Spectral and type I X-ray burst studies of M15 X-2 using NICER observations
Accretion; Accretion discs; Stars: neutron; X-rays: binaries; X-rays: bursts, burst oscillation; X-rays: individual: M15 X-2
In this work, we present spectral and burst analyses of three thermonuclear type I X-ray bursts (B1, B2, and B3) detected from the ultracompact neutron star low-mass X-ray binary M15 X-2, using data from the Neutron Star Interior Composition Explorer (NICER). Time-averaged spectral fitting with the model tbabsthcompiskbb) suggests that the source was in a soft or soft-intermediate spectral state, characterized by a photon power law index of ??2 and an average mass accretion rate of ?0.09 m?Edd. The type I X-ray bursts exhibited rapid rise times of 1.25?2.75 s, followed by longer decay phases lasting 14.50?23.25 s, with characteristic burst timescales (?) of ?11 s, which are consistent with pure helium burning. Notably, burst B3 displayed a double-peaked profile indicative of a photospheric radius expansion event, from which we inferred the neutron star radius to be 10.8+2.4?2.2 km. Based on the peak flux of the burst, we estimated the source distance to be 10.54+1.43?1.26 kpc under the assumption of isotropic emission, and 14.06+1.90?1.68 kpc for anisotropic emission geometry. A strong ?420 Hz burst oscillation candidate was detected in the cooling tail of burst B1. 2025 Elsevier B.V.
Varun, M.; Thomas, Neal Titus; Giridharan, L.; Gudennavar, S.B.; Bubbly, S.G.
Journal of High Energy Astrophysics;Volume;49;Issue;;Article No.;100461;
Restricted Access; Hardcopy may be available in the library
https://doi.org/10.1016/j.jheap.2025.100461 https://www.scopus.com/pages/publications/105015778948?origin=resultslist
Varun M., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India; Thomas N.T., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India; Giridharan L., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India; Gudennavar S.B., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India; Bubbly S.G., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India
Spectral characteristics of the black hole binary 4U 1957+115: a multi mission perspective
accretion; accretion discs; black hole physics - X-rays: low mass X-ray binaries; X-rays: individual: 4U 1957+115
We report spectral analysis of the persistent black hole X-ray binary, 4U 1957+115, using AstroSat, Swift, and NuSTAR observations carried out between 2016 and 2019. Modelling with a disc emission, thermal Comptonization, and blurred reflection components revealed that the source was in the high-soft state with the disc flux ?87 per cent of the total and high-energy photon index ?2.6. There is an evidence that either the inner disc radius varied by ?25 per cent or the colour hardening factor changed by ?12 per cent. The values of the inner disc radius imply that for a non-spinning black hole, the black hole mass is < 7 M ? and the source is located > 30 kpc away. On the other hand, a rapidly spinning black hole would be consistent with the more plausible black hole mass of < 10 M ? and a source distance of ?10 kpc. Fixing the distance to 10 kpc and using a relativistic accretion disc model, constrained the black hole mass to 6 M? and inclination angle to 72. A positive correlation is detected between the accretion rate and inner radii or equivalently between the accretion rate and colour factor. 2022 The Author(s).
Mudambi S.P.; Gudennavar S.B.; Misra R.; Bubbly S.G.
Monthly Notices of the Royal Astronomical Society, Vol-517, No. 3, pp. 4489-4496.
https://doi.org/10.1093/mnras/stac2952 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85145263083&doi=10.1093%2fmnras%2fstac2952&partnerID=40&md5=3ca8d4d72d0e7b16667c03ac66c78df9
Mudambi S.P., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore Central Campus, Bengaluru, 560029, India; Gudennavar S.B., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore Central Campus, Bengaluru, 560029, India; Misra R., Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune, 411007, India; Bubbly S.G., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore Central Campus, Bengaluru, 560029, India
Spectral Evolution of GX 17+2 Using AstroSat and NICER Observations
We study the spectral evolution of the Z-track source GX 17+2 using AstroSat and NICER observations taken between 2016 and 2020. The AstroSat observations cover the period when the source is in the normal branch (NB) and the flaring branch (FB), while for the NICER ones the variability can be associated with the FB branch. The source spectra at different regions of the branches are well described by accretion disk emission, blackbody surface emission, and a thermal Comptonization component. In the NB, the total bolometric unabsorbed flux remains constant and the variation is due to changes in the Comptonization, disk fluxes. In particular, the inferred luminosity (LT) and accretion rate ( M ? ) remain constant, while there is significant variation in the inner disk radii and fraction of disk photons entering the corona, indicating changes in the geometry of the system. On the other hand, in the FB, there is significant variation in luminosity from ?4.0 to ?7.0 1038 erg s?1. Despite this significant variation in luminosity and in the inner disk radii, the accretion efficiency, defined as ? = L T / M ? c 2 , remains nearly constant at ?0.20 throughout the evolution of the source, as expected for a neutron star system. 2025. The Author(s). Published by the American Astronomical Society.
