A5036072719- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Gamma-ray bursts and supernovae
- Astrophysics and Star Formation Studies
- Geophysics and Gravity Measurements
- Pulsars and Gravitational Waves Research
- Spectroscopy and Laser Applications
- High-pressure geophysics and materials
- Semiconductor materials and devices
- Advanced Chemical Physics Studies
Scuola Internazionale Superiore di Studi Avanzati
2022-2024
Osservatorio Astronomico di Padova
2024
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...
Recent advancements in stellar evolution modeling offer unprecedented accuracy predicting the and deaths of stars. We present new evolutionary models computed with updated V2.0 code for a comprehensive homogeneous grid metallicities initial masses. Nuclear reaction networks, mass loss prescriptions, treatment elemental mixing have all been V2.0. thirteen spanning Z = to 0.03, masses ranging from 2.0 2000 consisting library over 1,100 (∼ 2100 tracks including pure-He models) full tracks. For...
Recent advancements in stellar evolution modeling offer unprecedented accuracy predicting the and deaths of stars. We present new evolutionary models computed with updated PARSEC V2.0 code for a comprehensive homogeneous grid metallicities initial masses. Nuclear reaction networks, mass loss prescriptions, treatment elemental mixing have all been V2.0. thirteen spanning $Z = 10^{-11}$ to 0.03$, masses ranging from 2.0 M$_{\odot}$ 2000 M$_{\odot}$, consisting library over 1,100 ($\sim 2100$...
Thermohaline mixing is one of the main processes in low-mass red giant stars that affect transport chemicals and, thus, surface abundances along evolution. The interplay thermohaline with other processes, such as downward overshooting from convective envelope, needs to be carefully investigated. This study aims understand combined effects and envelope overshooting. After implementing process parsec stellar evolutionary code, we computed tracks isochrones (with trilegal code) compared them...
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...
Benefiting from the GAIA second and early third releases of photometric astrometric data we examine population asymptotic giant branch (AGB) stars that appear in fields intermediate-age young open star clusters. We identify 49 AGB candidates, brighter than tip red branch, with a good-to-high cluster membership probability. Among them find 19 TP-AGB known spectral type: 4 M stars, 3 MS/S 12 C stars. By combining observations, stellar models, radiative transfer calculations include effect...
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...
Thermohaline mixing is one of the main processes in low-mass red giant stars that affect transport chemicals and, thus, surface abundances along evolution. The interplay thermohaline with other processes, such as downward overshooting from convective envelope, should be carefully investigated. This study aims to understand combined effects and envelope overshooting. After implementing process \textsc{parsec} stellar evolutionary code, we compute tracks isochrones (with \textsc{trilegal}...
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...