National Air And Space Museum Washington DC

Wissenschaft

Weitere ähnliche Inhalte

Andere mochten auch

Introduction to Algorithms

pppepito86

Why Ben Stein Is Wrong About History & Science

In our thesis work, we try to find out the efficiency of several sorting algorithms and generate a comparative report according to performance, based on experimental data size and data order for all algorithm. To do this we have researched, analyzed about 9 different types of well-known sorting algorithms. We convert the algorithms to programmable code, compile and run with different set of data. We keep the sorting algorithm’s description as it is. We give focus on, how the algorithms work, considering their total operation count (assignment count, comparison count) and complexity based on our same data set for all algorithm. We write programming code for each sorting algorithm in C programming language. In our investigation, we have also worked with big and small data for different cases (ordered, pre-ordered, random, disordered) and put their result in different tables. We show the increasing ratio to compare the result. we also show the data in graphical chart for view comparative report in same window. We mark their efficiency with point and ranked them. At last we discussed their result of efficiency in a single table. We modify the merge sort and try to make an improved tri-merge sorting algorithm that is more efficient than marge sort. Theoretically if we divide and conquer with higher number its result is better, some paper exists on it, but to manage the algorithm, there cost lot of operations count. Like, if we consider quadratic divide-conquer, its manage complexly is huge than binary divide-conquer that why we generally use binary merge. We found trimerge is theoretically and practically true based on investigation data set. Tri-marge take some more compare operation for manage and sort when data remain 1 or 2 at last stage, whereas binary merge don’t need such compare. But for big data size tri-merge gain lot of operation count that give significant result that declare tri-merge is more efficient than merge sort algorithm. We also experiment with penta-merge algorithm which give more better result but algorithm and implementation is too complex. We shall try to define the tri-merge algorithm so that it can be used to implement in any programming language. It will help students, researchers to use the algorithm, as like we got the various algorithm structure over the internet.

Tri Merge Sorting Algorithm

sPen Data Management

Ds 4

Dc parent 14 2

Was There A Darwinian Revolution

simple-sorting algorithms

Ravirajsinh Chauhan

Ancient Ideas of Creation & Evolution

American Astronautical Society

Introduction to Information Technology ch 02_a

Shahi Raz Akhtar

Google

vibhabehl

How We Got Where We Are: 40 Years of Planning...

Sorting algorithms

Edward Blurock

Google at a glance 1998 - 2008

Andreas Jaffke

One Long Argument

Introduction to Information Technology ch 01_b

Shahi Raz Akhtar

History of Google Local from 2004-2011

Mike Blumenthal

Introduction to "Origins, Evolution & Creation"

Andere mochten auch (18)

Introduction to Algorithms

Why Ben Stein Is Wrong About History & Science

Tri Merge Sorting Algorithm

sPen Data Management

Ds 4

Dc parent 14 2

Was There A Darwinian Revolution

simple-sorting algorithms

Ancient Ideas of Creation & Evolution

Introduction to Information Technology ch 02_a

Google

How We Got Where We Are: 40 Years of Planning...

Sorting algorithms

Google at a glance 1998 - 2008

One Long Argument

Introduction to Information Technology ch 01_b

History of Google Local from 2004-2011

Introduction to "Origins, Evolution & Creation"

Mehr von Shivakumar Patil

Case Study: Project and Change Management

Standing Ovation Award

GE Treasury Award

Shivakumar_Pat on Back

Denodo Installation

Rhode island

Stamford Museum & Nature Center Photos

Howe Caverns

New York City

Mianus River Gorge – Preserve Trail

EL_Certificate

HotJupiters are amongthebest-studied exoplanets, but it is still poorly understood how their chemical composition and cloud properties vary with longitude. Theoretical models predict that clouds may condense on the nightside and that molecular abundances can be driven out of equilibrium by zonal winds. Here we report a phase-resolved emission spectrum of the hot Jupiter WASP-43b measured from 5–12µ 5–12µ 5–12µm with JWST’s Mid-Infrared Instrument (MIRI). 1524 ±35 1524 ±35 and 863±23 The spectra reveal a large day–night temperature contrast (with average brightness temperatures of 1524 ± 35 863 ±23 863 ±23Kelvin, respectively) and evidence for water absorption at all orbital phases. Comparisons with three-dimensional atmospheric models show that both the phase curve shape and emission spectra strongly suggest the presence of nightside clouds which become optically thick to thermal emission at pressures greater than ∼100mbar. The dayside is consistent with a cloudless atmosphere above the mid-infrared photosphere. Con3trary to expectations from equilibrium chemistry but consistent with disequilibrium kinetics models, methane is not detected on the nightside (2σ upper limit of 1–6 parts per million, depending on model assumptions).

