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Slava G. Turyshev

Publications and source records attributed to Slava G. Turyshev.

At least 19 recordsLinked to original sources

Finite-amplitude establishment beyond local invasion in cooperative chemical networks

Local kinetic exponents and next-generation radii diagnose infinitesimal invasion, but they need not determine whether a nonlinear organized state is accessible. Motivated by the kinetic component of Gate~7 in a twelve-gate nonequilibrium framework, we study cooperative networks whose productive linearization contains no closed cycle. We prove that an acyclic productive Jacobian has $R=0$ and $λ_{\rm kin}=-\min_i d_i<0$ for every drive, while a nonlinear return path can create a stable finite-amplitude branch through a saddle-node. In a canonical catalyst--assembly model, the saddle's stable manifold---not a threshold in either concentration---is the deterministic establishment boundary, so equal-abundance seeds of different composition can have opposite outcomes. At finite copy number, establishment becomes a committor and first-passage problem. For a benchmark protocol with $Γ=2$, $Ω=16$, $η=0.02$, and horizon $T=1000$, density-Hill and pair-count generators give first-entrance probabilities $0.633$ and $0.339$; their interpolated half-success drives are $1.900$ and $2.148$, an approximately $13.1\%$ shift. The associated constant-source deterministic system retains a stable low state, so these transitions are fluctuation- and discrete-arrival-enabled. The finite-amplitude regime is not confined to exact acyclicity: a weak linear return leaves a finite interval with $0<R<1$, $λ_{\rm kin}<0$, and bistability. A general cooperative-return criterion separates the superlinear local condition from the global return-profile structure required for a fold. The resulting hierarchy of branch existence, basin accessibility, and finite-time stochastic establishment replaces a single onset threshold by a protocol-dependent kinetic criterion.

physics.gen-ph↗

An Information-Thermodynamic Accounting Framework for Planetary Biosphere Productivity

Planetary primary producers use stellar or internally generated free energy to maintain biomass and produce new material. We formulate the associated productivity ceiling while separating environmental losses, basal maintenance, retained biomass energy and net dissipation from heritable copying. Maintenance copy-reset cycles and copies retained in new biomass have distinct thermodynamic costs. For a specified feasible producer population, the normalized ceiling is $(1-x_0)/(1+q)$, where $x_0$ is the baseline copying fraction and $q$ is the growth-associated copying cost relative to other production costs. Exact interval bounds and global sensitivity analyses quantify both effects without assigning empirical probabilities to unmeasured biological parameters. Observation-constrained planetary resources and strain-matched genome and cellular-carbon measurements provide separate physical and biological benchmarks. For the two mean inventories, a 10\% growth-copying correction requires an effective copying cost $e_gχ$ about 63--84 times a published DNA fuel benchmark at unit production efficiency; the benchmark is not a measured dissipation cost. We also show that partitioning an already measured total maintenance budget cannot change the absolute productivity ceiling, and that population adjustment can preserve information-load fractions as supply falls. The framework provides conditional feasibility tests, inverse thresholds and measurement priorities, rather than a calibrated prediction of extraterrestrial productivity.

physics.bio-ph↗

A Covariance-Aware Framework for Spatially Resolved Exoplanet Biosignature Inference with the Solar Gravitational Lens

Assessing possible life on an exoplanet requires spatial, spectral, temporal, and environmental context. We develop a covariance-aware Solar Gravitational Lens (SGL) framework for regional biosignature inference from reconstructed Einstein-ring measurements. A controlled 0.45-2.40 um Stokes-$I$ experiment uses ten illuminated cells, 128 channels, and R=70 to compare resolved and exactly projected disk spectra with common parameters and priors. Across 96 synthetic scenes, the joint gas, vegetation, and mineral block gains (1.52+/-0.03) nats after marginalizing cloud and calibration/response parameters; adding independently trained surrogate-discrepancy covariance gives (1.49+/-0.03) nats. Held-out mismatch nevertheless produces linearized shifts up to 6.08 posterior standard deviations; preserved precision does not establish unbiased recovery or evidence for life. For fixed Gaussian hypotheses, the expected log-likelihood-ratio loss under disk integration equals half the squared whitened contrast discarded by the projection. A separate 0.40-20 um continuum calculation provides absolute photon rates and observing-time estimates for an Earth-radius planet at 30 pc, observed from 650 AU. It includes source-averaged SGL amplification, finite-aperture extraction, coronal and host-star photons, detector noise, and a declared calibration floor. A reconstruction-covariance bracket reduces an 8 x 8 coadd gain from 7.77 to 3.00, costing 6.7 times the exposure in the statistical-noise limit. The framework connects regional spectroscopy and co-location tests to the physical and instrumental validation needed to assess exoplanet biospheres and possible biological activity.

