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Koushik Ghosh

Publications and source records attributed to Koushik Ghosh.

18 recordsLinked to original sources

Eukaryotes evade information storage-replication rate trade-off with endosymbiont assistance leading to larger genomes

Genome length varies widely among organisms, from compact genomes of prokaryotes to vast and complex genomes of eukaryotes. In this study, we theoretically identify the evolutionary pressures that may have driven this divergence in genome length. We use a parameter-free model to study genome length evolution under selection pressure to minimize replication time and maximize information storage capacity. We show that prokaryotes tend to reduce genome length, constrained by a single replication origin, while eukaryotes expand their genomes by incorporating multiple replication origins. We propose a connection between genome length and cellular energetics, suggesting that endosymbiotic organelles, mitochondria and chloroplasts, evolutionarily regulate the number of replication origins, thereby influencing genome length in eukaryotes. We show that the above two selection pressures also lead to strict equalization of the number of purines and their corresponding base-pairing pyrimidines within a single DNA strand, known as Chagraff's second parity rule, a hitherto unexplained observation in genomes of nearly all known species. This arises from the symmetrization of replichore length, another observation that has been shown to hold across species, which our model reproduces. The model also reproduces other experimentally observed phenomena, such as a general preference for deletions over insertions, and elongation and high variance of genome lengths under reduced selection pressure for replication rate, termed the C-value paradox. We highlight the possibility of regulation of the firing of latent replication origins in response to cues from the extracellular environment leading to the regulation of cell cycle rates in multicellular eukaryotes.

q-bio.GN

High nucleotide skew palindromic DNA sequences function as replication origins due to their unzipping propensity

Locations of DNA replication initiation in prokaryotes, called "origins of replication", are well-characterized. However, a mechanistic understanding of the sequence-dependence of the local unzipping of double-stranded DNA, the first step towards replication initiation, is lacking. Here, utilizing a Markov chain model that was created to address the directional nature of DNA unzipping and replication, we model the sequence dependence of local melting of double-stranded linear DNA segments. We show that generalized palindromic sequences with high nucleotide skews have a low kinetic barrier for local melting near melting temperatures. This allows for such sequences to function as replication origins. We support our claim with evidence for high-skew palindromic sequences within the replication origins of mitochondrial DNA, bacteria, archaea and plasmids.

q-bio.GN

High-Efficiency Photodetector Based On CVD-Grown WS$_2$ Monolayer

Future generation technologies demand high efficiency photodetectors to enable sensing and switching devices for ultrafast communication and machine vision. This require direct-band gap materials with high photosensitivity, high detectivity and high quantum efficiency. Monolayered two- Dimensional (2D)-Semiconductors based photodetectors are the most promising materials for such applications, although experimental realization has been limited due to unavailability of high quality sample. In the current manuscript, we report about WS$_2$ based photodetector having sensitivity of 290 AW-1 upon 405 nm excitation and incident power density as low as 0.06 mW/cm$^2$. The fabricated device shows detectivity of 52*10^14 with external quantum efficiency of 89*10$^3$%. The observed superior photo-response parameters of CVD grown WS$_2$ based photodetector as compared to Si-detectors establishes it capability to replace the Si-photodetectors with monolayered ultrathin device having superior performance parameters.

physics.ins-det

Impact of liquid coolant subcooling on boiling heat transfer and dryout in heat-generating porous media

The present article discusses the impact of liquid coolant subcooling on multiphase fluid flow and boiling heat transfer in porous media with internal heat generation. Although extremely relevant and important, only limited studies are available in the open literature on the effects of coolant subcooling in heat-generating porous media and hence, this requires a detailed analysis. The analysis is carried out using a developed computational model of multiphase fluid flow through clear fluid and porous media considering the relevant heat transfer and mass transfer phenomena. Results suggest that the qualitative nature of boiling heat transfer from the heat-generating porous body, with subcooled coolants, remain similar to that observed with a saturated coolant. Quantitative differences are, however, observed as a result of solid-liquid convective heat transfer, and competing mechanisms of boiling and condensation heat transfer, when subcooled liquid coolant is present. It is observed that a substantially larger heating power density is required - as coolant subcooling is increased - for achieving the same temperature rise in the porous body. Dryout power density at different coolant subcooling is also observed to follow a similar trend. The thermal energy removal limit is, hence, observed to be substantially enhanced in presence of subcooled coolants. Further, the dryout region within the porous body is observed to gradually shift towards its interior as the coolant subcooling is increased.

