Existence Of Corona Research Articles

Community Perceptions on Corona Virus- A Survey of Garhshankar Block of Hoshiarpur district, Punjab

Nature’s forces seem to have rallied around on reclaim their upset balance. Humans have disturbed the natural forces by exploiting Earth’s resources in an irresponsible manner. The history of our planet has witnessed several pandemics that threatened to successively decimate mankind some examples are the Antonine Plague (165 AD), Leprosy (11th century), the Black Death (1350), the Goat Plague of London (1665), First Cholera Pandemic (1817), HIV/AIDS (1981), and the most recent COVID-19 or Corona (2021) that is coming in several phases. All these geographically widespread epidemics have led to millions of deaths around the globe. The Corona virus appears to have mutated in India in 2021 after the world had paid its toll in 2020. Lives everywhere have been experiencing an almost complete lockdown to contain this viral disease. The focal point of this research paper is to determine the awareness levels of the population with respect to the COVID-19 crisis. Do people believe in the existence of Corona? What precautions are they taking to protect themselves? How confident are they of the effectiveness of the vaccine? The study was carried out in the Garhshankar block of Hoshiarpur district in Punjab among 305 respondents through an online questionnaire methodology to ascertain their views on the ongoing pandemic. The findings of the study are expected to be the pre-cursor of launching programs to address the needs of the community in facing the pandemic situation successfully.

Underwater Networked Wireless Sensor Data Collection for Computational Intelligence Techniques: Issues, Challenges, and Approaches.

Underwater wireless sensor networks (UWSNs) is emerging as an advance terminology for monitoring and controlling the underwater aquatic life. This technology determines the undiscovered resources present in the water through computational intelligence (CI) techniques. CI here pertains to the capability of a system to acquire a specific task from data or experimental surveillance below the water. In today’s time data is considered as the identity for everything that exists in nature, whether that data is related to human beings, machines or any type of device like internet of underwater things (IoUT). The collected data should be correct, complete and fulfill the requirements of a particular task to be done. Underwater data collection is very tough because of sensors mobility due to water drift 3 meters/sec, crest and trough. A lot of packet drop also exists due to underwater conditions that hurdles the data collection process. Various techniques already exists for efficient collection of data below the water but these are not properly classified. This manuscript has summarized the concept of data collection in UWSN along with its classification based on routing. Also, a short discussion about existence of CORONA below the water along with water purification is carried out. Furthermore, some data routing approaches are also analyzed on the basis of quality of service parameters and the current challenges to be tackled during data collection are also discussed.

Magnetic activity in thick accretion disks and associated observable phenomena. 2: Flux storage

In paper I, we have studied the conditions under which flux tubes are expelled from adiabatic thick accretion disks. In the present paper, we explore a few other models of thick disks, where flux tubes could be stored. We show that flux tubes with sufficiently weak fields are not expelled out if they move adiabatically inside an isothermal disk; they continue to oscillate around mean equipotential surfaces inside the disk. If the field in the flux tube is amplified due to the shear, they are eventually expelled away. We explore a `toy' model also, where the entropy increase outwards from the center of the thick disk and find a similar behavior. Flux storage in the disk, as in the case of the sun, in general, enhances the possibility of sustained magnetic activity formation of coronae in the chimney region. The existence of coronae on the disk surface may explain the short-time variability in the spectra of Blazars and the emission of energetic particles from AGNs and Quasars. It may also supply matter to the cosmic jets through magnetized winds.

The physics of the galactic halo gas

The available data speak in favour of space and time inhomogeneity of gaseous corona of our Galaxy. The observedCIV and SiIV ions are formed mainly by fast photons and localized inHII-clouds of the galactic halo. On the other hand, theNV ions are thermally ionized and localized in the gas corresponding to a transformation of hot intercloud coronal gas in theHII-clouds. TheHII-clouds exhibit downward the gas flow. The galactic fountain can eject the interstellar matter up to height of 1 kpc. Such ejections may be also displayed inCIV, SiIV, and partiallyNV, and partiallyNV absorptions. But large gaseous corona extending up to 3–5 kpc proves to be mass-unbalanced. It is possible that the existence of corona is evidence for violent star formation in the galactic disc in the recent past.