astro-ph.IM↗

An Analytic Error-Budget Model for the Habitable Worlds Observatory Coronagraph: From Optical Disturbances to Flux-Ratio Noise

A coronagraph stability allocation must protect a planet measurement, not merely satisfy a contrast target. Residual starlight both generates photon noise and interferes with small field perturbations, coupling optical stability to detection reliability. We develop a modular analytic model for the Habitable Worlds Observatory (HWO), using a reduced two-roll angular-differential-imaging realization of its OS-1 scenario. Complex-field sensitivities, wavefront sensing/control, finite observing windows, polarization, detector calibration are propagated to flux-ratio noise (FRN) and detection probabilities. Joint-visit Gaussian quadratic moments retain differential bias, cross covariance; spatial overlap/field phase determine which disturbances resemble a planet. A 6-m, 500-nm benchmark shows why the science test must precede category allocation. For a 115.46-parts-per-trillion (ppt) quadrature planet, 30,000 independent Gaussian search statistics, and a $10^{-3}$ family-wise false-alarm objective, 20-ppt FRN gives 64.55% conditional detection power; 99% requires 14.94 ppt. Photon and calibration noise exhaust the optical remainder at 8.11 pc in 100 h under the fixed response, so tighter stability alone cannot restore feasibility. An unrecognized 1% high-variance component carrying twenty percent of the variance tightens the modal allowance by a factor of 2.88; an ideal, exactly known state label reduces that penalty to 1.29 under equal conditional false-alarm limits and the same average-power objective. Thus, requirements depend on both the optical response and the information retained by the observing protocol. The framework identifies when suppression, stability, calibration, or state monitoring addresses the limiting mechanism. Numerical tolerances are controlled model results; flight allocation requires architecture-specific responses and calibrated disturbance state-estimation laws.

astro-ph.IM↗

Wavefront-Conditioned Photon Measurements for Exoplanet Spectroscopy: Contrast Limits and Conditional Gains

A wavefront-sensor (WFS) prediction can select the photon measurement before detection or condition its likelihood afterward. This matters for reflected-light spectra requiring hundreds of hours, because subtracting residual starlight cannot remove its photon noise. In a two-mode, low-occupation model, isotropically distributed leakage makes planet-mode projection---ideal single-mode injection matched to the planet---the optimal fixed single-photon measurement, including unequal aligned backgrounds and equal Poisson detector-event rates per output. For nonzero leakage, an attainable two-output conditioned measurement is optimal and strictly more informative before differential loss. For an isotropic background, a contrast bound holds for any distribution of recorded leakage directions: relative transmission $0.80$ and relative admitted-time duty $0.90$ limit the Fisher information per scheduled time to $0.81$ of the fixed optimum at equal predictable-leakage and planet contrasts. Haar averaging sharpens this ceiling to $0.78$. The necessary leakage-to-planet ratios for gain are approximately $2.25$ for any direction law and $3.26$ for Haar directions. A concentration-model certificate identifies directional diversity sufficient to beat recalibrated fixed measurements. Independently gated fixed-basis fallback guarantees no loss of continuum-profiled spectral information when rates and costs are known. For the Habitable Worlds Observatory, the candidate regime is predictable, directionally diverse, leakage-dominated residuals, not a general sensitivity improvement.