Bhattacherjee, Sree; Misra, Ranjeev; Sarkar, Biplob; Jithesh, V.; Roy, Jayashree; Bhulla, Yashpal
Astrophysical Journal;Volume;989;Issue;1;Article No.;23;
All Open Access; Gold Open Access; Green Open Access
https://doi.org/10.3847/1538-4357/ade9ad https://www.scopus.com/pages/publications/105012271188?origin=resultslist
Bhattacherjee S., Department of Applied Sciences, Tezpur University, Assam, Napaam, 784028, India; Misra R., Inter-University Center for Astronomy and Astrophysics, Ganeshkhind, Pune, 411007, India; Sarkar B., Department of Applied Sciences, Tezpur University, Assam, Napaam, 784028, India; Jithesh V., Department of Physics and Electronics, Christ University, Hosur Main Road, Bengaluru, 560029, India; Roy J., Inter-University Center for Astronomy and Astrophysics, Ganeshkhind, Pune, 411007, India; Bhulla Y., Pacific Academy of Higher Education and Research University, Udaipur, 313003, India
Spectral Properties of the Soft X-Ray Transient MAXI J0637-430 Using AstroSat
Soft X-ray transients are systems that are detected when they go into an outburst, wherein their X-ray luminosity increases by several orders of magnitude. These outbursts are markers of the poorly understood change in the spectral state of these systems from the low/hard state to the high/soft state. We report the spectral properties of one such soft X-ray transient: MAXI J0637-430, with data from the SXT and LAXPC instruments on board the AstroSat mission. The source was observed for a total of ?60 ks in two observations on 2019 November 8 and 21 soon after its discovery. Flux-resolved spectral analysis of the source indicates the presence of a multicolor blackbody component arising from the accretion disk and a thermal Comptonization component. The stable low temperature (?0.55 keV) of the blackbody component points to a cool accretion disk with an inner disk radius of the order of a few hundred kilometers. In addition, we report the presence of a relativistically broadened Gaussian line at 6.4 keV. The disk-dominated flux and photon power-law index of ?2 and a constant inner disk radius indicate the source to be in the soft state. From the study we conclude that MAXI J0637-430 is a strong candidate for a black hole X-ray binary. 2022. The Author(s). Published by the American Astronomical Society.
Thomas N.T.; Gudennavar S.B.; Misra R.; Bubbly S.G.
https://doi.org/10.3847/1538-4357/ac425e https://www.scopus.com/inward/record.uri?eid=2-s2.0-85125866427&doi=10.3847%2f1538-4357%2fac425e&partnerID=40&md5=98c2bcce8d33553e86dc98b90d71510a
Thomas N.T., Department of Physics and Electronics, CHRIST (Deemed to Be University), Central Campus, Bengaluru, 560029, India; Gudennavar S.B., Department of Physics and Electronics, CHRIST (Deemed to Be University), Central Campus, Bengaluru, 560029, India; Misra R., Inter-University Centre of Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune, 411007, India; Bubbly S.G., Department of Physics and Electronics, CHRIST (Deemed to Be University), Central Campus, Bengaluru, 560029, India
Spectral quasi-linearization and irreversibility analysis of magnetized cross fluid flow through a microchannel with two different heat sources and Newton boundary conditions
Fluid flow in a microchannel with heat transport effects can be seen in various applications such as micro heat collectors, mechanicalelectromechanical systems, electronic device cooling, micro-air vehicles, and micro-heat exchanger systems. However, little is known about the consequence of internal heat source modulations on the flow of fluids in a microchannel. Therefore, in this work, the heat transfer of a magnetized cross fluid is carried out in a micro-channel subjected to two different heat source modulations. Entropy production analysis is also performed. The mathematical model consists of a cross fluid model. In addition, the effects of Joule heating, external magnetism, and the boundary conditions of Newton's heating are also examined. Determinant equations are constructed under steady-state conditions and parameterized using dimensionless variables. The numerical spectral quasi-linearization (SQLM) method was developed to interpret the Bejan number, entropy production, temperature, and velocity profiles. It is established that the power-law index of the cross fluid reduces the magnitude of the entropy production, velocity, and thermal field in the entire microchannel region. Furthermore, a larger Weissenberg number is capable of producing greater entropy, velocity, and thermal fields throughout the microchannel region. The variation in temperature distribution is more noticeable for the ESHS aspect than the THS aspect. The values of the pressure gradient parameter and the Eckert number must be kept high for maximum heat transport of the cross fluid. The entropy production of the cross fluid increases significantly with the physical aspects of Joule heating and convection heating in the system. 2021, The Author(s), under exclusive licence to SocietItaliana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature.
Al-Kouz W.; Reddy C.S.; Alqarni M.S.; Mahanthesh B.
