2,436 research outputs found
Temporal evolution of velocity structures in the solar wind
Generally poor correlations were obtained of solar wind flow speed measurements at one point in the ecliptic plane with measurements at the same point 28 days (one solar rotation) earlier or with measurements at other points in the ecliptic plane separated by 50 deg or more in solar longitude. This is evidence that either the flow speed is a very sensitive function of solar latitude or that temporal processes typically alter the speed of the wind emanating from particular solar regions on a time scale of about 4 days. From a measure of the persistence of the flow speed at the orbit of the earth, it appears that the temporal explanation is more likely to be the correct one
Solar cycle variation of real CME latitudes
With the assumption of radial motion and uniform longitudinal distribution of
coronal mass ejections (CMEs), we propose a method to eliminate projection
effects from the apparent observed CME latitude distribution. This method has
been applied to SOHO LASCO data from 1996 January to 2006 December. As a
result, we find that the real CME latitude distribution had the following
characteristics: (1) High-latitude CMEs ( where is
the latitude) constituted 3% of all CMEs and mainly occurred during the time
when the polar magnetic fields reversed sign. The latitudinal drift of the
high-latitude CMEs was correlated with that of the heliospheric current sheet.
(2) 4% of all CMEs occurred in the range .
These mid-latitude CMEs occurred primarily in 2000, near the middle of 2002 and
in 2005, respectively, forming a prominent three-peak structure; (3) The
highest occurrence probability of low-latitude () CMEs was
at the minimum and during the declining phase of the solar cycle. However, the
highest occurrence rate of low-latitude CMEs was at the maximum and during the
declining phase of the solar cycle. The latitudinal evolution of low-latitude
CMEs did not follow the Sp\"{o}rer sunspot law, which suggests that many CMEs
originated outside of active regions.Comment: 4 pages, 4 figures, accepted by ApJ Lette
Multiple spacecraft observations of interplanetary shocks: Characteristics of the upstream ULF turbulence
All interplanetary shocks observed by ISEE-3 and either ISEE-1 or ISEE-2 or both in 1978 and 1979 are examined for evidence of upstream waves. In order to characterize the properties of these shocks it is necessary to determine accurate shock normals. An overdetermined set of equations were inverted to obtain shock normals, velocities and error estimates for all these shocks. Tests of the method indicate it is quite reliable. Using these normals the Mach number and angle were between the interplanetary magnetic field and the shock normal for each shock. The upstream waves were separated into two classes: whistler mode precursors which occur at low Mach numbers and upstream turbulence whose amplitude at Mach numbers greater than 1.5 is controlled by the angle of the field to the shock normal. The former waves are right hand circularly polarized and quite monochromatic. The latter waves are more linearly polarized and have a broadband featureless spectrum
Towards a Java Subtyping Operad
The subtyping relation in Java exhibits self-similarity. The self-similarity
in Java subtyping is interesting and intricate due to the existence of wildcard
types and, accordingly, the existence of three subtyping rules for generic
types: covariant subtyping, contravariant subtyping and invariant subtyping.
Supporting bounded type variables also adds to the complexity of the subtyping
relation in Java and in other generic nominally-typed OO languages such as C#
and Scala. In this paper we explore defining an operad to model the
construction of the subtyping relation in Java and in similar generic
nominally-typed OO programming languages. Operads, from category theory, are
frequently used to model self-similar phenomena. The Java subtyping operad, we
hope, will shed more light on understanding the type systems of generic
nominally-typed OO languages.Comment: 13 page
The imperial war museum’s social interpretation project
This report represents the output from research undertaken by University of Salford and MTM
London as part of the joint Digital R&D Fund for Arts and Culture, operated by Nesta, Arts
Council England and the AHRC. University of Salford and MTM London received funding from
the programme to act as researchers on the Social Interpretation (SI) project, which was led by
the Imperial War Museum (IWM) and their technical partners, The Centre for Digital
Humanities, University College London, Knowledge Integration, and Gooii. The project was
carried out between October 2011 and October 2012
The determination of shock ramp width using the noncoplanar magnetic field component
We determine a simple expression for the ramp width of a collisionless fast
shock, based upon the relationship between the noncoplanar and main magnetic
field components. By comparing this predicted width with that measured during
an observation of a shock, the shock velocity can be determined from a single
spacecraft. For a range of low-Mach, low-beta bow shock observations made by
the ISEE-1 and -2 spacecraft, ramp widths determined from two-spacecraft
comparison and from this noncoplanar component relationship agree within 30%.