astro-ph.IM↗

High-Precision Relativistic Time Scales for Mars Surface and Orbital Clocks

We develop a Mars-centered post-Newtonian framework for relating barycentric coordinate time, Mars-centered coordinate time, a conventional Mars surface time scale, and the proper times of landed and orbiting clocks. The construction follows the International Astronomical Union BCRS/TCB formalism, introduces Areocentric Coordinate Time (TCA), and writes each clock transformation as a secular rate plus zero-mean periodic terms. Terms are retained when their fractional-frequency amplitude exceeds 5e-18 or their one-way accumulated timing amplitude exceeds 0.1 ps. The numerical realization uses the GMM-3 Mars gravity field through degree and order 120, point-mass tides from the Sun, Phobos, and Deimos with origin and dipole terms removed, and bounds on omitted local c^-4 and external-perturber terms. Representative low-Mars-orbit, areostationary, Phobos-/Deimos-distance, and highly elliptical relay regimes are evaluated. Relative to the adopted Mars surface scale, a 300 km near-polar clock is slower by 4.56 microseconds per day, while areostationary and Deimos-distance clocks are faster by 9.13 and 9.52 microseconds per day. The leading Mars-J2 timing line is about 87 ps at 300 km altitude and remains several ps near areostationary radius for inclined or librating areosynchronous cases; perihelion-scaled solar tides become retained sub-ps terms in high relay orbits. The result is a reference-system and model-retention framework, not a final operational Mars Time Ephemeris. A realized sub-ps system still requires a selected planetary ephemeris, Mars orientation and seasonal-gravity model, spacecraft orbit determination, calibrated link delays, and covariance analysis. Time-variable low-degree gravity from seasonal CO2 exchange is a leading surface-realization term and must be modeled, monitored, or empirically bounded before sub-ps Mars surface-scale claims are made.

gr-qc↗

Sustained Habitation Beyond Earth: Health, Recovery, and Renewal

Establishing a lasting human settlement beyond Earth requires a habitable destination at arrival and sustained renewal of its population/infrastructure. We compare Earth delivery, robotic predeployment, local resource processing, localized manufacture under coupled protection, power, recovery, health requirements. In a 1,000-resident case, specific retention times and 1% annual growth require ~1.8 tonnes of equipment replacement/expansion per resident-year. Local manufacture raises mean site electricity from 11.8 to 19.5 MW; the declared retention range gives 17-26 MW at fixed processing intensity. A separate 100-ton/year pilot reduces 10-year deliveries from 1,000 to 419 tonnes after a 3-year commissioning ramp, while retaining imported inputs. Local production thus reduces freight by adding maintained capacity at the destination. Receiving capacity is bounded by replacement-adjusted supply, not passenger throughput. Published Martian transport gives ~63,000 tonnes of planar cover per hectare for the selected 10-mSv/year GCR allocation; Earth-like acceleration at 2~rpm requires a 224-m rotation radius. These scales favor local shielding and modular rotating habitats. Repeated 10-day wastewater outages every 35 days require capacity at least 1.4 times inflow; storage cannot correct a persistent deficit. Existing evidence leaves lifelong partial-gravity, mixed-field radiation responses, gestation, development and subsequent fertility unresolved. With sustained investment, recoverable habitats, resource pilots, controlled-gravity investigations are credible 10-20-year objectives; broad industrial renewal requires multidecade development. Earth-supported habitation is a credible development path. Independent population continuity requires demonstrated health, recovery, demographic resilience, essential-product renewal within one exposure/resource history; its completion cannot yet be dated.

physics.gen-ph↗

Sector-Resolved Bayesian Model Averaging for DESI-Era Cosmology

We present a quotient-space Bayesian formulation for DESI-era anomaly interpretation. Given a pattern-labeled catalog with map \(i\mapsto \Act(i)\), the induced posterior \(p(\Act\mid D)\), sector inclusion probabilities \(P_α\), co-activation probabilities \(P_{αβ}\), and grouped Bayes factors \(B_α(D)\) are exact summaries over predeclared physical activation events. Pairwise comparisons such as \(\lcdm\) versus \(\wacdm\) remain ordinary Bayes-factor tests between specified families; the quotient construction addresses the coarser question of which physical sector carries posterior support when different sectors are represented by unequal numbers of catalog elements. We derive a sector-resolved DESI-CMB-SN likelihood specification for late-time background, early-time ruler, supernova calibration, perturbation, and gravitational-wave propagation sectors. The construction includes an Alcock-Paczynski/isotropic-scale BAO decomposition, a pure-ruler projection, analytic marginalization of low-rank supernova calibration modes, Fisher-normalized sector priors, inactive-sector leakage tests, log-evidence uncertainty propagation, and prior/sector-partition diagnostics. The result is a quantitative procedure for reporting model-comparison support at the level of physically interpretable sectors.

