Improved solar Lyman α irradiance modeling from 1947 through 1999 based on UARS observations

Details Improved solar Lyman α irradiance modeling from 1947 through 1999 based on UARS observations Improved solar Lyman α irradiance modeling from 1947 through 1999 based on UARS observations

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000jgr...10527195w&link_type=abstract

Journal of Geophysical Research, Volume 105, Issue A12, p. 27195-27216

Astronomy and Astrophysics

Astrophysics

129

Solar Physics, Astrophysics, And Astronomy: Solar Activity Cycle, And Astronomy: Solar Irradiance, And Astronomy: Transition Region, And Astronomy: Ultraviolet Emissions

Scientific paper

The solar Lyman α radiation is the brightest solar vacuum ultraviolet (VUV: λ<200nm) emission, and this radiation is deposited in Earth's atmosphere above 70 km. The Lyman α irradiance and its variability are therefore important for many studies of the Earth's upper atmosphere. A long-term data set of the solar Lyman α irradiance from 1947 through 1999 is constructed using the measurements from the Atmospheric Explorer E (AE-E), the Solar Mesospheric Explorer (SME), and the Upper Atmosphere Research Satellite (UARS) along with predictions from proxy models to fill in data gaps and to extrapolate back to 1947. The UARS measurement is used as the reference, and the AE-E and SME measurements and the proxy models are adjusted to agree with the UARS values. The estimated 1-σ uncertainty for this long-term Lyman α time series is 10%. The average solar rotation (27-day) variability in Lyman α is 9% from this composite times series, and the solar rotation variability averaged over 2 years at solar minimum and maximum conditions is 5 and 11%, respectively. The average solar cycle (11-year) variability is a factor of 1.5 when the data are smoothed over 2 years, and the extreme Lyman α variability is a factor of 2.1. The Lyman α irradiances averaged over 2 years during solar minimum and maximum conditions are 3.7 and 5.6×1011photonss-1cm-2, respectively. The proxy models include three components to better fit the UARS measurements; nonetheless, there remain differences between the proxy models and the observed Lyman α irradiance, which are related to the source of the Lyman α radiation being different than that for the proxies. The available proxies are primarily chromospheric and coronal emissions, whereas the Lyman α variability is manifested more in the transition region. It is shown that emissions throughout the chromosphere, transition region, and corona vary differently mainly because their contrasts for active network and plage components are different. A transition region proxy is needed to improve the empirical proxy models of solar irradiance, and this composite Lyman α time series could serve as a proxy for other transition region emissions.

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