Mehr von Shivakumar Patil (11)

Case Study: Project and Change Management

Standing Ovation Award

GE Treasury Award

Shivakumar_Pat on Back

Denodo Installation

Rhode island

Stamford Museum & Nature Center Photos

Howe Caverns

New York City

Mianus River Gorge – Preserve Trail

EL_Certificate

Kürzlich hochgeladen

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

Understanding circumstellar disks is of prime importance in astrophysics, however, their birth process remains poorly constrained due to observational and numerical challenges. Recent numerical works have shown that the small-scale physics, often wrapped into a sub-grid model, play a crucial role in disk formation and evolution. This calls for a combined approach in which both the protostar and circumstellar disk are studied in concert. Aims. We aim to elucidate the small scale physics and constrain sub-grid parameters commonly chosen in the literature by resolving the star-disk interaction. Methods. We carry out a set of very high resolution 3D radiative-hydrodynamics simulations that self-consistently describe the collapse of a turbulent dense molecular cloud core to stellar densities. We study the birth of the protostar, the circumstellar disk, and its early evolution (< 6 yr after protostellar formation). Results. Following the second gravitational collapse, the nascent protostar quickly reaches breakup velocity and sheds its surface material, thus forming a hot (∼ 103 K), dense, and highly flared circumstellar disk. The protostar is embedded within the disk, such that material can flow without crossing any shock fronts. The circumstellar disk mass quickly exceeds that of the protostar, and its kinematics are dominated by self-gravity. Accretion onto the disk is highly anisotropic, and accretion onto the protostar mainly occurs through material that slides on the disk surface. The polar mass flux is negligible in comparison. The radiative behavior also displays a strong anisotropy, as the polar accretion shock is shown to be supercritical whereas its equatorial counterpart is subcritical. We also f ind a remarkable convergence of our results with respect to initial conditions. Conclusions. These results reveal the structure and kinematics in the smallest spatial scales relevant to protostellar and circumstellar disk evolution. They can be used to describe accretion onto regions commonly described by sub-grid models in simulations studying larger scale physics.

Formation of low mass protostars and their circumstellar disks

Context. Determining the size distribution of asteroids is key to understanding the collisional history and evolution of the inner Solar System. Aims. We aim to improve our knowledge of the size distribution of small asteroids in the main belt by determining the parallaxes of newly detected asteroids in the Hubble Space Telescope (HST) archive and subsequently their absolute magnitudes and sizes. Methods. Asteroids appear as curved trails in HST images because of the parallax induced by the fast orbital motion of the spacecraft. Taking into account the trajectory of this latter, the parallax effect can be computed to obtain the distance to the asteroids by fitting simulated trajectories to the observed trails. Using distance, we can obtain the absolute magnitude of an object and an estimation of its size assuming an albedo value, along with some boundaries for its orbital parameters. Results. In this work, we analyse a set of 632 serendipitously imaged asteroids found in the ESA HST archive. Images were captured with the ACS/WFC and WFC3/UVIS instruments. A machine learning algorithm (trained with the results of a citizen science project) was used to detect objects in these images as part of a previous study. Our raw data consist of 1031 asteroid trails from unknown objects, not matching any entries in the Minor Planet Center (MPC) database using their coordinates and imaging time. We also found 670 trails from known objects (objects featuring matching entries in the MPC). After an accuracy assessment and filtering process, our analysed HST asteroid set consists of 454 unknown objects and 178 known objects. We obtain a sample dominated by potential main belt objects featuring absolute magnitudes (H) mostly between 15 and 22 mag. The absolute magnitude cumulative distribution logN(H > H0) ∝ αlog(H0) confirms the previously reported slope change for 15 < H < 18, from α ≈ 0.56 to α ≈ 0.26, maintained in our case down to absolute magnitudes of around H ≈ 20, and therefore expanding the previous result by approximately two magnitudes. Conclusions. HST archival observations can be used as an asteroid survey because the telescope pointings are statistically randomly oriented in the sky and cover long periods of time. They allow us to expand the current best samples of astronomical objects at no extra cost in regard to telescope time.