physics.gen-ph↗

High-Power AM-CW Lunar Laser Ranging as a $μ$Hz SGWB Detector

High-power amplitude-modulated continuous-wave lunar laser ranging (AM-CW LLR) is a stochastic-gravitational-wave-background (SGWB) experiment that measures GW-driven drift and diffusion of the Earth--Moon orbit. Its observable is the coherent phase of a GHz modulation envelope returned by an individually resolved single hollow corner-cube retroreflector (HCCR), converted to absolute range and analyzed through its time-dependent mean and covariance. The response occurs at lunar orbital harmonics; the dominant low-eccentricity channel is centered at $f_2=0.847245\,μ{\rm Hz}$, and a five-year broadband forecast applies to spectra smooth over the resolution scale $T_{\rm obs}^{-1}=6.34\,$nHz about that resonance. A scalar 1-kW, 1064-nm link yields $5.893\times10^3$ detected photons s$^{-1}$ and an $88.8$--$124.3\,μ$m photon contribution in 100 s, while the forecasts adopt projected total range precisions of $80$ and $50\,μ$m. In the covariance-dominated weak-signal regime, $Ω_{\rm gw}^{95}\proptoσ_R^2\nuEff^{-1}T_{\rm obs}^{-4}$. Using the published Earth--Moon response normalization, the five-year 95\% thresholds are $1.86\times10^{-7}\Dtot$ for $80\,μ$m and $500\,{\rm yr}^{-1}$ and $2.42\times10^{-8}\Dtot$ for $50\,μ$m and $1500\,{\rm yr}^{-1}$, where $\Dtot$ is the full-analysis threshold divided by the unit-factor response-anchored forecast. If end-to-end calibration, sampling, and marginalization give $\Dtot\le1.15$, the higher-performance campaign reaches nominal source-statistic equality for $Ω_{\rm gw}=7.08\times10^{-8}$ in five years. These measurable performance and information-retention requirements define high-power AM-CW LLR as a standalone quantitative SGWB experiment at the $0.85\,μ{\rm Hz}$ Earth--Moon resonance.

gr-qc↗

Do Quantum Measurement Advantages Survive to Astrophysical Inference? Seven Benchmarks in Optical Interferometry and Imaging

Quantum techniques matter to optical astronomy when they preserve information in the parameter-bearing measurement channel after realistic loss, calibration, covariance, and inference are propagated to the final astrophysical observable. We compare 7 approaches by the quantity they change: internal optical-path delay, sub-Rayleigh source separation, coronagraphic planet throughput & stellar leakage, coherent field quadratures, nonlocal complex visibility, null depth, active phase sensing. In an Earth-analog astrometry case, 6-dB squeezed internal metrology improves the measured phase quadrature by 1.58 and the complete readout by ~1.20, but fixed-time planet-mass precision by only 1.010 (95 % interval 1.005-1.045); mission duration, useful baseline, cadence, calibration have greater modeled leverage. For a close young binary, signed spatial-mode demultiplexing preserves sub-Rayleigh orbital information that is substantially degraded in the tested direct-imaging comparator. A representative matched-model calculation gives a dynamical-mass RMSE gain 1.77 1.47-2.15). For illustrative equal-prior pre-main-sequence predictions at 0.10 and \(0.12M_\odot\), mass precisions of 15%, 10%, 7% correspond to correct-selection probabilities of ~73%, 82%, 90%. The numerical gain remains provisional because the event-level continuous-image comparator, strict tail convergence, externally measured broadband transfer matrix, and finite-photon calibration are not yet closed. Modal coronagraphy and quantum-enhanced heterodyne reception define conditional receiver opportunities, while the nonlocal, nuller, and prepared-NOON cases identify physical bottlenecks that prevent an astrophysical advantage in the stated configurations. The common result is that quantum technology is most valuable when it changes an information-bearing observable and that channel remains consequential in the final science measurement.