Positive glow corona in quasi-uniform fields

Results of an experimental study of positive glow corona in nitrogen-oxygen mixtures under quasi-uniform fields are presented. Measurements of electrical and optical characteristics of the corona were preformed. Both average and time resolved measurements were performed. Measurements of the electrical fields at the electrodes were made during the existence of corona. A theoretical model based upon available initiation by photodetachment of electrons from oxygen ions is proposed.

Chromospheres, Coronae, and Mass Loss in Stars Hotter than the Sun

AbstractReviews of the mass-loss characteristics of OB stars have been published recently, and the present review therefore emphasizes the A and F stars and very recent results on O and B stars. For the F stars, chromospheric indicators are present in the form of emission lines, seen in visible and ultraviolet wavelengths. Winds are present in A supergiants, but not in main sequence stars, although at least a few of the latter are X-ray sources, indicating the possible existence of coronae. Most OB supergiants are X-ray sources as well, indicating, along with the presence of super-ionization, that these stars have coronae. On the main sequence, the O stars and some B stars (including Be stars in many cases) have mass loss with highly-ionized species in the wind. The winds in the O and B stars are commonly variable. The mass-loss rates do not show a simple dependence on luminosity, contrary to the predictions for radiatively-driven winds.

An analysis of ultraviolet resonance lines and the possible existence of coronae in O stars

view Abstract Citations (52) References (21) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS An analysis of ultraviolet resonance lines and the possible existence of coronae in O stars. Olson, G. L. Abstract A method for analyzing resonance line profiles is developed to determine the degree of ionization and the spatial distribution of ions in stellar winds. This technique is a two-parameter adaptation of the Sobolev approximation for line transfer. Families of line profiles are presented for two velocity laws, several radial dependences of the ionization, and the full range of ionic abundance. These profiles can be applied to interpreting observed resonance lines of any wavelength and oscillator strength in any star through simple scaling laws. The star Puppis (O4f) is analyzed in this manner to determine the ionic structure of its wind. This ionic structure is then compared to that predicted by a model consisting of a cool wind with a thin hot (T 5 x 106 K) corona at the base of the flow. This model is proposed as an alternative to "warm" wind models, which require electron temperatures near 200,000 K, to explain the high ionization potential ions such as O+ that are observed. Even though the coronal radiation is attenuated by the opacities of all the abundant elements, enough hard photons penetrate to produce O+ by the Auger process throughout the stellar wind. The coronal size required to fit the observed ionic structure of Pup has an emission which is very close to the X-ray upper limits set by the ANS satellite. Limits on the gas temperature and the radiation temperature in the far-UV can be obtained through this analysis. Subject headings: line profiles - stars: coronae - stars: early-type - stars: winds - ultraviolet: spectra Publication: The Astrophysical Journal Pub Date: November 1978 DOI: 10.1086/156592 Bibcode: 1978ApJ...226..124O Keywords: Line Spectra; O Stars; Stellar Coronas; Stellar Winds; Ultraviolet Spectra; Abundance; Optical Resonance; Optical Thickness; Plasma Composition; Plasma Temperature; Radial Velocity; Stellar Models; Astrophysics; Line Profiles:O Stars; O Stars:Stellar Coronae; O Stars:Stellar Winds; O Stars:UV Spectra full text sources ADS | data products SIMBAD (1)

Nebular observations and stellar coronae

We examine the ways in which nebular observations of He II lambda4686 can be used to infer the existence of coronae or hot winds of early-type stars. The O VI lambdalambda3811, 3834 doublet is seen in the spectra of some central stars of planetary nebulae, and several authors have considered this to be evidence of a coronal wind. Observations of NGC 6751 reinforce this view by showing that radiative equilibrium model atmospheres cannot sufficiently photoexcite the O VI transitions without producing too much nebular emission at lambda4686. The hot gas in the coronal model produces a significant amount of radiation at energies above 54 eV; therefore, the He II Zanstra temperatures can be affected. Discrepancies between the He II Zanstra temperatures and effective temperatures derived from other methods may indicate coronal emission from planetary nebula central stars.Observations of diffuse nebulae about Population I early-type stars may also prove useful in detecting hot winds. The Lamers and Morton model of the wind of the O4f star xi Pup predicts a small amount of He/sup +/ ionizing radiation. If NGC 7635 is associated with the Of star BD +60/sup 0/2522, then the observation of nebular emission at lambda4686 may indicate coronal emission.