Large-scale solar wind structures: occurrence rate and geoeffectiveness

Details Large-scale solar wind structures: occurrence rate and geoeffectiveness Large-scale solar wind structures: occurrence rate and geoeffectiveness

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216..648y&link_type=abstract

TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 648-651 (2010).

Computer Science

Databases

2

Solar Wind, Astronomical Catalogues, Solar Corona, Magnetic Fields, Weather, Particle Emission, Solar Wind, Astronomical Catalogs, Atlases, Sky Surveys, Databases, Retrieval Systems, Archives, Etc., Corona, Electric And Magnetic Fields, Solar Magnetism, Space Weather

Scientific paper

Large-scale phenomena in the solar wind are important elements of heliospheric physics and space weather. On the basis of the OMNI database of interplanetary measurements we identified large-scale structures of solar wind (SW types) for all time intervals during 1976-2000. Our classification includes quasi-steady types: (1) Heliospheric current sheet (HCS), (2) Slow and (3) Fast SW streams, respectively, from closed and open magnetic field structures in the solar corona, and disturbed types: (4) Corotating interaction regions (CIR-compressed regions between slow and fast SW streams), (5) SHEATH (compressed regions ahead of MC/EJECTA) and (6) Magnetic cloud (MC) and (7) EJECTA as well as (8) direct and (9) reverse interplanetary shocks (see catalog on site ftp://ftp.iki.rssi.ru/pub/omni/ and paper [1] ). We discuss several preliminary results obtained with our catalog (see more details in http://www.iki.rssi.ru./people/yyermol_inf.html) including effects on the Space Weather.

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