physics.gen-ph↗

Operations, Maintenance, and Industrial Scaling of MW-Class Orbital Data Centers

Megawatt-class orbital data centers require continuous maintenance, replacement, inventory, and service capacity in addition to spacecraft power/thermal systems. We formulate an analytical lifecycle framework for permanent/transient failures, modular orbital replacement units, robotic servicing, spare inventory, scheduled technology refresh, correlated faults, cybersecurity, optional human support. The model combines nonhomogeneous component hazards, capacity-weighted availability, multiclass robotic-service capacity, Poisson base-stock inventory, replacement-flow accounting, human-support break-even relations. For a 1 MW cluster with 10 active 100 kW nodes, 1 reserve node, ~200 5 kW compute cartridges, low, nominal, high deployed-mass allocations span ~50-75 kg/kW. Assumptions yield 70.2 random or life-limited interventions and 323-349 planned refresh operations/(MW-year), for a total of 393-419 standardized operations/(MW-year). Analysis gives a first-generation logistics of 5.3-9.0 t/(MW-year), with a nominal case of ~ 6.6 t/(MW year), 560-700 productive robot-hors/(MW-year). Planned refresh exceeds random replacement under the stated component populations, hazards, 3-15-year intervals. At ~400 standardized operations/(MW-year), the post-internal-recovery exception probability is <$10^{-3}$, with an objective near $10^{-4}$ at large scale; terminal non-recovery $p_U$ requires a smaller mission-level allocation. The target catastrophic-loss hazard for a 100 kW node is 0.01-0.03 1/yr. Parametric workload and cost cases place contingency visits at 10s of MWs, periodic campaigns at 10-100s of MWs, dedicated personnel at several 100 MWs to GWs. The reference first deployment is uncrewed, autonomously fault-managed, robotically maintainable, supported by specific inventory based on a 6-month replenishment horizon, compatible with later human access without permanent habitation.

physics.gen-ph↗

Quantum Technologies: System-Level Performance and Validation Priorities

Performance claims in quantum technology are not properties of hardware alone. They are properties of a declared task, system boundary, normalization denominator, uncertainty or security convention, and comparator. We perform a cross-domain analysis spanning quantum computing, simulation, communication, sensing, clocks, randomness generation, and their enabling technologies. The analysis changes substantive conclusions in several representative cases. For the longest direct finite-key quantum key distribution case analyzed here, the same final key gives rates differing by a factor of $1.91$ when normalized by complete acquisition rather than transmission-active time. In Advanced LIGO, $6.1\,\mathrm{dB}$ peak quantum-noise reduction coexists with a $0.534$ coincident analysis-ready fraction, separating detector-level gain from delivered observing service. In quantum computation and photonic sampling, matching the observable, error tolerance, loss model, sample count, amortization, and classical hardware moves or reverses published crossover claims. Across domains, the recurring limits are correlated error, multiplicative interface loss, thermal and nonequilibrium occupation, calibration covariance, measurement efficiency, fabrication yield, and control latency. A quantum advantage is therefore established only for a fixed task and boundary when the accepted output outperforms the best documented alternative at matched accuracy, elapsed time, availability, and lifecycle cost. The resulting framework identifies the measurements required to convert component records into reproducible system capability. Credible progress is defined by reproduced logical workloads, prospectively validated simulations, repeater links outperforming direct transmission, long-duration calibrated sensors and clocks, integrated hardware with predictable yield and reliability.

physics.gen-ph↗

Relativistic framework for high-precision GNSS processing in GCRS/BCRS with extension to cislunar space

We present an implementation-oriented relativistic modeling framework for high-precision {\tt GNSS} processing consistent with the IAU-adopted Barycentric and Geocentric Celestial Reference Systems (BCRS/GCRS) and their associated time scales (TCB/TDB and TCG/TT). We derive explicit ${\cal O}(c^{-2})$ transformations for position, velocity, and acceleration between TT-compatible GCRS quantities and TDB-compatible BCRS quantities, and provide screened operational forms with conservative remainder bounds that quantify state-map truncation errors for cm-class orbit modeling. For $10^{-16}$-class fractional-frequency transfer, the ${\cal O}(c^{-4})$ clock-rate terms identified below must be retained or explicitly included in the observable error budget. We implement a BCRS-native processing option in JPL's GipsyX and verify it internally via a 24~h round-trip GCRS$\rightarrow$BCRS$\rightarrow$GCRS propagation-and-transform closure test at the few-mm level, demonstrating consistency of the implemented dynamical model and state transformations under matched force-model assumptions. To support emerging Earth--Moon applications, we define a Lunicentric Celestial Reference System (LCRS), its coordinate time (TCL), and a scaled lunar-surface time (TL), and specify a minimal near-rectilinear halo orbit (NRHO)-like regression test that exercises the BCRS$\leftrightarrow$LCRS transformation chain together with the 1PN barycentric light-time model. End-to-end cislunar navigation performance additionally depends on signal availability and estimation strategy; the present work provides the relativistic reference-frame and time-transfer infrastructure needed to model observables at the centimeter and tens-of-picoseconds level.