European Physical Journal Plus, Vol-136, No. 6
Springer Science and Business Media Deutschland GmbH
https://doi.org/10.1140/epjp/s13360-021-01625-3 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85107593006&doi=10.1140%2fepjp%2fs13360-021-01625-3&partnerID=40&md5=36d2b4bf5177ab49bd2e5dfff71d15ee
Al-Kouz W., Department of Mechanical and Maintenance Engineering, German Jordanian University, Amman, 11180, Jordan; Reddy C.S., Department of Mathematics, Government City College, Nayapul, Hyderabad, 500002, India; Alqarni M.S., Department of Mathematics, College of Sciences, King Khalid University, Abha, 61413, Saudi Arabia, Mathematical Modelling and Applied Computation Research Group (MMAC), Department of Mathematics, King Abdulaziz University, P. O. Box 80203, Jeddah, 21589, Saudi Arabia; Mahanthesh B., Department of Mathematics, CHRIST (Deemed to be University), Bengaluru, 560029, Karnataka, India
Spectro-temporal and type I X-ray burst analysis of GX 3+1 using AstroSat observations
accretion, accretion discs; stars: neutron; X-rays: binaries; X-rays: bursts
GX 3+1, an atoll type neutron star low-mass X-ray binary, was observed four times by Soft X-ray Telescope and The Large Area X-ray Proportional Counter on-board AstroSat between 2017 October 5 and 2018 August 9. The hardness-intensity-diagram of the source showed it to be in the soft spectral state during all the four observations. The spectra of the source could be adequately fit with a model consisting of blackbody (bbody) and powerlaw (powerlaw) components. This yielded the blackbody radius and mass accretion rate to be ?8 km and ?2 10?9 M? y?1, respectively. In one of the observations, a type I X-ray burst having a rise and e-folding time of 0.6 and 5.6 s, respectively, was detected. Time-resolved spectral analysis of the burst showed that the source underwent a photospheric radius expansion. The radius of the emitting blackbody in GX 3+1 and its distance were estimated to be 9.19 +?00.8297 km and 10.17 +?00.1807 kpc, respectively. Temporal analysis of the burst yielded upper limits of the fractional root mean square amplitude of 7 per cent, 5 per cent, and 6 per cent during burst start, burst maximum, and right after the radius expansion phase, respectively. 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Thomas N.T.; Gudennavar S.B.; Bubbly S.G.
Monthly Notices of the Royal Astronomical Society, Vol-521, No. 1, pp. 433-442.
https://doi.org/10.1093/mnras/stad555 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85161580506&doi=10.1093%2fmnras%2fstad555&partnerID=40&md5=f94df9d043c50c2e2d9b68a88fd761a2
Thomas N.T., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India; Gudennavar S.B., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India; Bubbly S.G., Department of Physics and Electronics, CHRIST University, Karnataka, Bangalore, 560029, India
Spectrochemical and theoretical approaches for acylhydrazone-based fluoride sensors
Ab initio; Acylhydrazones; Anion recognition; Fluoride sensing; TD-DFT
Abstract: Acylhydrazone derivatives N?-[1-(2-fluorophenyl)ethylidene]pyridine-3-carbohydrazide (R1) and N?-[2-fluorobenzylidene]benzohydrazide (R2) were synthesized from their corresponding hydrazides and characterized by spectroscopic methods. The response of these acylhydrazones towards different anions was studied by colorimetric and spectrofluorometric methods in acetonitrile. The receptors exhibited a specific response towards fluoride ion. The binding affinity of the receptors with fluoride anion was studied by fluorescence spectroscopic techniques and abinitio density functional theory calculations with Beckers three-parameter LeeYangPar (B3LYP) exchange functional with 6-311G basis set. Graphical abstract: [Figure not available: see fulltext.]. 2018, Springer Nature B.V.
Jose J.; Sreekanth A.; John A.M.; Basheer S.M.; Sreeja P.B.
Research on Chemical Intermediates, Vol-45, No. 2, pp. 425-435.
Jose J., Department of Chemistry, CHRIST (Deemed to be University), Hosur Road, Bangalore, 560029, India; Sreekanth A., Department of Chemistry, National Institute of Technology, Tiruchirappalli, 620015, India; John A.M., Department of Chemistry, CHRIST (Deemed to be University), Hosur Road, Bangalore, 560029, India; Basheer S.M., Department of Chemistry, National Institute of Technology, Tiruchirappalli, 620015, India; Sreeja P.B., Department of Chemistry, CHRIST (Deemed to be University), Hosur Road, Bangalore, 560029, India
Spectrometric Analysis of Decrease in Sodium Dodecyl Sulfate (SDS) Concentration by Klebsiella Species Using the Stains-All Dye
anionic surfactant; bacterial biodegradation; detergent-degrading bacteria; SDS degradation; Stains-all, carbocyanine dye
Abstract: Sodium dodecyl sulfate (SDS)-degrading bacteria were isolated from soil and water samples from multiple locations using basal media with 0.05% SDS as the only carbon source. The bacteria were identified using 16S rRNA sequencing and deposited in the NCBI database with specific accession numbers and strain name. There were six bacteria iidentified as Klebsiella variicola MSK86, Klebsiella sp. MSK86, K. quasipneumoniae MSK86, and three K. pneumoniae strains, MSK86, MSK25, and NET12. The potential for decrease in SDS concentration by the bacteria was assessed using Stains-all. The SDS standard graph was plotted with different SDS concentration of 0 to 0.06%. The SDS-Stains-all complex exhibited a peak with maximum absorbance at 440 nm. The absorbance of the bacteria-inoculated samples was monitored at 440 nm on every 24 h until the sixth day of incubation. The decrease in concentration of SDS in the medium on day 6 of incubation by K. pneumoniae MSK86, K. variicola MSK86, and Klebsiella sp. MSK86 was found to be 86, 84, and 84%, respectively. K. pneumoniae NET12 demonstrated 76% of decrease. K. pneumoniae MSK25 and K.quasipneumoniae MSK86 were able to survive in the SDS medium, with decrease of 20 and 40%, respectively. The focus of this investigation was finding bacteria that can breakdown SDS, that may contribute to the decrease in the amount of detergent pollution in water. Pleiades Publishing, Ltd. 2025.
