منابع مشابه
Merged interaction regions at 1 AU
[1] We discuss the existence of large, complex merged interaction regions (MIRs) in the solar wind near Earth. MIRs can have configurations that cause more prolonged geomagnetic effects than a single flow structure. A MIR or successive MIRs can produce relatively long lasting Forbush decreases at 1 AU. We illustrate MIRs at 1 AU with two examples (MIR-1 and MIR-2) seen by WIND and ACE in the in...
متن کاملSolar wind turbulence and shear: A superposed‐epoch analysis of corotating interaction regions at 1 AU
[1] A superposed‐epoch analysis of ACE and OMNI2 measurements is performed on 27 corotating interaction regions (CIRs) in 2003–2008, with the zero epoch taken to be the stream interface as determined by the maximum of the plasma vorticity. When the measurements are rotated into the local‐Parker‐spiral coordinate system, the shear is seen to be abrupt. Converging flows are seen; about half of th...
متن کاملLarge-scale Magnetic Field Fluctuations and Development of the 1999–2000 Global Merged Interaction Region: 1–60 Au
We use a multifluid, spherically symmetric, MHD model with neutral atoms and pickup protons, with 1999 solar wind data at 1 AU as input, to calculate the magnetic field strength (B) profiles that would be observed at various points between 1 and 60 AU with a resolution of 1 day over an interval of 1 yr. These temporal profiles show radial evolution of the multiscale fluctuations in B near solar...
متن کاملEvolution of Magnetic Fields in Corotating Interaction Regions from 1 to 95 Au: Order to Chaos
We discuss the large-scale heliospheric magnetic field strength fluctuations as a function of distance from the Sun during the declining phase of a solar cycle, based on a one-dimensional, MHD, three-fluid model with observations made at 1 AU during 1995 as input. We consider daily averages of the magnetic field strength, B, as a function of time for a 1 year interval. The model predicts that B...
متن کاملCorotating Interaction Regions at High Latitudes
Ulysses observed a stable strong CIR from early 1992 through 1994 during its first journey into the southern hemisphere. After the rapid latitude scan in early 1995, Ulysses observed a weaker CIR from early 1996 to mid-1997 in the northern hemisphere as it traveled back to the ecliptic at the orbit of Jupiter. These two CIRs are the observational basis of the investigation into the latitudinal ...
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ژورنال
عنوان ژورنال: Journal of Geophysical Research
سال: 2003
ISSN: 0148-0227
DOI: 10.1029/2003ja010088