gr-qc↗

Optical Ground Stations for Space Communications:Systems Engineering, Availability, and Service Economics Through 2030

Optical ground stations (OGSs) are becoming networked infrastructure for high-rate space-to-Earth communications, but their adoption is governed by service availability and utilization as much as by optical line rate. This paper develops a systems-engineering and service-economics assessment of the OGS sector as of June~2026. The analysis combines public flight demonstrations and operational records with scalar link-budget, availability, and cost-normalization models. Public benchmarks span 25 Mbps from interplanetary range, 260 Mbps-class lunar links, 1.2 Gbps-class ISS relay, 1.8 Gbps operational GEO relay, 120 Gbps-class direct-to-ground demonstrations in China, and 200 Gbps from LEO in NASA's TBIRD mission. The resulting conclusion is that the bottleneck has shifted from peak line rate to repeatable service under weather, acquisition, scheduling, and operations constraints. Under one explicit planning normalization - a 10 Gbps near-Earth station, annualized cost of \$2 million/year, scheduled pre-weather optical contact time of 0.5 h/day, and weather-inclusive combined efficiency $η=0.7$ - the fixed-cost component is of order $(3-4)\times10^{3}$ USD/TB. This number is a sensitivity anchor, not a tariff forecast; the controlling variables are duty factor, effective weather diversity, shared-network loading, and service-level allocation. The public industrial evidence is best interpreted as a stratified value chain, not as a single vendor ranking. The defensible 2030 baseline is hybrid optical+radio-frequency (RF): optical for throughput, relay, and spectrum relief; RF for continuity, contingency, and assured command paths.

eess.SP↗

Ultra-High-Resolution Astronomy with the Solar Gravitational Lens

The solar gravitational lens (SGL) is a target-specific observatory: the Sun supplies the wave-optical element, while spacecraft provide occultation, annular photometry, sampling, metrology, and inverse reconstruction. We develop an observability framework for non-exoplanet SGL astronomy. Viability is set by image-plane scale, raster pitch, finite-source gain, source-to-background ratio, temporal coherence, PSF knowledge, calibration, metrology, and focal-line access. We separate the vector Poisson measurement operator from the scalar convolution used for benchmarks. Four analytic scenes are propagated and reconstructed: a solar analog and magnetic white dwarf at 10 pc, an M87*-scale millimeter ring/jet source, and a bright 0.1 AU protoplanetary subfield at 140 pc. Under stated kernel-mismatch, background, calibration-floor, support-mask, sampling, regularization, and imposed information-floor assumptions, the scalar reconstructions give SSIM values of 0.993, 0.918, 0.973, and 0.923. These metrics quantify scalar inverse conditioning, not delivered flight performance; FRC50, support-leakage, and information-floor sensitivity diagnostics expose the dependence on assumptions. Many self-luminous compact targets are not photon-starved relative to a reflected-light exo-Earth reference, shifting the dominant requirements to ring extraction, coronal subtraction, detector dynamic range, PSF knowledge, cadence, spectroscopy, metrology, scan overhead, and access. The strongest bounded cases are white-dwarf surface and magnetic mapping, nearby stellar surfaces, compact AGN/black-hole structure with long-wavelength instrumentation, velocity-resolved broad-line-region mapping, and planet-forming subfields. The priority enabling program is SGL transfer-function characterization: measuring solar-multipole, plasma, extended-Sun, and instrumental response needed for scientifically interpretable imaging.