physics.flu-dyn

Reevaluating the performance of the Double Exponential Smoothing filter and its Control Parameters

Double Exponential Smoothing (DES) has broad application in various fields primarily as a forecasting tool. The values of the two smoothing parameters and , involved in DES, are traditionally chosen by the users which yield minimum MSE. In this work the authors endeavor to assess the performance of the DES as a filter and tried to suggest the suitable values of the and for which DES perform best as a filter. In this regard along with the conventional MSE method, the dependency of the stability and other aspects associated with the frequency response of the filter like transfer function, cutoff frequency, bandwidth and center frequency on the smoothing parameters are also studied. The values of the parameters close to 0.5 are found to be most appropriate when DES acts as a filter.

eess.SP

A Theoretical Model of Non-conservative Mass Transfer with Non-uniform Mass Accretion Rate in Close Binary Stars

Mass transfer in close binaries is often non-conservative and the modeling of this kind of mass transfer is mathematically challenging as in this case due to the loss of mass as well as angular momentum the governing system gets complicated and uncertain. In the present work a new mathematical model has been prescribed for the non-conservative mass transfer in a close binary system taking in to account the gradually decreasing profile of the mass accretion rate by the accreting star with respect to time as well as with respect to the increase in mass of the accreting star. The process of mass transfer is understood to occur up to a critical mass limit of the accreting star beyond which this process may cease to work.

gr-qc

Theoretical Model of Non-Conservative Mass Transfer with Uniform Mass Accretion Rate in Contact Binary Stars

In contact binaries mass transfer is usually non-conservative which ends into loss of mass as well as angular momentum in the system. In the present work we have presented a new mathematical model of the non-conservative mass transfer with a uniform mass accretion rate in a contact binary system with lower angular momentum. The model has been developed under the consideration of reverse mass transfer which may occur simultaneously with the original mass transfer as a result of the large scale circulations encircling the entire donor and a significant portion of the gainer. These circulations in contact binaries with lower angular momentum are caused by the overflow of the critical equipotential surface by both the components of the binary system making the governing system more intricate and uncertain.

astro-ph.SR

Time Variations of the Forbush Decrease Data

We have used Simple Denoising Algorithm using Wavelet Transform on the daily Forbush decrease data from the year 1967 to 2003. For this data we observe periodicity around 5-6, 11, 13, 15 and 24 years. For all the obtained peaks corresponding confidence levels are higher than 95%. We observe that the periodicity of around 5-6 years is common to solar flare data, major proton event data and solar neutrino flux data. Because of that common periodicity, it is suggested that Forbush decrease with the solar flare data and major solar proton event data together with solar neutrino flux variations, behave similarly and may have a common origin.

astro-ph

Tracing of Error in a Time Series Data

A physical (e.g. astrophysical, geophysical, meteorological etc.) data may appear as an output of an experiment or it may contain some sociological, economic or biological information. Whatever be the source of a time series data some amount of noise is always expected to be embedded in it. Analysis of such data in presence of noise may often fail to give accurate information. Although text book data filtering theory is primarily concerned with the presences of random, zero mean errors; but in reality, errors in data are often systematic rather than random. In the present paper we produce different models of systematic error in the time series data. This will certainly help to trace the systematic error present in the data and consequently that can be removed as possible to make the data compatible for further study.

astro-ph

An Adaptive Approach to Filter a Time Series Data

A physical data (such as astrophysical, geophysical, meteorological etc.) may appear as an output of an experiment or it may come out as a signal from a dynamical system or it may contain some sociological, economic or biological information. Whatever be the source of a time series data some amount of noise is always expected to be embedded in it. Analysis of such data in presence of noise may often fail to give accurate information. The method of filtering a time series data is a tool to clean these errors as possible as we can just to make the data compatible for further analysis. Here we made an attempt to develop an adaptive approach of filtering a time series and we have shown analytically that the present model can fight against the propagation of error and can maintain the positional importance in the time series very efficiently.

astro-ph

Time Variations of the Solar Neutrino Flux Data from Sudbury Neutrino Observatory

