A5089221015- Stellar, planetary, and galactic studies
- Gamma-ray bursts and supernovae
- Astronomy and Astrophysical Research
- Pulsars and Gravitational Waves Research
- Astrophysics and Star Formation Studies
- Astro and Planetary Science
- High-pressure geophysics and materials
- Advanced Chemical Physics Studies
- History and Developments in Astronomy
- Scientific Research and Discoveries
- Semiconductor materials and devices
- Spectroscopy and Laser Applications
Osservatorio Astronomico di Padova
2022-2025
University of Padua
2024-2025
We present a new comprehensive collection of stellar evolutionary tracks and isochrones for rotating low- intermediate-mass stars assembled with the updated version PARSEC V2.0. This includes our recent calibration extra mixing from overshooting rotation, as well several improvements in nuclear reaction network, treatment convective zones, mass loss other physical input parameters. The initial models covers range 0.09 $M_\odot$ to 14 $M_\odot$, six sets metallicity, Z=0.004 Z=0.017. Rotation...
We present new evolutionary models of primordial very massive stars, with initial masses ranging from $100\,\mathrm{{M}_{\odot}}$ to $1000\,\mathrm{{M}_{\odot}}$, that extend the main sequence until onset dynamical instability caused by creation electron-positron pairs during core C, Ne, or O burning, depending on star's mass and metallicity. Mass loss accounts for radiation-driven winds as well pulsation-driven mass-loss red supergiant phase. After examining properties, we focus final...
ABSTRACT Gravitational lensing may render individual high-mass stars detectable out to cosmological distances, and several extremely magnified have in recent years been detected redshifts $z\approx 6$. Here, we present Muspelheim, a model for the evolving spectral energy distributions of both metal-enriched metal-free at high redshifts. Using this model, argue that lensed will form highly biased sample intrinsic distribution across Hertzsprung–Russell diagram, bias typically tend favour...
Abstract We calculate new evolutionary models of rotating primordial very massive stars, with initial mass from 100 M ⊙ to 200 , for two values the metallicity Z = 0 and 0.0002. For first time in this range, we consider stellar rotation pulsation-driven loss, along radiative winds. The evolve zero-age main sequence until onset pair-instability. discuss properties during their evolution then focus on final fate possible progenitors jet-driven events. All tracks that undergo pulsational-pair...
Abstract There has been growing evidence that the rich star clusters in Magellanic Clouds contain significant fractions of rapidly rotating stars. In this work, we aim to constrain these by studying colour-magnitude diagrams four clusters, selected among those with most striking signatures fast rotators. Using isochrones derived from parsec v2.0 stellar tracks, generate distinct populations, each covering a limited interval initial rotation rates $\mbox{$\omega _\mathrm{i}$}$, referred as...
There has been growing evidence that the rich star clusters in Magellanic Clouds contain significant fractions of rapidly rotating stars. In this work, we aim to constrain these by studying colour-magnitude diagrams four clusters, selected among those with most striking signatures fast rotators. Using isochrones derived from PARSEC v2.0 stellar tracks, generate distinct populations, each covering a limited interval initial rotation rates $\omega_\mathrm{i}$, referred as 'Partial Models'...
Abstract The initial–final mass relation (IFMR) plays a crucial role in understanding stellar structure and evolution by linking star’s initial to the of resulting white dwarf. This study explores IFMR range 0.8 ≤ M ini / ⊙ 4 using full PARSEC evolutionary calculations supplemented with COLIBRI computations complete ejection envelope obtain final core mass. Recent works have shown that supposed monotonicity is interrupted kink ≈ 1.65–2.10 , due interaction between recurrent dredge-up...
Abstract We address the critical need for accurate Rosseland mean gas opacities in high-pressure environments, spanning temperatures from 100 K to 32,000 K. Current opacity tables Wichita State University and Æ SOPUS 2.0 are limited <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mi>R</mml:mi> stretchy="false">)</mml:mo> <mml:mo>≤</mml:mo> <mml:mn>1</mml:mn> </mml:math> , where <mml:mo>=</mml:mo>...
The initial-final mass relation (IFMR) plays a crucial role in understanding stellar structure and evolution by linking star's initial to the of resulting white dwarf. This study explores IFMR range $0.8 \leq M_\mathrm{ini} / M_\odot 4$ using full PARSEC evolutionary calculations supplemented with COLIBRI computations complete ejection envelope obtain final core mass. Recent works have shown that supposed monotonicity is interrupted kink $M_\mathrm{ini} \approx 1.65-2.10 M_\odot$, due...
We address the critical need for accurate Rosseland mean gas opacities in high-pressure environments, spanning temperatures from 100 K to 32000 K. Current opacity tables Wichita State University and AESOPUS 2.0 are limited $\log(R) \le 1$, where $R=\rho\, T_6^{-3}$ units of $\mathrm{g}\,\mathrm{cm}^{-3}(10^6\mathrm{K})^{-3}$. This is insufficient modeling very low-mass stars, brown dwarfs, planets with atmospheres exhibiting higher densities pressures ($\log(R) > 1$). Leveraging extensive...
We calculate new evolutionary models of rotating primordial very massive stars, with initial mass from $100\,M_{\odot}$ to $200\,M_{\odot}$, for two values the metallicity ${Z=0}$ and ${Z=0.0002}$. For first time in this range, we consider stellar rotation pulsation-driven loss, along radiative winds. The evolve zero-age main sequence, until onset pair instability. discuss properties during their evolution then focus on final fate possible progenitors jet-driven events. All tracks that...
Gravitational lensing may render individual high-mass stars detectable out to cosmological distances, and several extremely magnified have in recent years been detected redshifts $z\approx 6$. Here, we present Muspelheim, a model for the evolving spectral energy distributions of both metal-enriched metal-free at high redshifts. Using this model, argue that lensed should form highly biased sample intrinsic distribution across Hertzsprung-Russell diagram, bias will typically tend favour...
We present new evolutionary models of primordial very massive stars, with initial masses ranging from $100\,\mathrm{{M}_{\odot}}$ to $1000\,\mathrm{{M}_{\odot}}$, that extend the main sequence until onset dynamical instability caused by creation electron-positron pairs during core C, Ne, or O burning, depending on star's mass and metallicity. Mass loss accounts for radiation-driven winds as well pulsation-driven mass-loss red supergiant phase. After examining properties, we focus final...