astro-ph.IM↗

Gravitational lensing for interstellar power transmission

We investigate the propagation of monochromatic electromagnetic waves through multiple, well-separated, monopole gravitational lenses in the thin-lens/eikonal approximation. For the axially aligned transmitter--lens(es)--receiver geometry, the relevant diffraction integrals can be evaluated analytically, yielding closed-form expressions for the point-spread function (PSF) and for the aperture-averaged gain. A single gravitational lens can enhance transmission when it is used either at the transmitting end or at the receiving end. For a two-lens link, the second lens focuses the signal into a much smaller diffraction pattern; however, for optical wavelengths and metre-scale receiving apertures this fine structure is aperture-averaged, and the averaged additional gain becomes independent of the second lens mass. We estimate photon rates and shot-noise-limited SNRs for these idealized configurations. The results indicate that gravitational lensing can in principle support high-SNR interstellar optical power links, subject to stringent alignment, finite-aperture, transmitter-beam, and coronal-background assumptions.

gr-qc↗

Direct High-Resolution Imaging of Earth-like Exoplanets with the Solar Gravitational Lens

We present a scalar, aperture-averaged observability benchmark for resolved exoplanet imaging with the solar gravitational lens (SGL). A real Earth luminance map is propagated through a scanned SGL image plane using source-to-image-plane compression, a finite-aperture SGL kernel, and an Einstein-ring photon-count model. We inject photon noise, finite-exposure smear, cloud-like temporal variability, coronal and detector-calibration residuals, optical-operator mismatch, and navigation error, then reconstruct with a regularized Fourier/Wiener inverse. For an Earth-radius planet at 30 pc observed from 650 AU with a 1 m telescope, the projected image cylinder is 1.338 km across; a $128\times128$ raster has 10.46 m image-plane pitch, 99.55 km source pixels, and convolved-image SNR 43.16 for 1800 s per sample. With the stated ring-extraction, temporal, background, calibration, and navigation mitigations, the fiducial reconstruction reaches SNR 6.89, structural similarity 0.848, normalized RMS error 0.439, and a 232 km Fourier-ring-correlation resolution proxy. A higher-count case reaches SNR 10.49, structural similarity 0.927, normalized RMS error 0.287, and the 199 km two-pixel grid floor. Controlled cloud tests show that a static inverse fails for rotating cloudy data, whereas phase-registered robust coadds recover persistent surface-proxy structure in the scalar model. The dominant requirements are temporal sampling, coronal and detector calibration, ring extraction, image-plane metrology, optical-operator knowledge, and dynamic inversion, not calibrated monopole SGL blur. The benchmark demonstrates recoverable 200-230 km-class broadband spatial contrast in the stated scalar model, but does not validate propulsion, communications, coronagraphic or external-occulter propagation, physical solar multipoles, physical cloud fields, or a full dynamic retrieval pipeline.

astro-ph.IM↗

Late-Transition Interacting Thawer Dark Energy: Model Definition and Benchmark Consistency Tests

We formulate the late-transition interacting thawer (LTIT) as a late-activating, variable-coupling realization of coupled quintessence in which a canonical scalar field couples conformally only to cold dark matter. The construction is a non-universal dark-sector interaction: baryons and radiation remain minimally coupled, while CDM follows a conformally related metric. This structure ties three observational sectors to one microscopic mechanism--the pre-recombination calibration scale, the low-redshift expansion history, and the coupled growth response. We derive the exact background equations, the exact CDM scaling identity $\rhoc(a)=ρ_{c0}a^{-3}C[ϕ(a)]/C(ϕ_0)$, and the coupled CDM--scalar perturbation equations in synchronous gauge in a form suitable for Einstein--Boltzmann solvers. In the representative benchmarks, $Ω_ϕ(z_*)\sim10^{-9}$, $|Δr_d/r_d|\le3.82\times10^{-3}$, and $\max_{0<z<3}|E/E_{Λ\mathrm{CDM}}-1|\le0.380\%$, while the quasi-static growth indicator ranges from $0.725\%$ to $5.94\%$. LTIT therefore demonstrates how late activation can preserve the early calibration sector while producing a perturbation-sensitive signature, providing a concrete target for Boltzmann-level tests of interacting dark energy.

gr-qc↗