Social indeterminacy and Quine's indeterminacy thesis

This article examines whether Willard Van Orman Quine’s indeterminacy thesis can be sustained. The argument from above, Quine argues, can derive indeterminacy as its conclusion. I will argue that the indeterminacy claim cannot be sustained. I further argue that Quine changed the formulation of the underdetermination of theory by evidence (UTE) argument from what Duhem said to the Quine/Pierce meaning verification view, in order use the new formulation of UTE to imply indeterminacy. Given all that, we see when we apply the old UTE argument we only arrive at underdetermination of theory by evidence, and that applies to all sciences, philosophy and knowledge, including philosophy of language

Exploring Searle's Social Ontology

In this short article, I will explore John Searle’s social ontology project from the perspective of social epistemology. The outcome of my analysis is that language is decisive for the collective acquisition and production of knowledge. I agree with Searle regarding the exposure of language as a central constitutive component of social forms of knowledge, a component that plays a significant role in the development of social epistemology

Exploring Searle's Social Ontology

In this short article, I will explore John Searle’s social ontology project from the perspective of social epistemology. The outcome of my analysis is that language is decisive for the collective acquisition and production of knowledge. I agree with Searle regarding the exposure of language as a central constitutive component of social forms of knowledge, a component that plays a significant role in the development of social epistemology

The young cluster NGC 2282 : a multi-wavelength perspective

We present the analysis of the stellar content of NGC~2282, a young cluster in the Monoceros constellation, using deep optical $BVI$ and IPHAS photometry along with infrared (IR) data from UKIDSS and $Spitzer$-IRAC. Based on the stellar surface density analysis using nearest neighborhood method, the radius of the cluster is estimated as $\sim$ 3.15\arcmin. From optical spectroscopic analysis of 8 bright sources, we have classified three early B-type members in the cluster, which includes, HD 289120, a previously known B2V type star, a Herbig Ae/Be star (B0.5 Ve) and a B5 V star. From spectrophotometric analyses, the distance to the cluster has been estimated as $\sim$ 1.65 kpc. The $K$-band extinction map is estimated using nearest neighborhood technique, and the mean extinction within the cluster area is found to be A$_V$ $\sim$ 3.9 mag. Using IR colour-colour criteria and H$_\alpha$-emission properties, we have identified a total of 152 candidate young stellar objects (YSOs) in the region, of which, 75 are classified as Class II, 9 are Class I YSOs. Our YSO catalog also includes 50 H$_\alpha$-emission line sources, identified using slitless spectroscopy and IPHAS photometry data. Based on the optical and near-IR colour-magnitude diagram analyses, the cluster age has been estimated to be in the range of 2 $-$ 5 Myr, which is in agreement with the estimated age from disc fraction ($\sim$ 58\%). Masses of these YSOs are found to be $\sim$ 0.1$-$2.0 M$_\odot$. Spatial distribution of the candidate YSOs shows spherical morphology, more or less similar to the surface density map.Comment: 16 pages, 19 Figure

Boundary Shear Stress Distribution in Smooth and Rough Open Channel Flow

Boundary shear distribution in open channel flow is a crucial issue for river engineer and researchers working in this area.An experimental investigation has been carried out to measure the boundary shear stress distribution along the wetted perimeter of the smooth and rough channel using piston tube technique the accuracy of the method has been compared and checked with another convention method,NDM, VDM,MPM,Velocity Profile Method and energy gradient approach.The boundary shear along the bed and wall of the channel are different for different flow depth and for different roughness conditions.The percentage of boundary shear carried by the wall and bed has been analysed and found to depends on upon non-dimensional geometry and hydraulic parameters such as Aspect ratio,Reynolds number and Froude’s number.A multi linear regression model has been applied to predict the boundary shear distribution for bed.The equation is useful to calculate the roughness coefficient (friction factor) of the wall and bed of the channel separately,which further determines the composite roughness of the open channel flow accuracy.The methodology has been applied successfully to calculate the stage discharge relationship of the open channel flow.The methodology has been validated against other experimental data, other researcher’s models and Natural Rive

The low-mass population in the young cluster Stock 8: Stellar properties and Initial Mass Function

The evolution of HII regions/supershells can trigger a new generation of stars/clusters at their peripheries, with environmental conditions that may affect the initial mass function, disk evolution and star formation efficiency. In this paper we study the stellar content and star formation processes in the young cluster Stock 8, which itself is thought to be formed during the expansion of a supershell. We present deep optical photometry along with JHK and 3.6, 4.5 {\mu}m photometry from UKIDSS and Spitzer-IRAC. We use multi-color criteria to identify the candidate young stellar objects in the region. Using evolutionary models, we obtain a median log(age) of ~6.5 (~3.0 Myr) with an observed age spread of ~0.25 dex for the cluster. Monte Carlo simulations of the population of Stock 8, based on estimates for the photometric uncertainty, differential reddening, binarity, and variability, indicate that these uncertainties introduce an age spread of ~0.15 dex. The intrinsic age spread in the cluster is ~0.2 dex. The fraction of young stellar objects surrounded by disk is ~35%. The K-band luminosity function of Stock 8 is similar to that of the Trapezium cluster. The IMF of Stock 8 has a Salpeter- like slope at >0.5 Msun and the IMF flattens and peaks at ~0.4 Msun, below which declines into the substellar regime. Although Stock 8 is surrounded by several massive stars, there seems to be no severe environmental effect in the form of IMF due to the proximity of massive stars around the cluster.Comment: Accepted for publication in Ap

Comparative analysis of two discretizations of Ricci curvature for complex networks

We have performed an empirical comparison of two distinct notions of discrete Ricci curvature for graphs or networks, namely, the Forman-Ricci curvature and Ollivier-Ricci curvature. Importantly, these two discretizations of the Ricci curvature were developed based on different properties of the classical smooth notion, and thus, the two notions shed light on different aspects of network structure and behavior. Nevertheless, our extensive computational analysis in a wide range of both model and real-world networks shows that the two discretizations of Ricci curvature are highly correlated in many networks. Moreover, we show that if one considers the augmented Forman-Ricci curvature which also accounts for the two-dimensional simplicial complexes arising in graphs, the observed correlation between the two discretizations is even higher, especially, in real networks. Besides the potential theoretical implications of these observations, the close relationship between the two discretizations has practical implications whereby Forman-Ricci curvature can be employed in place of Ollivier-Ricci curvature for faster computation in larger real-world networks whenever coarse analysis suffices.Comment: Published version. New results added in this version. Supplementary tables can be freely downloaded from the publisher websit