Articles liés à Doppler imaging: Magnetic field, Doppler effect, Spectral...

Doppler imaging: Magnetic field, Doppler effect, Spectral line, Maximum Entropy, Sun, Starspot, Zeeman- Doppler imaging - Couverture souple

 
9786130768874: Doppler imaging: Magnetic field, Doppler effect, Spectral line, Maximum Entropy, Sun, Starspot, Zeeman- Doppler imaging
Couverture souple
ISBN 10 : 6130768877 ISBN 13 : 9786130768874
Editeur : Alphascript Publishing, 2010

Synopsis

Please note that the content of this book primarily consists of articles available from Wikipedia or other free sources online. Inhomogeneous structures on stellar surfaces, i.e. temperature differences, chemical composition or magnetic fields, create characteristic distortions in the spectral lines due to the Doppler effect. These distortions will move across spectral line profiles due to the stellar rotation. The technique to reconstruct these structures on the stellar surface is called Doppler-imaging, often based on the Maximum Entropy image reconstruction to find the stellar image. This technique gives the smoothest and simplest image that is consistent with observations. To understand the magnetic field and activity on stars studies of the Sun is not sufficient, therefore studies of other stars are necessary. Periodic changes in brightness have long been observed in stars which indicate cooler or brighter starspots on the surface. These spots are larger than the ones on the Sun, covering up to 20% of the star. Spots with similar size as the ones on the Sun would hardly give rise to changes in intensity. In order to understand the magnetic field structure of a star it is not enough to know that spots exist, their location and extent are also important.

Les informations fournies dans la section « Synopsis » peuvent faire référence à une autre édition de ce titre.

Présentation de l'éditeur

Please note that the content of this book primarily consists of articles available from Wikipedia or other free sources online. Inhomogeneous structures on stellar surfaces, i.e. temperature differences, chemical composition or magnetic fields, create characteristic distortions in the spectral lines due to the Doppler effect. These distortions will move across spectral line profiles due to the stellar rotation. The technique to reconstruct these structures on the stellar surface is called Doppler-imaging, often based on the Maximum Entropy image reconstruction to find the stellar image. This technique gives the smoothest and simplest image that is consistent with observations. To understand the magnetic field and activity on stars studies of the Sun is not sufficient, therefore studies of other stars are necessary. Periodic changes in brightness have long been observed in stars which indicate cooler or brighter starspots on the surface. These spots are larger than the ones on the Sun, covering up to 20% of the star. Spots with similar size as the ones on the Sun would hardly give rise to changes in intensity. In order to understand the magnetic field structure of a star it is not enough to know that spots exist, their location and extent are also important.

Les informations fournies dans la section « A propos du livre » peuvent faire référence à une autre édition de ce titre.

Éditeur
Alphascript Publishing
Date d'édition
2010
Langue
anglais
ISBN 10 
6130768877
ISBN 13 
9786130768874
Reliure
Broché
Nombre de pages
92
Éditeur
Miller Frederic P., Vandome Agnes F., McBrewster John
Coordonnées du fabricant
non disponible
Personne responsable
non disponible