Solar EUV and UV spectral irradiances and solar indices

Floyd, L.; Newmark, J. S.; Cook, J. W.; Herring, L. C.; McMullin, D. R.

doi:10.1016/j.jastp.2004.07.013

Cited by 93 publications

(92 citation statements)

References 43 publications

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“…Mg c/w is the ratio of the chromospheric core to the photospheric wings of the compound Mg II absorption line measured in the vicinity of the 280 nm UV irradiance. This index is considered a reasonably good indicator for the changing emission of faculae and other bright solar features (Heath and Schlesinger, 1986;Floyd et al, 2005).…”

Section: Data Descriptionmentioning

confidence: 99%

Active region properties and irradiance variations

Baranyi

Pap

2012

Advances in Space Research

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Total solar irradiance (TSI) has been measured for more than three decades. These observations demonstrate that total irradiance changes on time scales ranging from minutes to years and decades. Considerable efforts have been made to understand the physical origin of irradiance variations and to model the observed changes using measures of sunspots and faculae. In this paper, we study the short-term variations in TSI during the declining portion and minimum of solar cycle 22 and the rising portion of cycle 23 (1993 -1998). This time interval of low solar activity allows us to study the effect of individual sunspot groups on TSI in detail. In this paper, we indicate that the effect of sunspot groups on total irradiance may depend on their type in the Zürich classification system and/or their evolution, and on their magnetic configuration. Some uncertainties in the data and other effects are also discussed.

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Section: Data Descriptionmentioning

confidence: 99%

Active region properties and irradiance variations

Baranyi

Pap

2012

Advances in Space Research

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“…The solar radio flux at 10.7 cm (F10.7) is a widely, if not the most widely used index of solar activity: this quantity describes solar UV forcing of the upper atmosphere and is measured daily since 1947 (Floyd et al 2005;Tapping 2013). Many operational space weather models and also climate models use the F10.7 index as their prime solar input.…”

Section: Introductionmentioning

confidence: 99%

The 30 cm radio flux as a solar proxy for thermosphere density modelling

Wit

Bruinsma²

2017

J. Space Weather Space Clim.

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The 10.7 cm radio flux (F10.7) is widely used as a proxy for solar UV forcing of the upper atmosphere. However, radio emissions at other centimetric wavelengths have been routinely monitored since the 1950 s, thereby offering prospects for building proxies that may be better tailored to space weather needs. Here we advocate the 30 cm flux (F30) as a proxy that is more sensitive than F10.7 to longer wavelengths in the UV and show that it improves the response of the thermospheric density to solar forcing, as modelled with DTM (Drag Temperature Model). In particular, the model bias drops on average by 0-20% when replacing F10.7 by F30; it is also more stable (the standard deviation of the bias is 15-40% smaller) and the density variation at the the solar rotation period is reproduced with a 35-50% smaller error. We compare F30 to other solar proxies and discuss its assets and limitations.

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“…The most popular proxy for the EUV/UV band is solar radio flux at 10.7 cm, which is better known as the F10.7 index. Other proxies include the sunspot number and the MgII core-to-wing index (Floyd et al 2005;Snow et al 2014). Although long and continuous EUV/UV observations are now becoming more routinely available, proxies are still likely to be preferred for a while, partly because so many atmosphere models have been tuned to them.…”

Section: Future Of Planetary Space Weathermentioning

confidence: 99%

What characterizes planetary space weather?

Lilensten

Coates

Déhant

et al. 2014

Astron Astrophys Rev

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Space weather has become a mature discipline for the Earth space environment. With increasing efforts in space exploration, it is becoming more and more necessary to understand the space environments of bodies other than Earth. This is the background for an emerging aspect of the space weather discipline: planetary space weather. In this article, we explore what characterizes planetary space weather, using some examples throughout the solar system. We consider energy sources and timescales, the characteristics of solar system objects and interaction processes. We

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Solar EUV and UV spectral irradiances and solar indices

Cited by 93 publications

References 43 publications

Active region properties and irradiance variations

Active region properties and irradiance variations

The 30 cm radio flux as a solar proxy for thermosphere density modelling

What characterizes planetary space weather?

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