Solar radio fluxes as indices of solar activity

Nicolet, M.; Bossy, L.

doi:10.1016/0032-0633(85)90096-0

Cited by 17 publications

(11 citation statements)

References 3 publications

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“…There has been much research into relating the 10.7-cm flux to the other activity measures, such as Ca II, UV and EUV spectral lines (for example, see Nicolet and Bossy [1985];…”

Section: Discussionmentioning

confidence: 99%

Recent solar radio astronomy at centimeter wavelengths: The temporal variability of the 10.7‐cm flux

Tapping¹

1987

J. Geophys. Res.

171

105

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Studies made by means of high-resolution radio telescopes indicate that solar centimetric emission contains contributions from many different sources and involves more than one radiation mechanism. Two emission components have been identified: bright, compact sources and weaker, diffuse emission which is distributed over the plage and surrounding areas of enhanced magnetic field. There is evidence for the occurrence of weaker but widely distributed radiation from elements of the active network. The good correlation between the 10.7-cm flux and shorter-wavelength indicators of solar activity, such as Ca II emission, suggests that gyromagnetic processes contribute little to the total centimetric flux. If the 10.7-cm flux is predominantly thermal (free-free) emission, its intensity will be a measure of the total amount of magnetic flux emerging through the photosphere and supporting density enhancements in the lower solar atmosphere.

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“…There has been much research into relating the 10.7-cm flux to the other activity measures, such as Ca II, UV and EUV spectral lines (for example, see Nicolet and Bossy [1985];…”

Section: Discussionmentioning

confidence: 99%

Recent solar radio astronomy at centimeter wavelengths: The temporal variability of the 10.7‐cm flux

Tapping¹

1987

J. Geophys. Res.

171

105

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“…Lean et al 1992) and to provide the input flux for planetary atmospheres on the other hand. Actually, the Lyman-α flux is not well correlated to the radio flux at 10.7 cm (Nicolet andBussy 1985, Nusinov andKatyushina 1994) and its calculation from the areas of typical features (active regions, cell and chromospheric network) is a difficult task (e.g. Fontenla et al 1999).…”

Section: 4/ Spatial and Temporal Variabilities In The Lyman-α α α αmentioning

confidence: 99%

The solar high-resolution imager - coronagraph LYOT mission

et al. 2003

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The LYOT (LYman Orbiting Telescope) solar mission is proposed to be implemented on a micro-satellite of CNES (France) under phase A study. It includes two main instruments, which image the solar disk and the low corona up to 2.5 R o in the H I Lyman-α line at 121.6 nm. The spatial resolution is about 1" for the disk and 2.5" for corona. It also carries an EIT-type telescope in the He II (30.4 nm) line. The coronagraph needs a super polished mirror at the entrance pupil to minimize the light scattering. Gratings and optical filters are used to select the Lyman-α wavelength. VUV cameras with 2048 x 2048 pixels record solar images up to every 10 seconds. The satellite operates at a high telemetry rate (more than 100 kb/s, after onboard data compression). The envisaged orbits are either geostationary or heliosynchronous. Possible launch dates could be end of 2006-beginning of 2007.

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“…La mesure systématique de l'émission résolue permet d'une part d'affiner les modèles d'émission globalè a 3 composantes spatiales ( [Lean et al, 1992]) et de fournir le flux d'entrée pour les atmosphères planétaires d'autre part. Rappelons que le flux H-Lyman α n'est pas bien corrélé au flux radioà 10.7 cm ( [Nicolet and Bossy, 1985] et [Nusinov and Katyushina, 1994]) et que sa reconstructionà partir de l'aire des régions types (régions actives, cellule et réseau chromosphériques) n'est pas chose facile. Il semble qu'il faille en fait 7 composantes pour bien reproduire le flux et ses variations (projet SUNRISE, voir par exemple le site http ://home.mho.net/jfontenla/SunRISE/ SunRISE2.html).…”

Section: Variabilités Spatiale Et Temporelle Dans La Raie H-lyman α ;unclassified

IFTSUV: an imaging Fourier transform spectrometer in UV for the next solar space missions

2006

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En premier lieu, je tiensà remercier la direction de l'Institut d'Astrophysique Spatiale pour son accueil et pour m'avoir permis de réaliser ces travaux de thèse dans les meilleures conditions possibles. Je voudrais exprimer ma profonde reconnaissanceà Philippe Lemaire et Jean-Claude Vial qui ont dirigé ces travaux. Les conseils prodigués par Philippe Lemaire au cours de ces trois années ont enrichi mes connaissances de façon inestimable. Je suis heureuse d'avoir commencé ma carrière avec un si talentueux instrumentaliste. Je remercie très sincèrement Jean-Claude Vial, son soutien constant et bienveillant et son aide précieuse m'ont permis de faire progresser le projet IFTSUV. Je remercie chaleureusement les membres du jury : Guy Guelachvili, Donald Hassler, Pierre Léna et Jean-Pierre Maillard, nos discussions ontété très enrichissantes. Je remercieégalement mes collègues de l'équipe physique solaire ; leur soutien amical aété très apprécié au cours de ces trois années.

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Solar radio fluxes as indices of solar activity

Cited by 17 publications

References 3 publications

Recent solar radio astronomy at centimeter wavelengths: The temporal variability of the 10.7‐cm flux

Recent solar radio astronomy at centimeter wavelengths: The temporal variability of the 10.7‐cm flux

The solar high-resolution imager - coronagraph LYOT mission

IFTSUV: an imaging Fourier transform spectrometer in UV for the next solar space missions

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