A5027464484- Stellar, planetary, and galactic studies
- Astro and Planetary Science
- Astrophysics and Star Formation Studies
- Astronomy and Astrophysical Research
- Ultrasonics and Acoustic Wave Propagation
- Geophysical Methods and Applications
- Numerical methods in engineering
- Geotechnical Engineering and Underground Structures
- Pulsars and Gravitational Waves Research
- Astronomical Observations and Instrumentation
- Vibration and Dynamic Analysis
- Gamma-ray bursts and supernovae
- High-pressure geophysics and materials
- Solar and Space Plasma Dynamics
- Acoustic Wave Phenomena Research
- Underwater Acoustics Research
- Nuclear physics research studies
- Electromagnetic Simulation and Numerical Methods
- Non-Destructive Testing Techniques
- Photocathodes and Microchannel Plates
Indian Institute of Astrophysics
2019-2023
Pondicherry University
2021-2023
Iowa State University
1990-1991
We have derived the stellar atmospheric parameters, effective temperature T$_{eff}$, microturbulent velocity $\zeta$, surface gravity log g, and metallicity [Fe/H] for HE 0017+0055, 2144-1832, 2339-0837, HD 145777, CD-27 14351 from local thermodynamic equilibrium analyses using model atmospheres. Elemental abundances of C, N, $\alpha$-elements, iron-peak elements, several neutron-capture elements are estimated equivalent width measurement technique as well spectrum synthesis calculations in...
The low-mass metal-poor stars in the Galaxy that preserve their atmosphere, chemical imprints of gas clouds from which they were formed can be used as probes to get insight into origin and evolution elements early galaxy, star formation nucleosynthesis. Among stars, a large fraction, so-called carbon-enhanced (CEMP) exhibits high abundance carbon. These exhibit diverse patterns, particularly for heavy elements, based on are classified different groups. diversity patterns points at scenarios....
Barium stars are one of the important probes to understand origin and evolution slow neutron-capture process elements in Galaxy. These extrinsic stars, where observed s-process element abundances believed have an now invisible companions that produced these at their Asymptotic Giant Branch phase evolution. We attempted nucleosynthesis, as well physical properties companion through a detailed comparison elemental 10 barium with predictions from AGB nucleosynthesis models, FRUITY. For we...
Elemental abundances of CH stars can provide observational constraints for theoretical studies on the nucleosynthesis and evolution low- intermediate-mass stars. However, available abundance data in literature are quite scanty. In our pursuit to generate a homogeneous database elemental we have performed detailed chemical study sample 12 potential star candidates based high resolution spectroscopy. We present first time analysis objects HE 0308-1612, CD-28 1082, HD 30443, 87853. For other...
Abstract We have performed detailed high-resolution spectroscopic analysis on seven metal-poor stars (BD+75 348, BD+09 3019, HD238020, HE0319–0215, HE0507–1653, HE0930–0018, HE1023–1504) and derived their atmospheric parameters T eff , log g [Fe/H], microturbulent velocity ( ξ ). The metallicity range is found to be –2.57 < [Fe/H] –0.42. elemental abundances of 17 light elements 12 heavy are estimated. classified BD+75 348 3019 as strong Ba stars, HD238020 a mild star, the remaining four...
Context. Understanding the surface chemical composition of carbon-enhanced metal-poor (CEMP) stars with enhanced abundances heavy elements remains problematic. Aims. One primary objectives is to investigate origin peculiar abundance pattern observed in extremely object HE 1005–1439, which enriched both s -process and i nucleosynthesis products thus forms a new class distinct pattern. Methods. We performed detailed, high-resolution spectroscopic analysis this based on SUBARU/HDS spectra...
ABSTRACT We present a study based on the high-resolution spectroscopy and K2 space photometry of five chemically peculiar stars in region open cluster M44. The analysis high-precision photometric data reveals that light variations HD 73045 76310 are rotational nature caused by spots or cloud-like co-rotating structures, which non-stationary short-lived. time-resolved radial velocity measurements, combination with photometry, confirm does not show any periodic variability time-scales shorter...
The abundances of the slow neutron-capture (s-) process elements observed in barium stars can be explained by considering mass transfer a binary system from an asymptotic giant branch (AGB) star onto smaller and less evolved companion star. Based on elements, are broadly divided into two categories: “strong” “mild” stars. However, understanding role characteristic properties AGBs formation different types is still lacking. This work focuses investigating masses AGB this context. In recent...
The low-mass metal-poor stars in the Galaxy that preserve their atmosphere, chemical imprints of gas clouds from which they were formed can be used as probes to get insight into origin and evolution elements early galaxy, star formation nucleosynthesis. Among stars, a large fraction, so-called carbon-enhanced (CEMP) exhibits high abundance carbon. These exhibit diverse patterns, particularly for heavy elements, based on are classified different groups. diversity patterns points at scenarios....
Abstract The direct boundary integral equation formalism is used to model reflected and transmitted wave fields due a bounded ultrasonic beam incident upon an arbitrarily curved interface separating fluid solid media. numerical procedure involves application of point collocation with quadratic isoparametric approximation that reduce the equations discrete set linear algebraic equations. Numerical results are provided for plane, concave convex interfaces profiles which Gaussian or...
The abundances of the slow neutron-capture (s-) process elements observed in barium stars can be explained by considering mass transfer a binary system from an asymptotic giant branch (AGB) star onto smaller and less evolved companion star. Based on are broadly divided into two categories, "strong" "mild" stars. However, understanding role characteristic properties AGBs formation different types is still lacking. This work focuses investigating AGB this context. In recent high-resolution...
We have performed detailed high-resolution spectroscopic analysis on seven metal-poor stars (BD+75 348, BD+09 3019, HD238020, HE0319-0215, HE0507-1653, HE0930-0018, HE1023-1504) and derived their atmospheric parameters T$_{eff}$, log$g$, [Fe/H], mictroturbulent velocity ($ξ$). The metallicity range is found to be -2.57$<$[Fe/H]$<$-0.42. elemental abundances of 17 light elements 12 heavy are estimated. classified BD+75 348 3019 as strong Ba stars, HD238020 a mild star, the remaining...