IACETH Institute for Atmospheric and Climate Science Representation of Middle Range Energy Electrons in the Chemistry-Climate Model SOCOL Pavle Arsenovic.

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Presentation transcript:

IACETH Institute for Atmospheric and Climate Science Representation of Middle Range Energy Electrons in the Chemistry-Climate Model SOCOL Pavle Arsenovic * Andrea Stenke *, Eugene Rozanov *,**, Thomas Peter * * Institute for Atmospheric and Climate Science, ETH Zürich ** PMOD/WRC, Davos ISSI Meeting, January

IACETH Institute for Atmospheric and Climate Science Outline Types of energetic particles Model framework Middle range energy electrons AIMOS Ionization rates Solar wind data Flow speed and dynamic pressure Z component of IMF Correlation between Ionization rates and solar wind Outlook 2

IACETH Institute for Atmospheric and Climate Science Energetic particles Galactic cosmic rays (up to 5x10 13 MeV) Solar protons (up to 500 MeV) 3 Low energy electrons (<30 keV) Middle energy electrons ( keV) High energy electrons (300 keV to 10 MeV) Turunen et al., 2008

IACETH Institute for Atmospheric and Climate Science Model framework SOCOL3-MPIOM 4 GCR SPE LEE MEE HEE

IACETH Institute for Atmospheric and Climate Science Middle range energy electrons Energy keV Originate from outer radiation belt Produce HOx and NOx between 60 and 80 km HOx and NOx deplete ozone 5

IACETH Institute for Atmospheric and Climate Science Data used for linking Ionization rates from Atmosphere Ionization Module Osnabrück (AIMOS) Satellite solar wind data:  Flow speed  Dynamic pressure  Z component of IMF 6

IACETH Institute for Atmospheric and Climate Science 7 AIMOS Ionization Rates Vertical resolution – 8 levels between 60 and 80 km Horizontal resolution – 96x48 Time resolution – from 2004 to 2010, 2 hourly

IACETH Institute for Atmospheric and Climate Science 8

IACETH Institute for Atmospheric and Climate Science 9

IACETH Institute for Atmospheric and Climate Science 10

IACETH Institute for Atmospheric and Climate Science 11

IACETH Institute for Atmospheric and Climate Science 12 AIMOS Ionization Rate

IACETH Institute for Atmospheric and Climate Science 13 Solar Wind Data Solar wind flow speed (v) Solar wind dynamic pressure (p) p = c N p V p 2 Z component of interplanetary magnetic field (Bz) Time resolution – from 2004 to 2010, 5 minutes

IACETH Institute for Atmospheric and Climate Science 14

IACETH Institute for Atmospheric and Climate Science 15

IACETH Institute for Atmospheric and Climate Science 16

IACETH Institute for Atmospheric and Climate Science 17 Bz of interplanetary magnetic field

IACETH Institute for Atmospheric and Climate Science 18

IACETH Institute for Atmospheric and Climate Science 19

IACETH Institute for Atmospheric and Climate Science Outlook Correlation between AIMOS Ionization rates and solar wind data is low for 2-hourly and daily data Yearly data correlation shows much higher correlation (~0.9) Time lag between the peaks in v, bz and ionization rates? Current state: Including AIMOS ionization rates (daily) in SOCOL and compare results with runs with no MEE (in progress) 20