A theory for the origin of the slow solar wind is described. Recent papers have demonstrated that magnetic flux moves across coronal holes as a result of the interplay between the differential rotation of the photosphere and the non-radial expansion of the solar wind in more rigidly rotating coronal holes. This flux will be deposited at low latitudes and should reconnect with closed magnetic lo...

A&G • February 2013 • Vol. 54 1.25 The continuous flow of matter that escapes out of the solar gravitational well is known as the solar wind. As the material flows out of the Sun, it is accelerated to between 400 and 800 km s. Through this continuous flow of material, the Sun loses more than one million tonnes every second. But this is just a tiny fraction, corresponding to 2 × 10 of a solar ma...

Wind affects adversely the cooling tower thermal performance. A field investigation was carried out to study the thermal performance of Heller cooling towers under wind conditions, involving measurement of wind velocity and its direction around the cooling tower, and obtaining water flow rates and temperatures at the cooling tower inlet and outlet. Results show that air suction at the tower top...

Studies of quasar absorption lines reveal that the low density intergalactic medium at z ∼ 3 is enriched to 10−10 solar metallicity. This enrichment may have occurred in an early generation of Population III stars at redshift z ∼> 10, by protogalaxies at 6 ∼< z ∼< 10, or by larger galaxies at 3 ∼< z ∼< 6. This paper addresses the third possiblity by calculating the enrichment of the IGM at z ∼>...

One of the fundamental astrobiology questions is how life has formed in our Solar System. In this context the formation and stability of abiotic organic molecules such as CH4, formic acid and amino acids, is important for understanding how organic material has formed and survived shocks and energetic particle impact from winds in the early Solar System. Shock waves have been suggested as a plau...

[1] To determine the efficacy of turbulence in the solar wind, the amount of mixing of the solar wind plasma is quantified. If magnetohydrodynamic turbulence in the solar wind acts as does Navier-Stokes turbulence, the chunk mixture of scalar quantities in the solar wind plasma should evolve with time. In particular, (1) the sizes of plasma chunks should decrease with distance from the Sun owin...

Nonlinear three dimensional, time dependent, fluid simulations of whistler wave turbulence are performed to investigate role of whistler waves in solar wind plasma turbulence in which characteristic turbulent fluctuations are characterized typically by the frequency and length scales that are respectively bigger than ion gyro frequency and smaller than ion gyro radius. The electron inertial len...

Low frequency magnetic fluctuations generated by solar wind/cometary ion distributions cause pitch-angle scattering of cometary ions. The nature of this pitch angle scattering is examined by means of one-dimensional hybrid simulations, in which newborn ions are created at a constant rate, and for various injection angles, o•, relative to the magnetic field. Pitch angie scattering in the quasipe...

We demonstrate a software application designed for the display and interactive manipulation of 3D heliospheric volume data, such as solar wind density, velocity and magnetic field. The Volume Explorer software exploits the capabilities of the Volume Pro 1000 (from TeraRecon, Inc.), a low-cost 64-bit PCI board capable of rendering a 512-cubed array of volume data in real time at up to 30 frames ...

Using data obtained between 1991 and 1996 with the SWICS instrument (Solar Wind Ion Composition Spectrometer) aboard the Ulysses spacecraft, a long time average of the (4He/3He) isotopic ratio of 2450 ± 460 in coronal hole dominated solar wind is derived. To assess the influence of inefficient Coulomb friction in the inner corona and to infer the solar photospheric abundance ratio from the sola...