Microbiology (Russian Federation);Volume;94;Issue;1;pp.128-133
https://doi.org/10.1134/S0026261724606419 https://www.scopus.com/pages/publications/85219586966?origin=resultslist
Mittu Koshy, Department of Life Sciences, CHRIST (Deemed To Be University), Bangalore, 560029, India; Biljo V. Joseph, Department of Life Sciences, CHRIST (Deemed To Be University), Bangalore, 560029, India
Spectroscopic analysis of lead borate systems
Oxide glass systems are interesting because of their bonding like bridging and non-bridging oxygens. Depending on the modifier, the B2O3 glass system can have various Boron-Oxygen network. It is found that, PbO modifies the borate network and increases the formation of penta and diborate groups. In this work, we investigated optical properties of Lead Borate glass systems (x PbO: (1-x) B2O3) with x varying from 30-85 mol % using UV-VIS Spectra and the corresponding band gap was estimated using Tauc relation and these systems behave like direct allowed band gap systems. These results show that, Eg decreases with the addition of lead content. Further the refractive index measurements also have been carried out at various wavelengths. Many correlation is found between the band gap and refractive index for different compositions. Using different theoretical models a best fit has been tried and Ravindra's relation is found to match with our experimental results. 2018 Author(s).
Georgi A.D.; Ramesh K.P.; Mallikarjunaiah K.J.
Georgi A.D., Department of Physics, Christ University, Bengaluru, 560028, India; Ramesh K.P., Department of Physics, Indian Institute of Science, Bengaluru, 560012, India; Mallikarjunaiah K.J., Undergraduate Programme-Physics, Indian Institute of Science, Bengaluru, 560012, India
Spectroscopic and TDDFT investigation of highly selective fluoride sensors by substituted acyl hydrazones
Acyl hydrazones; Anion recognition; Chemosensors; Fluoride sensing; Theory (TDDFT); Time dependent density functional
In this work, we report the synthesis of two receptors for fluoride ions based on acyl hydrazone, such as N?-[(1Z)-1-(4-fluorophenyl)ethylidene]benzohydrazide (R1) and N?-[(1Z)-1-(2-hydroxyphenyl)ethylidene]benzohydrazide (R2). The receptors R1 and R2 were synthesized from the corresponding ketones and benzoic acid hydrazide and characterized spectroscopically by UVvisible, IR and 1HNMR techniques. The response of R1 and R2 towards different anions was studied colourimetrically in acetonitrile. The receptors exhibited a specific response towards fluoride ions. Further studies of 1:1 composition of receptors, R1/R2:fluoride ions by different spectroscopic techniques such as UVVisible, IR and 1HNMR spectroscopy indicated the participation of -NH proton of the receptors in the sensing action through the hydrogen bonding. To understand the mechanism, Time-Dependent Density Functional Theory (TD-DFT) studies were done using the CAM-B3LYP/6311G++ (3df,2p) with Grimme's D3BJ empirical dispersion basis set. The studies supported the role of hydrogen bonding interaction of -NH and-OH protons of the receptors with the fluoride ions. 2020 Elsevier B.V.
John A.M.; Jose J.; Thomas R.; Thomas K.J.; Balakrishnan S.P.
Spectrochimica Acta - Part A: Molecular and Biomolecular Spectroscopy, Vol-236
ISSN: 13861425; PubMed ID: 32299039; CODEN: SAMCA
https://doi.org/10.1016/j.saa.2020.118329 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85083028106&doi=10.1016%2fj.saa.2020.118329&partnerID=40&md5=35d8ac7cd9472f0151d0f42a472ee54d
John A.M., Department of Chemistry, CHRIST (Deemed to be University), Bangalore, 560029, Karnataka, India; Jose J., Department of Chemistry, CHRIST (Deemed to be University), Bangalore, 560029, Karnataka, India; Thomas R., Department of Chemistry, St. Berchmans College (Autonomous), Changanassery, 686101, Kerala, India; Thomas K.J., Department of Chemistry, CHRIST (Deemed to be University), Bangalore, 560029, Karnataka, India; Balakrishnan S.P., Department of Chemistry, CHRIST (Deemed to be University), Bangalore, 560029, Karnataka, India
Spectroscopic investigation on shuttlecock-shaped liquid crystalline trimers: Mesomorphic behaviour and its application in optical storage devices
In this paper, we discuss the synthesis and characterization of 2,3,4-tris[n-((4-(-cyanophenyl)diazenyl)phenoxy)alkyloxy]benzonitrile obtained by coupling 2,3,4-trihydroxy benzonitrile and (E)-4-((4-((n-bromoalkyl)oxy)phenyl)diazenyl)benzonitrile, pertain to shuttlecock shaped liquid crystals. The molecular structure was confirmed by NMR spectroscopic and elemental analyzer. The thermal behavior of the trimers was assessed using a polarizing optical microscope (POM) and differential scanning calorimetry (DSC). The three diazo groups in the trimers enabled us to study the photo-isomerization effect and evaluate their potential applications in optical storage devices. Importantly, we found these trimers easy to synthesize and process, paving the way for cost-effective alternatives to traditional LC materials. We fabricated an optical storage device to study the light effects on shuttlecock-shaped LC trimers, demonstrating that the geometry of the trimers plays a crucial role in determining structure-property relationships. 2024
Sandhya Kumari D.; Shetty A.; Ranjitha B.S.; M V.; Shanker G.; Alaasar M.; Hegde G.