We have used the Ferraz-Mello Method of Date Compensated Discrete Fourier Transform on the solar neutrino flux data from the Sudbury Neutrino Observatory (SNO) in order to search for its time variation. We present results from Ferraz-Mello Method for both pure D2O and salt phase data sets from SNO. For the D2O data the obtained periods are 5.36, 14.99, 23.06, 40.31, 65.63, 115.03, 131.27, 152.67, 188.74, 294.49 and 412.79 days and for the salt phase data the periods are obtained at around 37.84, 43.89, 59.17, 67.48, 72.47, 78.52, 86.54, 95.91, 109.83 and 317.01 days. For all the obtained periods the levels of confidence are sufficiently higher than 95 percent.

hep-ph

Finite Variance Scaling Analysis of the Solar Neutrino Flux Data from Sage and Gallex-Gno Detectors

The scaling behaviours of the monthly solar neutrino flux data from (1) SAGE detector during the period from 1st January 1990 to 31st December 2000; (2) SAGE detector during the period from April 1998 to December 2001; (3) GALLEX detector during the period from May 1991 to January 1997; (4) GNO detector during the period from May 1998 to December 2001; (5) GALLEX-GNO detector (combined data) from May 1991 to December 2001 and (6) average of the data from GNO and SAGE detectors during the period from May 1998 to December 2001 are analysed. In the present analysis the monthly solar neutrino flux data in each case is processed through finite variance scaling method in order to find the corresponding Hurst exponent. The study reveals that the monthly solar neutrino flux data in 1), 3), 4), 5) and 6) exhibit anti-persistent behaviour (or, negative autocorrelation) and has underlying trends while the monthly solar neutrino flux data in 2) shows the nature of a long memory process.

hep-ph

Periodicities in Solar Neutrino Flux Data from Sage and Gallex-Gno Detectors

We have used both the Date-Compensated Discrete Fourier Transform and Periodogram analysis of the monthly solar neutrino flux data from (1) SAGE detector during the period from 1st January 1990 to 31st December 2000; (2) SAGE detector during the period from April 1998 to December 2001; (3) GALLEX detector during the period from May 1991 to January 1997; (4) GNO detector during the period from May 1998 to December 2001; (5) GALLEX-GNO detector (Combined data) from May 1991 to December 2001 and (6) average of the data from GNO and SAGE detectors during the period from May 1998 to December 2001. (1) exhibits periodicity around 19, 24 and 80-85 months. (2) shows periodicity around 1.5 months. For (3) we observe periodicity around 1.6, 2.5 and 19 months. For (4) periodicity is seen around 1.4 and 3.4 months. (5) gives periodicity around 1.7 and 19 months while (6) shows periodicity around 1.8 and 2.2 months. We have found almost similar periods in the solar flares, sunspot data, solar proton data which indicates that the solar activity cycle is due to the pulsating character of nuclear energy generation inside the sun.

hep-ph

Time Variations of the Superkamiokande Solar Neutrino Flux Data by Rayleigh Power Spectrum Analysis

We have used the Rayleigh Power Spectrum Analysis of the solar neutrino flux data from 1) 5-day-long samples from Super-Kamiokande-I detector during the period from June, 1996 to July, 2001; 2) 10 -day-long samples from the same detector during the same period and (3) 45-day long from the same detector during the same period. According to our analysis (1) gives periodicities around 0.25, 23.33, 33.75 and 42.75 months; (2) exhibits periodicities around 0.5, 1.0, 28.17, 40.67 and 52.5 months and (3) shows periodicities around 16.5 and 28.5 months. We have found almost similar periods in the solar flares, sunspot data, solar proton data.

astro-ph

Time Variations of the Solar Neutrino Flux Data from Sage and Gallex-Gno Detectors Obtained by Rayleigh Power Spectrum Analysis

We have used Rayleigh power spectrum analysis of the monthly solar neutrino flux data from (1) SAGE detector during the period from 1st January 1990 to 31st December 2000; (2) SAGE detector during the period from April 1998 to December 2001; (3) GALLEX detector during the period from May 1991 to January 1997; (4) GNO detector during the period from May 1998 to December 2001; (5) GALLEX-GNO detector (combined data) from May 1991 to December 2001 and (6) average of the data from GNO and SAGE detectors during the period from May 1998 to December 2001. (1) exhibits periodicity around 1.3, 4.3, 5.5, 6.3, 7.9, 8.7, 15.9, 18.7, 23.9, 32.9 and 48.7 months. (2) shows periodicity around 1.5, 2.9, 4.5, 10.1 months. For (3) we observe periodicity around 1.7, 18.7 and 26.9 months. For (4) periodicity is seen around 3.5, 5.5, 7.7 and 10.5 months. (5) gives periodicity around 1.7, 18.5, 28.5 and 42.1 months while (6) shows periodicity around 4.3, 6.9, 10.3 and 18.1 months. We have found almost similar periods in the solar flares, sunspot data, solar proton data which indicates that the solar activity cycle may be due to the variable character of nuclear energy generation inside the sun.