Pulmonary drug delivery system M.pharm -2nd sem P'ceutics

sakshisoni2385

Nanoparticles synthesis and characterization

kaibalyasahoo82800

Recombination DNA Technology (Nucleic Acid Hybridization )

aarthirajkumar25

Biopesticide (2).pptx .This slides helps to know the different types of biop...

RohitNehra6

Hubble Asteroid Hunter III. Physical properties of newly found asteroids

Context. WASP-76 b has been a recurrent subject of study since the detection of a signature in high-resolution transit spectroscopy data indicating an asymmetry between the two limbs of the planet. The existence of this asymmetric signature has been confirmed by multiple studies, but its physical origin is still under debate. In addition, it contrasts with the absence of asymmetry reported in the infrared (IR) phase curve. Aims. We provide a more comprehensive dataset of WASP-76 b with the goal of drawing a complete view of the physical processes at work in this atmosphere. In particular, we attempt to reconcile visible high-resolution transit spectroscopy data and IR broadband phase curves. Methods. We gathered 3 phase curves, 20 occultations, and 6 transits for WASP-76 b in the visible with the CHEOPS space telescope. We also report the analysis of three unpublished sectors observed by the TESS space telescope (also in the visible), which represents 34 phase curves. Results. WASP-76 b displays an occultation of 260±11 and 152±10 ppm in TESS and CHEOPS bandpasses respectively. Depending on the composition assumed for the atmosphere and the data reduction used for the IR data, we derived geometric albedo estimates that range from 0.05 ± 0.023 to 0.146 ± 0.013 and from <0.13 to 0.189 ± 0.017 in the CHEOPS and TESS bandpasses, respectively. As expected from the IR phase curves, a low-order model of the phase curves does not yield any detectable asymmetry in the visible either. However, an empirical model allowing for sharper phase curve variations offers a hint of a flux excess before the occultation, with an amplitude of ∼40 ppm, an orbital offset of ∼−30◦ , and a width of ∼20◦ . We also constrained the orbital eccentricity of WASP-76 b to a value lower than 0.0067, with a 99.7% confidence level. This result contradicts earlier proposed scenarios aimed at explaining the asymmetry observed in high-resolution transit spectroscopy. Conclusions. In light of these findings, we hypothesise that WASP-76 b could have night-side clouds that extend predominantly towards its eastern limb. At this limb, the clouds would be associated with spherical droplets or spherically shaped aerosols of an unknown species, which would be responsible for a glory effect in the visible phase curves.

Bacterial Identification and Classifications

Areesha Ahmad

GBSN - Microbiology (Unit 1)

Areesha Ahmad

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

Jupiter’s moon Io hosts extensive volcanism, driven by tidal heating. The isotopic composition of Io's inventory of volatile chemical elements, including sulfur and chlorine, reflects its outgassing and mass loss history, and thus records information about its evolution. We used millimeter observations of Io’s atmosphere to measure sulfur isotopes in gaseous SO2 and SO, and chlorine isotopes in gaseous NaCl and KCl. We find 34S/32S = 0.0595 ± 0.0038 (equivalent to δ34S = +347 ± 86‰), which is highly enriched compared to average Solar System values and indicates that Io has lost 94 to 99% of its available sulfur. Our measurement of 37Cl/35Cl = 0.403 ± 0.028 (δ37Cl = +263 ± 88‰) shows that chlorine is similarly enriched. These results indicate that Io has been volcanically active for most (or all) of its history, with potentially higher outgassing and mass-loss rates at earlier times.

Isotopic evidence of long-lived volcanism on Io