https://doi.org/10.1016/j.heliyon.2024.e37455 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85203975088&doi=10.1016%2fj.heliyon.2024.e37455&partnerID=40&md5=e22bff47dab6975e5e0a0fb44645a03b
Sandhya Kumari D., Department of Chemistry, Jnana Bharathi Campus, Bangalore University, Bengaluru, 560056, India; Shetty A., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India, Centre for Advanced Research and Development (CARD), Christ University, Hosur Road, Bengaluru, 560029, India; Ranjitha B.S., Department of Chemistry, Jnana Bharathi Campus, Bangalore University, Bengaluru, 560056, India; M V., Department of Chemistry, Christ University, Hosur Road, Bengaluru, 560029, India, Centre for Advanced Research and Development (CARD), Christ University, Hosur Road, Bengaluru, 560029, India; Shanker G., Department of Chemistry, Jnana Bharathi Campus, Bangalore University, Bengaluru, 560056, India; Alaasar M., Department of Chemistry, Faculty of Science, Cairo University, Giza, Egypt; Hegde G., Centre for Advanced Research and Development (CARD), Christ University, Hosur Road, Bengaluru, 560029, India
Spectroscopic parameters of red emitting Eu3 +-doped La2Ba3B4O12 phosphor for display and forensic applications
Forensic application; Judd-Ofelt theory; Photoluminescence; Solid-state lighting; Spectroscopic parameter
Eu3+-activated La2Ba3B4O12 (LBBO) phosphor was synthesized by the solid-state reaction method. LBBO phosphors characterized by structural analysis (X-ray diffraction), including refinement parameters and crystallite size, morphological analysis by (Scanning Electron Microscopy and Transmission Electron Microscopy). Photoluminescence (PL) studies of synthesized phosphors monitored in the range of 450-675 nm for the LBBO phosphor doped with Eu3 +. An excitation peak was found at 254nm and several sharp emission peaks were found around 466, 541, 588, 593, 613, and 626nm with high intensities. The crystallite size of the Eu3 +-doped LBBO phosphor was around 126nm. It is found that the intense emission peak is in the red region. The detailed processes involved and a possible mechanism for the PL are studied and discussed. The phosphor can also be used in forensic science to detect fingerprints. 2021 Elsevier Ltd All rights reserved.
Dubeya N.; Michalska-Doma?skab M.; Sajic J.; Dubeyd V.; Salujaa J.K.
Hybrid Perovskite Composite Materials: Design to Applications, pp. 169-180.
Dubeya N., Department of Physics, Govt. V.Y.T.PG. Auto. College, Chhattisgarh, Durg, India; Michalska-Doma?skab M., Institute of Optoelectronics, Military University of Technology, Warsaw, Poland; Sajic J., Department of Sciences and Humanities, Faculty of Engineering, Christ (Deemed to be University), Bangalore, India; Dubeyd V., Department of Physics, Bhilai Institute of Technology Raipur, Chhattisgarh, Kendri, India; Salujaa J.K., Department of Physics, Govt. V.Y.T.PG. Auto. College, Chhattisgarh, Durg, India
Spectroscopic Studies and Theoretical Analysis of Some Selected Heterocycles
Seven derivatives of heterocycles benzimidazole, benzoxazole and benzothiazole were studied, five of which were synthesized and characterized. The molecular geometry and newlinespectroscopic data of the compounds in the ground state were calculated using the density functional theory (DFT/B3LYP) method with the 6-311++G(d,p) basis set. A comparison between the experimental and calculated data was attempted. Molecular electrostatic potential (MEP) and global reactivity parameters were deduced using theoretical calculations. HOMO-LUMO energy gap for each compound was determined by DFT and cyclic voltammetry. The cyclic voltammograms were recorded in acetonitrile solvent using lithium perchlorate as the supporting electrolyte. For all the compounds experimentally determined HOMO LUMO energy gap in polar solvent was lesser than that from DFT calculated energy gap. Using the HOMO-LUMO energy gap, global reactivity parameters were calculated. The effect of solvents of varying polarity on the absorption and emission spectra of the compounds was studied. Large excitation and emission energy differences were observed for all the selected heterocycles. The excitation and fluorescence spectra of selected heterocycles were recorded in eight solvents of different solvent polarity. It is evident from the excitation spectra that on increase of the solvent polarity, a bathochromic shift takes place for and#960;-and#960;* transition, and this is attributed to the high influence of solvent polarity in the excited state of heterocycle newlinecompared to its ground state. The dipole moments in the ground and the first excited state of heterocycle derivatives were newlinecalculated using Lippert-Mataga and Kawski-Chamma-Viallet methods. Guggenheim-Debye method was adopted to calculate ground state dipole moment. The dipole moments of the compounds were also calculated using Time Dependent-Density Functional Theory (TD-DFT). The dipole moment values of the compounds suggested that the excited state has more charge separation and thus becomes more polar.
