probe of weak gravity in an evolving cosmology, satisfying $H(z)=H_0\sqrt{1+ω_m(6z+12z^2+12z^3+6z^4+(6/5)z^5)}/(1+z)$ with baryonic matter content $ω_m$ sans tension to $H_0$ in surveys of the Local Universe. Galaxy rotation curves show anomalous galaxy dynamics in weak gravity $a_N<a_{dS}$ across a transition radius $r_t = 4.7\,\mbox{kpc}\,M_{11}^{1/2}(H_0/H)^\frac{1}{2}$ in galaxies of mass $M=10^{11}M_\odot M_{11}$, where $a_N$ is the Newtonian acceleration based on baryonic matter content. We identify this behavior with a holographic origin of inertia from entanglement entropy, that introduces a $C^0$ onset across $a_N=a_{dS}$ with asymptotic behavior described by a Milgrom parameter satisfying $a_0=ω_0/2π$, where $ω_0=\sqrt{1-q}H$ is a fundamental eigenfrequency of the cosmological horizon. Extending an earlier confrontation with data covering $0.003\lesssim a_N/a_{dS}\lesssim1$ at redshift $z\sim0$ in Lellie et al. (2016), the modest anomalous behavior in the Genzel et al. sample at redshifts $0.854\le z\le 2.282$ is found to be mostly due to clustering $0.36\lesssim a_N/a_{dS}\lesssim1$ close to the $C^0$ onset to weak gravity and an increase of up to 65\% in $a_0$.

astro-ph.GA↗

arXiv2017

Deep searches for broadband extended gravitational-wave emission bursts by heterogeneous computing

We present a heterogeneous search algorithm for broadband extended gravitational-wave emission (BEGE), expected from gamma-ray bursts and energetic core-collapse supernovae. It searches the $(f,\dot{f})$-plane for long duration bursts by inner engines slowly exhausting their energy reservoir by matched filtering on a {\em Graphics Processor Unit} (GPU) over a template bank of millions of one-second duration chirps. Parseval's Theorem is used to predict the standard deviation $σ$ of filter output, taking advantage of near-Gaussian noise in LIGO S6 data over 350-2000 Hz. Tails exceeding a mulitple of $σ$ are communicated back to a {\em Central Processing Unit} (CPU). This algorithm attains about 65\% efficiency overall, normalized to the Fast Fourier Transform (FFT). At about one million correlations per second over data segments of 16 s duration $(N=2^{16}$ samples), better than real-time analysis is achieved on a cluster of about a dozen GPUs. We demonstrate its application to the capture of high frequency hardware LIGO injections. This algorithm serves as a starting point for deep all-sky searches in both archive data and real-time analysis in current observational runs.

astro-ph.IM↗

arXiv2017

Galaxy rotation curves and the deceleration parameter in weak gravity

We present a theory of weak gravity parameterized by a fundamental frequency $ω_0 = \sqrt{1-q}H$ of the cosmoloogical horizon, where $H$ and $q$ denote the Hubble and, respectively, deceleration parameter. It predicts (i) a $C^0$ onset to weak gravity across accelerations $α= a_{dS}$ in galaxy rotation curves, where $a_{dS}=cH$ denotes the de Sitter acceleration with velocity of light $c$, and (ii) fast evolution $Q(z)=dq(z)/dz$ of the deceleration parameter by $Λ=ω_0^2$ satisfying $Q_0>2.5$, $Q_0=Q(0)$, distinct from $Q_0\lesssim1$ in $Λ$CDM. The first is identified in high resolution data of Lellie et al.(2017), the second in heterogeneous data on $H(z)$ over $0<z<2$. A model-independent cubic fit in the second rules out $Λ$CDM by $4.35σ$ and obtains $H_0=74.0\pm 2.2$ km s$^{-1}$ Mpc$^{-1}$ consistent with Riess et al. (2016). Comments on possible experimental tests by the LISA Pathfinder are included.

gr-qc↗

arXiv2016

New estimates of the deceleration parameter in weak gravity

We consider weak gravity at accelerations $α 2.5$) versus $Λ$CDM ($Q_0<1$).

astro-ph.CO↗

arXiv2016

On the origin of exponential growth in induced earthquakes in Groningen

The Groningen gas field shows exponential growth in earthquakes event counts around a magnitude M1 with a doubling time of 6-9 years since 2001. This behavior is identified with dimensionless curvature in land subsidence, which has been evolving at a constant rate over the last few decades {essentially uncorrelated to gas production.} We demonstrate our mechanism by a tabletop crack formation experiment. The observed skewed distribution of event magnitudes is matched by that of maxima of event clusters with a normal distribution. It predicts about one event $<$\,M5 per day in 2025, pointing to increasing stress to human living conditions.

physics.geo-ph↗

arXiv2016

On extreme transient events from rotating black holes and their gravitational wave emission

The super-luminous object ASASSN-15lh (SN2015L) is an extreme event with a total energy $E_{rad}\simeq 1.1\times 10^{52}$ erg in black body radiation on par with its kinetic energy $E_k$ in ejecta and a late time plateau in the UV, that defies a nuclear origin. It likely presents a new explosion mechanism for hydrogen-deprived supernovae. With no radio emission and no H-rich environment we propose to identify $E_{rad}$ with dissipation of a baryon-poor outflow in the optically thick remnant stellar envelope produced by a central engine. By negligible time scales of light crossing and radiative cooling of the envelope, SN2015L's light curve closely tracks the evolution of this engine. We here model its light curve by the evolution of black hole spin, during angular momentum loss in Alvén waves to matter at the Inner Most Stable Circular Orbit (ISCO). The duration is determined by $σ=M_T/M$ of the torus mass $M_T$ around the black hole of mass $M$: $σ\sim 10^{-7}$ and $σ\sim 10^{-2}$ for SN2015L and, respectively, a long GRB. The observed electromagnetic radiation herein represents a minor output of the rotational energy $E_{rot}$ of the black hole, while most is radiated unseen in gravitational radiation. This model explains the high-mass slow-spin binary progenitor of GWB150914, as the remnant of two CC-SNe in an intra-day binary of two massive stars. This model rigorously predicts a change in magnitude $Δm\simeq 1.15$ in the light curve post-peak, in agreement with the light curve of SN2015L with no fine-tuning.

astro-ph.HE↗

arXiv2016

Scaling in global tidal dissipation of the Earth-Moon system

The Moon migrated to $r_{\leftmoon}\simeq3.8\times10^{10}$ cm over a characteristic time $r/v=10^{10}$ Gyr by tidal interaction with the Earth's oceans at a present velocity of $v=3.8$ cm yr$^{-1}$. We derive scaling of global dissipation that covers the entire history over the past 4.52 Gyr. Off-resonance tidal interactions at relatively short tidal periods in the past reveal the need for scaling {with amplitude}. The global properties of the complex spatio-temporal dynamics and dissipation in broad spectrum ocean waves is modeled by damping $ε= h F/(2Q_0)$, where $h$ is the tidal wave amplitude, $F$ is the tidal frequency, and $Q_0$ is the $Q$-factor at the present time. It satisfies $Q_0\simeq 14$ for consistency of migration time and age of the Moon consistent with observations for a near-resonance state today. It shows a startingly fast eviction of the Moon from an unstable near-synchronous orbit close to the Roche limit, probably in a protolunar disk. Rapid spin down of the Earth from an intial $\sim30\%$ of break-up by the Moon favored early formation of a clement global climate. Our theory suggests moons may be similarly advantageous to potentially habitable exoplanets.

astro-ph.EP↗