astro-ph

Fractal Nature of Solar Interior

Fractal method has been studied to understand the irregular and chaotic nature of any physical structure. Conventionally it is suggested that the solar interior is rigid in nature. Since solar neutrino flux is the indicator of the interior solar structure it is natural to study the solar neutrino flux source to find if the nuclear energy generation inside the sun is fractal in nature or not. At present there exist five solar neutrino experiments to detect neutrinos from the sun which can suggest which type of nuclear energy generation occurs inside the sun. Since we know that the solar atmosphere is irregular in nature many authors have studied this irregular nature by fractal analysis. In this regard we have studied solar neutrino flux data from 1) Homestake detector during the period from March, 1970 to April, 1994; 2) SAGE detector during the period from 1st January, 1990 to 31st December, 2000; 3) SAGE detector during the period from April, 1998 to December, 2001; 4) GALLEX detector during the period from May, 1991 to January, 1997; 5) GNO detector during the period from May, 1998 to December, 2001; 6) GALLEX-GNO detector (combined data) from May, 1991 to December, 2001; 7) average of the data from GNO and SAGE detectors during the period from May, 1998 to December, 2001; 8) 5-day-long samples from Super-Kamiokande-I detector during the period from June, 1996 to July,2001; 9) 10-day-long samples from Super-Kamiokande-I detector during the period from June,1996 to July,2001 and 10) 45-day-long samples from Super-Kamiokande-I detector during the period from June,1996 to July,2001 by fractal analysis and we have arrived at the conclusion that the solar neutrino flux data are fractal in nature.

hep-ph

Time Variations of the Solar Neutrino Flux Data from Sage and Gallex-Gno Detectors by Simple Denoising Algorithm Using Wavelet Transform

We have used Simple Denoising Algorithm using Wavelet Transform on the monthly solar neutrino flux data from (1) SAGE detector during the period from 1st January 1990 to 31st December 2000; (2) SAGE detector during the period from April 1998 to December 2001; (3) GALLEX detector during the period from May 1991 to January 1997; (4) GNO detector during the period from May 1998 to December 2001; (5) GALLEX-GNO detector (combined data) from May 1991 to December 2001 and (6) average of the data from GNO and SAGE detectors during the period from May 1998 to December 2001. (1) exhibits periodicity around 20, 27, 36, 70, 90 and 114 months. (2) shows periodicity around 21, 28, 31 and 33 months. For (3) we observe periodicity around 24, 40, 54, 57, 59, 62 and 64 months. For (4) periodicity is seen around 23, 30 and 34 months. (5) gives periodicity around 49, 57, 64, 74, 79, 88, 95 and 99 months while (6) shows periodicity around 24, 32, 35 and 38 months. We have found almost similar periods in the solar flares, sunspot data, solar proton data which indicates that the solar activity cycle may be due to the variable character of nuclear energy generation inside the sun.

hep-ph

Time Variations of the Superkamiokande Solar Neutrino Flux Data

We have used the Date-Compensated Discrete Fourier Transform and Periodogram analysis of the solar neutrino flux data from 1) 5-day-long samples from Super-Kamiokande-I detector during the period from June, 1996 to July, 2001; 2) 10-day-long samples from the same detector during the same period and 3) 45-day-long samples from the same detector during the same period. (1) exhibits periodicity around 0.21-0.22, 0.67-0.77, 1.15-1.98, 6.72-6.95, 12.05-13.24, 22.48-24.02, 33.50 and 40.73 months. (2) shows periodicity around 0.39-0.45, 1.31-2.23, 5.20-5.32, 9.43-11.65, 13.54-14.38, 24.54, 32.99 and 41.69 months. For (3) we observe periodicity around 1.61, 14.01, 24.06, 32.50 and 42.03 months. We have found almost similar periods in the solar flares, sunspot data, solar proton data (\barε>10 Mev) which indicates that the solar activity cycle may be due to the variable character of nuclear energy generation inside the sun.

hep-ph