Spectroscopic studies and theoretical analysis of some selected heterocycles /
Spectroscopic Studies of Galactic Field Be Stars
Be stars provide excellent opportunity to study circumstellar disks. But the disc formation mechanism of classical Be (CBe) stars- the Be phenomenon- is still poorly understood. This can be understood by studying CBe stars in various locations like clusters and fields. Spectra of Be stars show interesting emission lines of different elements like hydrogen, helium, iron, oxygen calcium, etc. These emission lines are valuable indicators in providing information about the circumstellar disks of Be stars. In the past several decades various aspects of Be stars have been studied. But literature review clearly indicates the need of further studies to frame a consolidated picture about Be phenomenon in CBe stars. It is found that especially, the region ?????? 7500 - 8800 ??? is a less studied, and thus poorly understood area in Be star research. But this area shows some interesting features like emission lines calcium, iron, oxygen and Paschen series. So, here we have studied a sample of 118 field CBe stars taken from the catalogue of Jaschek & Egret (1982) and whose medium resolution spectra were obtained in ?????? 3800 ?? 9000 ??? region during December, 2007 to January, 2009 with the 2.1-m Himalayan Chandra Telescope (HCT), located at Hanle, Ladakh, India and operated by the Indian Institute of Astrophysics (IIA), Bangalore. In this thesis, we present three works which investigate the disc properties of our 118 program Be stars by studying their spectral line features, focussing primarily on the less explored ?????? 7500 - 8800 ??? region. Firstly, we have analyzed the less studied Fe II 7712 ??? emission line for our stars to understand the possible Fe II line excitation mechanism in CBe stars. Our work predicts that Ly???fluorescence may be the possible Fe II line excitation mechanism in CBe stars. Secondly, we have studied the Ca II triplet emission lines for our stars and have developed a new technique for deblending Ca II components from their counterpart Paschen lines, thus providing a more efficient way to analyze Ca II lines. Analyzing Ca II lines through this technique, we suggest that the gas producing these lines is optically thick. This leads us to predict that Ca II lines may be an indicator of binarity in Be stars. Lastly, we have estimated the Balmer decrement values, D34 and D54 for 81 of our sample stars to shed light on opacity effects in Be star disks. Our work confirms the disc transient nature of Be stars through epoch-wise D34 and D54 variation study and also suggests that Be star disks are optically thick.
Spectroscopic Studies on Structurally Modified Anthraquinone Azo Hydrazone Tautomer: Theoretical and Experimental Approach
Anthraquinone; Antitubercular activity; DFT; Molecular docking; UV-absorption and photoluminescence
A series of unique four mono-azo substituted anthraquinone analogue were synthesized by using the anthraquinone components in the diazo-coupling technique. The FT-IR, 1H NMR, and HRMS, data were used to confirm the structure of the molecules, and spectroscopic techniques like UV-Vis, and photoluminescence spectroscopy were employed to estimate the photophysical properties of the molecules. The molecular optimized geometry and frontier molecular orbitals were estimated using density functional theory. Further, global chemical reactivity descriptors parameter was theoretically estimated using the value of the highest occupied molecular orbit and lowest unoccupied molecular orbits. The anti-tubercular action of the synthesised dyes were also examined. The results of this biological activity showed that N-isopropyl aniline combined with anthraquinone N-isopropyl aniline had superior anti-tubercular activity when compared to Rifampicin as the standard. As per molecular docking studies, the synthesized compound Q1 showed excellent binding energy (-10.0kcal/mol) among all compounds against the 3ZXR Protein. These results agreed with our in-vitro anti-TB activity results. 2023, The Author(s), under exclusive licence to Springer Science+Business Media, LLC, part of Springer Nature.
