175 papers
By analyzing Gaia DR3 data to model the local stellar population around supernova remnant S147, the study identifies a high-mass progenitor range of $21.5M_{\odot}41.1M_{\odot}$ for the supernova, based on the ages of the most luminous nearby stars including the unbound binary companion HD 37424.
This paper demonstrates that the LuSEE-Night lunar pathfinder radio telescope can produce low-resolution (~5-degree) maps of the sub-50 MHz sky by applying a Wiener filter-based linear map-making algorithm that effectively marginalizes systematic effects such as beam uncertainty and gain fluctuations.
This paper demonstrates that low-resolution spectroscopic surveys suffer from significant radial velocity biases due to incomplete modeling of pressure-broadened hydrogen line wings, and it provides resolution-independent corrections that validate SDSS-V wavelength calibration and enable accurate white dwarf mass-radius tests.
This paper demonstrates that the modified gravity theory, through a non-minimal matter-curvature coupling, allows for stable super-Chandrasekhar white dwarf configurations and uses Bayesian inference with observational data to constrain the coupling parameter .
This paper introduces and validates "Nemesis," a flexible and scalable multi-scale, multi-physics algorithm built on AMUSE that accurately simulates complex astrophysical systems like star clusters with planetary binaries, matching the precision of direct N-body codes while maintaining computational efficiency through effective time synchronization and parallelization.
Based on a 45-year radial velocity survey of 625 stars in the Hyades cluster, this study characterizes the binary population by determining a 40% binary frequency, updating orbital parameters for over 100 systems, revising the tidal circularization period to approximately 5.9 days, and measuring the cluster's velocity dispersion and stellar gravitational/convective shifts.
This study reconstructs and analyzes the first four ground-level enhancements (GLEs) from the 1940s by digitizing forgotten cosmic-ray data, revealing distinct temporal evolution patterns and spectral hardness characteristics for these historically missing events.
This study derives an analytical function based on the progressive wave picture to quantitatively link mixed mode visibilities and detectability to core damping rates in red giants, revealing that finite damping can mimic infinite damping effects and explaining observed populations with unusually low mode amplitudes.
This study reveals a puzzling contradiction in the Necklace planetary nebula, where the central binary system's properties suggest a carbon-rich evolutionary history and an inflated carbon dwarf companion, yet the inner nebula observed via Hubble Space Telescope spectroscopy appears carbon-poor.
Through 56 3D hydrodynamic simulations of ONe white dwarfs, this study identifies a critical transition density range and demonstrates that both ignition conditions and laminar flame speeds are decisive factors in determining whether electron-capture supernovae result in a thermonuclear explosion or a gravitational collapse.
By re-examining 1,405 exoplanets orbiting 1,221 stars with high-precision parameters from SWEET-Cat, this study confirms the existence of the radius valley and reveals its dependence on period, flux, stellar mass, and age, providing evidence that supports a core-powered atmospheric mass loss scenario while highlighting the need for improved stellar characterizations in future missions like PLATO.
Using 3D radiative magnetohydrodynamic simulations of collapsing cores, this study demonstrates that anisotropic, streamer-fed accretion driven by magnetic fields and turbulence not only facilitates rapid disk spreading but also continuously generates and sustains significant eccentricity () in Class 0 protoplanetary disks, with profound implications for planet formation and cosmochemistry.
This study introduces a physically motivated mass-loss prescription for Eddington-limit induced ejections in 1D stellar evolution codes, demonstrating that incorporating this mechanism into single and binary models successfully reconciles theoretical predictions with observed massive star populations in the Magellanic Clouds, including their luminosity limits, evolutionary stages, and binary fractions.
By combining L-band spectra of 15 backlit young stellar objects in the Central Molecular Zone with multi-wavelength data, this study reveals an ensemble-averaged methanol ice abundance profile that is systematically lower than in the Galactic disk and increases from the inner to outer envelope regions, likely due to the sublimation of methanol ice caused by intense heating from massive protostars.
This study presents the first self-consistent 3D MHD simulation demonstrating that decayless kink oscillations in solar coronal loops emerge spontaneously with linear polarization, suggesting a self-sustained driver rather than a stochastic source.
By applying hydrodynamically-consistent PoWR-HD modeling and Gaia DR3 parallaxes to a sample of six Galactic WN4b stars, this study resolves parameter degeneracies inherent in traditional grid-based analyses to reveal a narrow temperature range, confirm the existence of low-luminosity Wolf-Rayet stars, and identify distinct mass-loss characteristics compared to WN2 stars.
This study utilizes multi-survey light curves and infrared data to demonstrate that the variable mean magnitudes observed in approximately 0.9% of RR Lyrae stars in the Galactic bulge are genuine astrophysical phenomena, likely caused by variable dust extinction rather than photometric errors.
Using the TARDIS radiative-transfer code combined with neural network emulation and MCMC inference, this study demonstrates that single high-velocity density enhancements cannot simultaneously reproduce the observed silicon and calcium high-velocity features in Type Ia supernovae, suggesting that current delayed- and double-detonation explosion models are incomplete.
This study utilizes an expanded catalog of 1976 interplanetary coronal mass ejection events observed from 0.07 to 5.4 au to demonstrate that their magnetic field evolution follows a single power law with an exponent of approximately -1.57, while revealing that a two-exponent multipole model is required to reconcile these interplanetary measurements with solar source field strengths.
Using high-precision radial velocities from HARPS-N combined with Gaia DR3 astrometry, the GAPS programme confirmed that the companion HD 128717 B (Gaia-6 B) is a long-period, high-eccentricity brown dwarf with a mass of approximately 20 Jupiter masses, correcting a previously inaccurate orbital solution derived solely from Gaia data.