E-Print Archive

There are 4553 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
The Solar Wind Disappearance Event of 11 May 1999: Source Region Evolution. View all abstracts by submitter

Janardhan Padmanabhan   Submitted: 2008-07-17 00:44

Context. A recent, detailed study of the well-known solar wind disappearance event of 11 May 1999 traced its origin to a coronal hole (CH) lying adjacent to a large active region (AR), AR8525 in Carrington rotation 1949. The AR was located at central meridian on 05 May 1999 when the flows responsible for this event began. We examine the evolution of the AR-CH complex during 5-6 May 1999 to study the changes that apparently played a key role in causing this disappearance event. Aims. To study the evolution of the solar source region of the disappearance event of 11 May 1999. Methods. Using images from the Soft X-ray Telescope (SXT), the Extreme-ultraviolet Imaging Telescope (EIT) and the Michelson Doppler Imager (MDI) to examine the evolution of the CH and AR complex at the source region of the disappearance event. Results. We find a dynamic evolution taking place in the CH-AR boundary at the source region of the disappearance event of 11 May 1999. This evolution, which is found to reduce the area of the CH, is accompanied by the formation of new loops in EUV images that are spatially and temporally correlated with emerging flux regions as seen in MDI data. Conclusions. In the period leading up to the disappearance event of 11 May 1999, our observations, during quiet solar conditions and in the absence of CMEs, provide the first clear evidence for Sun-Earth connection originating from an evolving AR-CH region located at central meridian. With the exception of corotating interacting regions (CIR), these observations provide the first link between the Sun and space weather e ects at 1 AU, arising from non-explosive solar events.

Authors: P. Janardhan, D. Tripathi, and H.E. Mason
Projects: None

Publication Status: Accepted for publication in A&A Letters
Last Modified: 2008-09-23 20:56
Go to main E-Print page  Slip-Squashing Factors as a Measure of Three-Dimensional Magnetic Reconnection  RHESSI Microflares: II. Implications for Loop Structure and Evolution  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Stability of slow magnetoacoustic and entropy waves in the solar coronal plasma with thermal misbalance
The chromosphere underneath a Coronal Bright Point
Characterising fast-time variations in the hard X-ray time profiles of solar flares using Solar Orbiter's STIX
The quiet sun at mm wavelengths as seen by ALMA
Explosive Events in the Quiet Sun Near and Beyond the Solar Limb Observed with the Interface Region Imaging Spectrograph (IRIS)
Multi-stage reconnection powering a solar coronal jet
A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons
Numerical Study on Excitation of Turbulence and Oscillation in Above-the-loop-top Region of a Solar Flare
Oscillatory reconnection as a plasma diagnostic in the solar corona
The independence of oscillatory reconnection periodicity from the initial pulse
Oscillatory Reconnection of a 2D X-point in a hot coronal plasma
Formation Of The Lyman Continuum During Solar Flares
MHD simulation of Solar Eruption from Active Region 11429 Driven by Photospheric Velocity Field
Unfolding Drift Effects for Cosmic Rays over the Period of the Sun's Magnetic Field Reversal
Problems in Observation and Identification of Torsional Waves in the Lower Solar Atmosphere
Solar Orbiter and SDO Observations, and Bifrost MHD Simulations of Small-scale Coronal Jets
Dominance of Bursty over Steady Heating of the 48 MK Coronal Plasma in a Solar Active Region: Quantification Using Maps of Minimum, Maximum, and Average Brightness
Solar flare hard X-rays from the anchor points of an eruptive filament
Plasmoids, Flows, and Jets During Magnetic Reconnection in a Failed Solar Eruption
Connecting Chromospheric Condensation Signatures to Reconnection-driven Heating Rates in an Observed Flare

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2000-2020 Solar Physics Group - Montana State University