Shekharagouda P.; Mamatha G.P.; Nagaraju G.; Krishnamurthy C.; Gouthaman S.; Al-Asbahi B.A.; Al-Hada N.M.; Naik L.
https://doi.org/10.1007/s10895-023-03542-3 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85181504590&doi=10.1007%2fs10895-023-03542-3&partnerID=40&md5=ac548bcbe95c8fb90e085fb4fda1a711
Shekharagouda P., Department of Studies in Chemistry, Davangere University, Shivagangothri, Davanagere, Karnataka, 577 007, India; Mamatha G.P., Department of Studies in Chemistry, Davangere University, Shivagangothri, Davanagere, Karnataka, 577 007, India; Nagaraju G., Energy Material Research Laboratory, Department of Chemistry, Siddaganga Institute of Technology, Karnataka, Tumakuru, 572 103, India; Krishnamurthy C., Department of PG Studies and Research in Chemistry, Kuvempu University, Jnanasahyadri, Shankaraghatta, Karnataka, Shivamogga, 577451, India; Gouthaman S., Organic material lab, Department of Chemistry, School of Chemistry, Indian Institute of Technology, Uttarakhand, Roorkee, 247667, India; Al-Asbahi B.A., Department of Physics & Astronomy, College of Science, King Saud University, P.O. Box 2455, Riyadh, 11451, Saudi Arabia; Al-Hada N.M., Shandong Key Laboratory of Biophysics, Institute of Biophysics, Dezhou University, Dezhou, 253023, China; Naik L., Department of Physics and Electronics, CHRIST University, Bengaluru, Central Campus, Karnataka, Bengaluru, 560029, India
A series of unique four mono-azo substituted anthraquinone analogue were synthesized by using the anthraquinone components in the diazo-coupling technique. The FT-IR, 1H NMR, and HRMS, data were used to confirm the structure of the molecules, and spectroscopic techniques like UV-Vis, and photoluminescence spectroscopy were employed to estimate the photophysical properties of the molecules. The molecular optimized geometry and frontier molecular orbitals were estimated using density functional theory. Further, global chemical reactivity descriptors parameter was theoretically estimated using the value of the highest occupied molecular orbit and lowest unoccupied molecular orbits. The anti-tubercular action of the synthesised dyes were also examined. The results of this biological activity showed that N-isopropyl aniline combined with anthraquinone N-isopropyl aniline had superior anti-tubercular activity when compared to Rifampicin as the standard. As per molecular docking studies, the synthesized compound Q1 showed excellent binding energy (-10.0kcal/mol) among all compounds against the 3ZXR Protein. These results agreed with our in-vitro anti-TB activity results. The Author(s), under exclusive licence to Springer Science+Business Media, LLC, part of Springer Nature 2023.
Shekharagouda, Pampapathi; Mamatha, G.P.; Nagaraju, G.; Krishnamurthy, Chethan; Gouthaman, Siddan; Al-Asbahi, Bandar Ali; Al-Hada, Naif Mohammed; Naik, Lohit
Journal of Fluorescence;Volume;35;Issue;2;Article No.;103610;pp.819-833
https://doi.org/10.1007/s10895-023-03542-3 https://www.scopus.com/pages/publications/85181504590?origin=resultslist
Shekharagouda P., Department of Studies in Chemistry, Davangere University, ShivagangothriKarnataka, Davanagere, 577 007, India; Mamatha G.P., Department of Studies in Chemistry, Davangere University, ShivagangothriKarnataka, Davanagere, 577 007, India; Nagaraju G., Energy Material Research Laboratory, Department of Chemistry, Siddaganga Institute of Technology, Karnataka, Tumakuru, 572 103, India; Krishnamurthy C., Department of PG Studies and Research in Chemistry, Kuvempu University, Jnanasahyadri, Shankaraghatta, Karnataka, Shivamogga, 577451, India; Gouthaman S., Organic material lab, Department of Chemistry, School of Chemistry, Indian Institute of Technology, Uttarakhand, Roorkee, 247667, India; Al-Asbahi B.A., Department of Physics & Astronomy, College of Science, King Saud University, P.O. Box 2455, Riyadh, 11451, Saudi Arabia; Al-Hada N.M., Shandong Key Laboratory of Biophysics, Institute of Biophysics, Dezhou University, Dezhou, 253023, China; Naik L., Department of Physics and Electronics, CHRIST University, Bengaluru, Central Campus, Karnataka, Bengaluru, 560029, India
Spectroscopic study of Be-shell stars: 4 Her and 88 Her
emission-line, Be - circumstellar matter - stars; individual (4 Her, 88 Her) - stars; rotation- techniques; spectroscopic; stars
We present an optical spectroscopic study based on 41 spectra of 4 Her and 32 spectra of 88 Her, obtained over a period of 6 months. We estimate the rotational velocity of these stars from HeI lines in the blue spectral region (4000-4500 . We find that these stars are likely to be rotating at a fractional critical rotation of ?0.80. We measure the average I p/I c ratio to quantify the strength of the H? line and obtain 1.63 for 4 Her and 2.06 for 88 Her. The radius of the H? emission region is estimated to be Rd/R? ?5.0, assuming a Keplerian disk. These stars are thus found to be fast rotators with a relatively small H? emission region. We detect V/R variation of the H? spectral line during the observed period. We re-estimate the periods for both stars and obtain a period of ?46 d and its harmonic of 23.095 d for 4 Her, and a period of ?86 d for 88 Her. As these two cases are shell stars with binaries and have low H? EW with the emission region closer to the central star, the V/R variation and a change in period may be an effect of the binary on the circumstellar disk. 2016 National Astronomical Observatories, Chinese Academy of Sciences and IOP Publishing Ltd.
Bhat S.S.; Paul K.T.; Subramaniam A.; Mathew B.
