Radiocontinuum in nearby galaxies

The observed radio-continuum in galaxies is the addition of thermal and non-thermal emissions. Thermal emission, due to hot gas ionized by stars, has a flat spectrum and is best observed at high radio frequencies. The non-thermal emission, due to relativistic electrons spiralling in magnetic fields...

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Detalles Bibliográficos
Autor principal: Wielebinski, R.
Formato: Articulo Comunicacion
Lenguaje:Inglés
Publicado: 1981
Materias:
Astronomía
Galaxias
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/111744
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-111744
record_format dspace
spelling I19-R120-10915-1117442024-09-04T18:30:00Z http://sedici.unlp.edu.ar/handle/10915/111744 Radiocontinuum in nearby galaxies Wielebinski, R. 1981 2021-01-21T12:31:21Z en Astronomía Galaxias The observed radio-continuum in galaxies is the addition of thermal and non-thermal emissions. Thermal emission, due to hot gas ionized by stars, has a flat spectrum and is best observed at high radio frequencies. The non-thermal emission, due to relativistic electrons spiralling in magnetic fields of a galaxy, has a steep spectrum and dominates at lover radio frequencies. Relativistic electrons can originate in supernovae, pulsars, X-ray sources and CB-stars. The non-thermal emission process offers an additional possibility since the radio emission is linearly polarized. We can use the observations of polarized radiation to trace the magnetic fields in galaxies. Asociación Argentina de Astronomía Articulo Comunicacion http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) application/pdf
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Astronomía
Galaxias
spellingShingle Astronomía
Galaxias
Wielebinski, R.
Radiocontinuum in nearby galaxies
topic_facet Astronomía
Galaxias
description The observed radio-continuum in galaxies is the addition of thermal and non-thermal emissions. Thermal emission, due to hot gas ionized by stars, has a flat spectrum and is best observed at high radio frequencies. The non-thermal emission, due to relativistic electrons spiralling in magnetic fields of a galaxy, has a steep spectrum and dominates at lover radio frequencies. Relativistic electrons can originate in supernovae, pulsars, X-ray sources and CB-stars. The non-thermal emission process offers an additional possibility since the radio emission is linearly polarized. We can use the observations of polarized radiation to trace the magnetic fields in galaxies.
format Articulo
Comunicacion
author Wielebinski, R.
author_facet Wielebinski, R.
author_sort Wielebinski, R.
title Radiocontinuum in nearby galaxies
title_short Radiocontinuum in nearby galaxies
title_full Radiocontinuum in nearby galaxies
title_fullStr Radiocontinuum in nearby galaxies
title_full_unstemmed Radiocontinuum in nearby galaxies
title_sort radiocontinuum in nearby galaxies
publishDate 1981
url http://sedici.unlp.edu.ar/handle/10915/111744
work_keys_str_mv AT wielebinskir radiocontinuuminnearbygalaxies
_version_ 1809774283566612480

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