Stellar analogs for the solar wind have proven to be frustratingly difficult to detect directly. However, these stellar winds can be studied indirectly by observing the interaction regions carved out by the collisions between these winds and the interstellar medium (ISM). These interaction regions are called "astrospheres", analogous to the "heliosphere" surrounding the Sun. The heliosphere and...

OBJECTIVE To examine the psychometric validity and reliability of the incident reporting culture questionnaire (IRCQ; in Chinese) following an exploration of the reporting culture perceived by hospital nurses in Taiwan. DESIGN Scale development with psychometric examination and a cross-sectional study. SETTING Ten teaching hospitals. PARTICIPANTS A total of 1064 nurses participated with a...

Exoplanets that orbit close to their host stars are much more highly irradiated than their solar system counterparts. Understanding the thermal structures and appearances of these planets requires investigating how their atmospheres respond to such extreme stellar forcing. We present spectroscopic thermal emission measurements as a function of orbital phase ("phase-curve observations") for the ...

A the middle of the last century, the French philosopher Auguste Comte speculated that knowledge of the chemical composition of stars would be forever beyond the reach of science. Scarcely a decade later, however, the new science of spectroscopy was bom-and with it the ability to determine the chem­ ical makeup of stellar atmospheres. 1his development precipitated a revolution in physics. The s...

2 GENERAL CHARACTERISTICS 4 2.1 Stellar Atmospheres . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4 2.2 Accretion Disks . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5 2.3 Approximate models . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 2.4 Word of Caution . . . . . . . . . . . . . . . . . . . . . . . . . . . ...

We discuss prospects of using multi-dimensional time-dependent simulations to study the atmospheres of brown dwarfs and extrasolar giant planets, including the processes of convection, radiation, dust formation, and rotation. We argue that reasonably realistic simulations are feasible, however, separated into two classes of local and global models. Numerical challenges are related to potentiall...

in this research, the high-energy planetary mill was employed to produce nanocrystalline ti-50al(γ)(at%) powders. initial powders were mechanically alloyed in 99.9999% and 90% purities of argon and also air atmosphere with alloying times up to 50h. the effect of impurity of argon atmosphere on the microstructure and the rate of phase transformation of ti-50al were investigated during mechanical...

The problems of escape of a planetary atmosphere is reviewed. Formulae are derive for the rates of loss of mass and angular momentum from a unit area and from the whole planetary surface. The resulting formulae are applied to find the residence times of H, O, N2, O2 and CO2 in Martian atmosphere. All constituents are so stable while hydrogen is never stable and cannot be retained to my extent.

Planetary nebulae (PNe) are circumstellar gas ejected during an intense mass-losing phase in the the lives of asymptotic giant branch stars. PNe have a stunning variety of shapes, most of which are not spherically symmetric. The debate over what makes and shapes the circumstellar gas of these evolved, intermediate mass stars has raged for two decades. Today the community is reaching a consensus...

[1] Sprites are a spectacular type of transient luminous events which occur above thunderstorms immediately after lightning. They have shapes of giant jellyfish, carrots, or columns and last tens of milliseconds. In Earth’s atmosphere, sprites mostly emit in red and blue wavelengths from excited N2 and N2 + and span a vertical range between 50 and 90 km above the surface. The emission spectra, ...