Research in Astronomy and Astrophysics, Vol-16, No. 5
Bhat S.S., Department of Physics, Christ University, Bangalore, 560029, India; Paul K.T., Department of Physics, Christ University, Bangalore, 560029, India; Subramaniam A., Indian Institute of Astrophysics, II Block Kormangala, Bangalore, 560034, India; Mathew B., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai, 400005, India
Spectroscopic study of Herbig Ae/Be stars in the Galactic anti-centre region from LAMOST DR5
accretion; stars: emission-line; techniques: photometric; techniques: spectroscopic
We study a sample of 119 Herbig Ae/Be stars in the Galactic anti-centre direction using the spectroscopic data from large sky area multi-object fiber spectroscopic telescope survey program. Emission lines of hydrogen belonging to the Balmer and Paschen series, and metallic lines of species such as Fe ii, O i, Ca ii triplet are identified. A moderate correlation is observed between the emission strengths of H? and Fe ii 5169 suggesting a possible common emission region for Fe ii lines and one of the components of H?. We explored a technique for the extinction correction of the HAeBe stars using diffuse interstellar bands present in the spectrum. We estimated the stellar parameters such as age and mass of these HAeBe stars, which are found to be in the range 0.1-10 Myr and 1.5-10 M, respectively. We found that the mass accretion rate of the HAeBe stars in the Galactic anti-centre direction follows the relation ?acc ? M?3.12-0.34+0.21, which is similar to the relation derived for HAeBe stars in other regions of the Galaxy. The mass accretion rate of HAeBe stars is found to have a functional form of ?acc ? t-1.10.02 with age, in agreement with previous studies. 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Nidhi S.; Mathew B.; Shridharan B.; Arun R.; Anusha R.; Kartha S.S.
Monthly Notices of the Royal Astronomical Society, Vol-524, No. 4, pp. 5166-5181.
https://doi.org/10.1093/mnras/stad2067 https://www.scopus.com/inward/record.uri?eid=2-s2.0-85168674554&doi=10.1093%2fmnras%2fstad2067&partnerID=40&md5=e9fb93e28368df58a5209957a045f952
Nidhi S., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India; Mathew B., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India; Shridharan B., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India; Arun R., Indian Institute of Astrophysics (IIA), Sarjapur Road, Koramangala, Bangalore, 560034, India; Anusha R., Department of Physics & Astronomy, University of Western Ontario, London, N6A 5B7, ON, Canada; Kartha S.S., Department of Physics and Electronics, Christ (Deemed to Be University), Bangalore, 560029, India
Spectroscopic Study of Late-type Emission-line Stars Using the Data from LAMOST DR6
Line: identification; Stars: activity; Stars: late-type
Low-mass emission-line stars belong to various evolutionary stages, from pre-main-sequence young stars to evolved stars. In this work, we present a catalog of late-type (F0 to M9) emission-line stars from the LAMOST Data Release 6. Using the scipy package, we created a Python code that finds the emission peak at H? in all late-type stellar spectra. A data set of 38,152 late-type emission-line stars was obtained after a rigorous examination of the photometric quality flags and the signal-to-noise ratio of the spectra. Adopting well-known photometric and spectroscopic methods, we classified our sample into 438 infrared (IR) excess sources, 4669 post-main-sequence candidates, 9718 Fe/Ge/Ke sources, and 23,264 dMe sources. From a crossmatch with known databases, we found that 29,222 sources, comprising 65 IR excess sources, 7899 Fe/Ge/Ke stars, 17,533 dMe stars, and 3725 PtMS candidates, are new detections. We measured the equivalent width of the major emission lines observed in the spectra of our sample of emission-line stars. Furthermore, the trend observed in the line strengths of major emission lines over the entire late-type spectral range is analyzed. We further classified the sample into four groups based on the presence of hydrogen and calcium emission lines. This work presents a large data set of late-type emission-line stars, which can be used to study active phenomena in late-type stars. 2024 National Astronomical Observatories, CAS and IOP Publishing Ltd. All rights, including for text and data mining, AI training, and similar technologies, are reserved.
Edwin D.; Mathew B.; Shridharan B.; Valsan V.; Nidhi S.; Bhattacharyya S.; Kartha S.S.; Robin T.
Research in Astronomy and Astrophysics, Vol-24, No. 12
https://doi.org/10.1088/1674-4527/ad8f9b https://www.scopus.com/inward/record.uri?eid=2-s2.0-85211070102&doi=10.1088%2f1674-4527%2fad8f9b&partnerID=40&md5=be6d900bd3d42d47afbb3fda2b91a4db
Edwin D., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India; Mathew B., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India; Shridharan B., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India, Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai, 400005, India; Valsan V., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India; Nidhi S., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India, The Oxford College of Science, 17th, 32, 19th Main road, Sector 4, HSR Layout, Karnataka, Bengaluru, 560102, India; Bhattacharyya S., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India; Kartha S.S., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India; Robin T., Department of Physics and Electronics, CHRIST (Deemed to be University, Hosur Main Road, Bangalore, 560029, India