Development of an Ionosphere-Plasmasphere-Polar Wind Model and Studies of Storms and Substorms

2008 ◽  
Author(s):  
Larry C. Gardner ◽  
Herbert C. Carlson
Keyword(s):  
Polar Wind ◽  
Wind Model ◽  
Storms And Substorms

scholarly journals On the puzzling line spectrum of the B[e]-supergiant R 4 of the SMC

1987 ◽  
Vol 122 ◽  
pp. 439-440
Author(s):  
F.-J. Zickgraf ◽  
B. Wolf
Keyword(s):  
General Scheme ◽  
Exceptional Case ◽  
Magellanic Clouds ◽  
Absorption Lines ◽  
Line Spectrum ◽  
Wind Component ◽  
Early Type ◽  
Polar Wind ◽  
Wind Model ◽  
Two Component

The early-type supergiants of the Magellanic Clouds (MC's) include a class of objects, the B[e] -supergiants, which are described in detail in Zickgraf et al. (1985, 1986) who suggested a two-component wind model consisting of a cool, dense and slowly expanding disk-like equatorial wind component and a hot line-driven fast polar wind. This model could explain many properties of most of the B[e] -supergiants as e. g. the occurrence of “shell” absorption lines. R 4 of the SMC, however, although well fitting to the general scheme of B[e) -supergiants exhibits several pecularities of its line spectrum, which make this particular star an exceptional case among the B[e] -supergiants of the MC's.

Coupling the Generalized Polar Wind Model to Global Magnetohydrodynamics

2016 ◽  
pp. 179-194 ◽  
Author(s):  
Daniel T. Welling ◽  
Abdallah R. Barakat ◽  
J. Vincent Eccles ◽  
R. W. Schunk ◽  
Charles R. Chappell
Keyword(s):  
Polar Wind ◽  
Wind Model

scholarly journals Decay of the Dst field of geomagnetic disturbance after substorm onset and its implication to storm-substorm relation

1996 ◽  
Vol 14 (6) ◽  
pp. 608-618 ◽  
Author(s):  
T. Iyemori ◽  
D. R. K. Rao
Keyword(s):  
Ring Current ◽  
Geomagnetic Storms ◽  
Sharp Decrease ◽  
Geomagnetic Disturbance ◽  
Substorm Onset ◽  
Significant Development ◽  
H Index ◽  
Magnetospheric Tail ◽  
Storms And Substorms ◽  
Substorm Onsets

Abstract. In order to investigate the causal relationship between magnetic storms and substorms, variations of the mid-latitude geomagnetic indices, ASY (asymmetric part) and SYM (symmetric part), at substorm onsets are examined. Substorm onsets are defined by three different phenomena; (1) a rapid increase in the mid-latitude asymmetric-disturbance indices, ASY-D and ASY-H, with a shape of so-called `mid-latitude positive bay\\'; (2) a sharp decrease in the AL index; (3) an onset of Pi2 geomagnetic pulsation. The positive bays are selected using eye inspection and a pattern-matching technique. The 1-min-resolution SYM-H index, which is essentially the same as the hourly Dst index except in terms of the time resolution, does not show any statistically significant development after the onset of substorms; it tends to decay after the onset rather than to develop. It is suggested by a simple model calculation that the decay of the magnetospheric tail current after substorm onset is responsible for the decay of the Dst field. The relation between the IMF southward turning and the development of the Dst field is re-examined. The results support the idea that the geomagnetic storms and substorms are independent processes; that is, the ring-current development is not the result of the frequent occurrence of substorms, but that of enhanced convection caused by the large southward IMF. A substorm is the process of energy dissipation in the magnetosphere, and its contribution to the storm-time ring-current formation seems to be negligible. The decay of the Dst field after a substorm onset is explained by a magnetospheric energy theorem.

Horizontal wind model (HWM) (1990)

1992 ◽  
Vol 40 (4) ◽  
pp. 556-557 ◽  
Author(s):  
A.E. Hedin
Keyword(s):  
Horizontal Wind ◽  
Wind Model

scholarly journals The Kinematics of Quasar Broad Emission Line Regions Using a Disk-Wind Model

2017 ◽  
Vol 34 ◽  
Author(s):  
Suk Yee Yong ◽  
Rachel L. Webster ◽  
Anthea L. King ◽  
Nicholas F. Bate ◽  
Matthew J. O’Dowd ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Inclination Angle ◽  
Opening Angle ◽  
Line Profiles ◽  
Wind Model ◽  
Disk Wind ◽  
Reverberation Mapping ◽  
Broad Emission ◽  
Line Region

AbstractThe structure and kinematics of the broad line region in quasars are still unknown. One popular model is the disk-wind model that offers a geometric unification of a quasar based on the viewing angle. We construct a simple kinematical disk-wind model with a narrow outflowing wind angle. The model is combined with radiative transfer in the Sobolev, or high velocity, limit. We examine how angle of viewing affects the observed characteristics of the emission line. The line profiles were found to exhibit distinct properties depending on the orientation, wind opening angle, and region of the wind where the emission arises.At low inclination angle (close to face-on), we find that the shape of the emission line is asymmetric, narrow, and significantly blueshifted. As the inclination angle increases (close to edge-on), the line profile becomes more symmetric, broader, and less blueshifted. Additionally, lines that arise close to the base of the disk wind, near the accretion disk, tend to be broad and symmetric. Single-peaked line profiles are recovered for the intermediate and equatorial wind. The model is also able to reproduce a faster response in either the red or blue sides of the line profile, consistent with reverberation mapping studies.

scholarly journals Signatures of storm sudden commencements in geomagnetic H, Y and Z fields at Indian observatories during 1958−1992

1999 ◽  
Vol 17 (11) ◽  
pp. 1426-1438 ◽  
Author(s):  
R. G. Rastogi
Keyword(s):  
Sri Lanka ◽  
Equatorial Electrojet ◽  
Interplanetary Shocks ◽  
Low Latitude ◽  
Disturbance Vector ◽  
Storm Sudden Commencement ◽  
Interplanetary Physics ◽  
Sudden Commencements ◽  
Electrojet Current ◽  
Storms And Substorms

Abstract. The work describes an intensive study of storm sudden commencement (SSC) impulses in horizontal (H), eastward (Y) and vertical (Z) fields at four Indian geomagnetic observatories between 1958–1992. The midday maximum of ΔH has been shown to exist even at the low-latitude station Alibag which is outside the equatorial electrojet belt, suggesting that SSC is associated with an eastward electric field at equatorial and low latitudes. The impulses in Y field are shown to be linearly and inversely related to ΔH at Annamalainagar and Alibag. The average SC disturbance vector is shown to be about 10–20°W of the geomagnetic meridian. The local time variation of the angle is more westerly during dusk hours in summer and around dawn in the winter months. This clearly suggests an effect of the orientation of shock front plane of the solar plasma with respect to the geomagnetic meridian. The ΔZ at SSC have a positive impulse as in ΔH. The ratio of ΔZ/ΔH are abnormally large exceeding 1.0 in most of the cases at Trivandrum. The latitudinal variation of ΔZ shows a tendency towards a minimum over the equator during the nighttime hours. These effects are explained as (1) resulting from the electromagnetic induction effects due to the equatorial electrojet current in the subsurface conducting layers between India and Sri Lanka, due to channelling of ocean currents through the Palk Strait and (2) due to the concentration of induced currents over extended latitude zones towards the conducting graben between India and Sri Lanka just south of Trivandrum.Key words. Interplanetary physics (interplanetary shocks) · Ionosphere (equatorial ionosphere) · Magnetospheric physics (storms and substorms)

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