Modeling the Fine Structure of a Sunspot Penumbra through the Inversion of Stokes Profiles
Not Available
Borrero, J. M. et al.
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2003
This section contains the publications database that collects IAC articles published in scientific journals. Please, click on the arrow to see full search filter and sort options: author, journal, year, etc..
It also provides access to IAC Preprints Repository here: https://research.iac.es/preprints/
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Mid-Infrared Images of the Star Forming Region GGD14Mid-IR images at 8.7 9.7 and 12.5 µm are presented of the star forming region GGD14 associated with the IRAS source 06084-0611. In an area of ˜30arcsec around the IRAS position we have found two mid-IR sources identified with the cometary compact HII region VLA1 and with the faint and unresolved radio continuum source VLA4. The mid-IR morphology ofPersi, Paolo et al.
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02003 -
Mid-infrared images of compact and ultracompact HII regions: W51 and W75N.A mid-infrared imaging survey at 8.7, 9.7 and 12.5 mu m of a selected number of compact and ultracompact (UC HII) regions has been undertaken with the 2.1m telescope of the OAN at San Pedro Martir, Mexico. We present a detailed plane of the observations, and we discuss the preliminary results of two massive star-forming regions; W51 and W75N.Persi, Paolo et al.
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Mid IR Obscuring Structures in Seyfert GalaxiesNot AvailableRodríguez Espinosa, José M. et al.
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Measuring the true supernova rate in galaxiesOne of the best tracers of massive stars is the rate of supernovae in galaxies. Studies of the supernova rate in galaxies are though severely affected by the line of sight extinction. Geometrical effects (e.g. edgewise presentation) may lead to the majority of supernovae that appear in a galaxy being undetectable in the visible. We propose to useKidger, Mark R. et al.
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Mag Waves in Sunspot Umbra: Slow Mode Leaking to the CoronaThe linear oscillations of a stratified atmosphere embedded by a uniform vertical magnetic field are studied here. We use a simple theoretical model formed by the superposition of two isothermal layers representing respectively i) the photosphere and the chromosphere and ii) the corona. The bottom layer behaves for some modes as a resonant cavityYelles Chaouche, Lotfi et al.
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02003