When two-spacecraft measurements are not available or are inefficient, this
technique provides a reasonable estimation of scale size for low-Mach shocks.Comment: 6 pages, LaTeX (aguplus + agutex);
packages:amsmath,times,graphicx,float, psfrag,verbatim; 3 postscript figures
called by the file; submitted to Geophys. Res. Let
Can Streamer Blobs prevent the Buildup of the Interplanetetary Magnetic Field?
Coronal Mass Ejections continuously drag closed magnetic field lines away
from the Sun, adding new flux to the interplanetary magnetic field (IMF). We
propose that the outward-moving blobs that have been observed in helmet
streamers are evidence of ongoing, small-scale reconnection in streamer current
sheets, which may play an important role in the prevention of an indefinite
buildup of the IMF. Reconnection between two open field lines from both sides
of a streamer current sheet creates a new closed field line, which becomes part
of the helmet, and a disconnected field line, which moves outward. The blobs
are formed by plasma from the streamer that is swept up in the trough of the
outward moving field line. We show that this mechanism is supported by
observations from SOHO/LASCO. Additionally, we propose a thorough statistical
study to quantify the contribution of blob formation to the reduction of the
IMF, and indicate how this mechanism may be verified by observations with
SOHO/UVCS and the proposed NASA STEREO and ESA Polar Orbiter missions.Comment: 7 pages, 2 figures; accepted by The Astrophysical Journal Letters;
uses AASTe
CSM-392 PhD in Open Constraint Satisfaction Technical Report 1: The Simple Supply Chain Model (SSCM)
On the Cause of Supra-Arcade Downflows in Solar Flares
A model of supra-arcade downflows (SADs), dark low density regions also known
as tadpoles that propagate sunward during solar flares, is presented. It is
argued that the regions of low density are flow channels carved by
sunward-directed outflow jets from reconnection. The solar corona is
stratified, so the flare site is populated by a lower density plasma than that
in the underlying arcade. As the jets penetrate the arcade, they carve out
regions of depleted plasma density which appear as SADs. The present
interpretation differs from previous models in that reconnection is localized
in space but not in time. Reconnection is continuous in time to explain why
SADs are not filled in from behind as they would if they were caused by
isolated descending flux tubes or the wakes behind them due to temporally
bursty reconnection. Reconnection is localized in space because outflow jets in
standard two-dimensional reconnection models expand in the normal (inflow)
direction with distance from the reconnection site, which would not produce
thin SADs as seen in observations. On the contrary, outflow jets in spatially
localized three-dimensional reconnection with an out-of-plane (guide) magnetic
field expand primarily in the out-of-plane direction and remain collimated in
the normal direction, which is consistent with observed SADs being thin.
Two-dimensional proof-of-principle simulations of reconnection with an
out-of-plane (guide) magnetic field confirm the creation of SAD-like depletion
regions and the necessity of density stratification. Three-dimensional
simulations confirm that localized reconnection remains collimated.Comment: 16 pages, 5 figures, accepted to Astrophysical Journal Letters in
August, 2013. This version is the accepted versio
Anomalous aspects of magnetosheath flow and of the shape and oscillations of the magnetopause during an interval of strongly northward interplanetary magnetic field
On 15 Feb. 1978, the orientation of the interplanetary magnetic field (IMF) remained steadily northward for more than 12 hours. The ISEE 1 and 2 spacecraft were located near apogee on the dawn side flank of the magnetotail. IMP 8 was almost symmetrically located in the magnetosheath on the dusk flank and IMP 7 was upstream in the solar wind. Using plasma and magnetic field data, we show the following: (1) the magnetosheath flow speed on the flanks of the magnetotail steadily exceeded the solar wind speed by 20 percent; (2) surface waves with approximately a 5-min period and very non-sinusoidal waveform were persistently present on the dawn magnetopause and waves of similar period were present in the dusk magnetosheath; and (3) the magnetotail ceased to flare at an antisunward distance of 15 R(sub E). We propose that the acceleration of the magnetosheath flow is achieved by magnetic tension in the draped field configuration for northward IMF and that the reduction of tail flaring is consistent with a decreased amount of open magnetic flux and a larger standoff distance of the subsolar magnetopause. Results of a three-dimensional magnetohydrodynamic simulation support this phenomenological model
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