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Fe II fluorescence in symbiotic stars

Eriksson, Mattias LU ; Veenhuizen, H.; Wahlgren, Glenn LU and Johansson, Sveneric LU (2004) IAU Colloquium 191 on the Environment and Evolution of Double and Multiple Stars In The Environment and Evolution of Double and Multiple Stars, Proceedings of IAU Colloquium 191 (Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias ) 21. p.132-136
Abstract
Fe 0 fluorescence by PAR has been investigated in eight symbiotic starshaving a wide range in temperature of the hot component and orbitalperiod. The data used are spectra obtained from the IUE archive. Allpumping lines investigated in this work are in the short wavelengthregion of IUE (1200-2000 Å), except for He 0 λ 1084.942 andO 0 λ 1032.041. The resulting Fe 0 fluorescence lines are mainlyin the long wavelength region (2000-3300 Å), but a few fall in thesame region as the pumping lines. The aim is to understand the optimalconditions for formation of Fe 0 fluorescence lines caused by PAR. Threeof the selected systems, RR Tel, AG Peg and V1016 Cyg, have 10-30 activeFe 0 channels. Two conditions connect those systems to each other: Thehot... (More)
Fe 0 fluorescence by PAR has been investigated in eight symbiotic starshaving a wide range in temperature of the hot component and orbitalperiod. The data used are spectra obtained from the IUE archive. Allpumping lines investigated in this work are in the short wavelengthregion of IUE (1200-2000 Å), except for He 0 λ 1084.942 andO 0 λ 1032.041. The resulting Fe 0 fluorescence lines are mainlyin the long wavelength region (2000-3300 Å), but a few fall in thesame region as the pumping lines. The aim is to understand the optimalconditions for formation of Fe 0 fluorescence lines caused by PAR. Threeof the selected systems, RR Tel, AG Peg and V1016 Cyg, have 10-30 activeFe 0 channels. Two conditions connect those systems to each other: Thehot component is a white dwarf of extreme temperature (80 .10<SUP>3</SUP>-150 . 10<SUP>3</SUP> K) and all three systems are socalled symbiotic novae and have had outbursts during the last 150 years.Three systems, AG Dra, RW Hya and R Aqr, have only 2-3 active Fe 0channels. In the two remaining systems, CI Cyg and T CrB, Fe 0fluorescence lines were totally absent. These two systems have twofeatures in common: The emission strength of highly ionized elements isless than in most symbiotic systems, and the hot component is suspectedto be an accreting main sequence star rather than a white dwarf. (Less)
Please use this url to cite or link to this publication:
author
organization
publishing date
type
Chapter in Book/Report/Conference proceeding
publication status
published
subject
keywords
binaries: symbiotic, Atomic Processes
in
The Environment and Evolution of Double and Multiple Stars, Proceedings of IAU Colloquium 191 (Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias )
editor
Allen, Christine and Scarfe, Colin
volume
21
pages
132 - 136
publisher
Instituto de Astronomía, UNAM
conference name
IAU Colloquium 191 on the Environment and Evolution of Double and Multiple Stars
external identifiers
  • WOS:000225291100029
  • Scopus:33646533740
ISBN
970-32-0607-7
language
English
LU publication?
yes
id
cc487916-a859-4054-ab8f-413c588e46b3 (old id 528481)
alternative location
http://www.astroscu.unam.mx/rmaa/RMxAC..21/PDF/RMxAC..21_eriksson.pdf
date added to LUP
2007-09-17 12:00:10
date last changed
2016-10-13 04:49:29
@misc{cc487916-a859-4054-ab8f-413c588e46b3,
  abstract     = {Fe 0 fluorescence by PAR has been investigated in eight symbiotic starshaving a wide range in temperature of the hot component and orbitalperiod. The data used are spectra obtained from the IUE archive. Allpumping lines investigated in this work are in the short wavelengthregion of IUE (1200-2000 Å), except for He 0 λ 1084.942 andO 0 λ 1032.041. The resulting Fe 0 fluorescence lines are mainlyin the long wavelength region (2000-3300 Å), but a few fall in thesame region as the pumping lines. The aim is to understand the optimalconditions for formation of Fe 0 fluorescence lines caused by PAR. Threeof the selected systems, RR Tel, AG Peg and V1016 Cyg, have 10-30 activeFe 0 channels. Two conditions connect those systems to each other: Thehot component is a white dwarf of extreme temperature (80 .10&lt;SUP&gt;3&lt;/SUP&gt;-150 . 10&lt;SUP&gt;3&lt;/SUP&gt; K) and all three systems are socalled symbiotic novae and have had outbursts during the last 150 years.Three systems, AG Dra, RW Hya and R Aqr, have only 2-3 active Fe 0channels. In the two remaining systems, CI Cyg and T CrB, Fe 0fluorescence lines were totally absent. These two systems have twofeatures in common: The emission strength of highly ionized elements isless than in most symbiotic systems, and the hot component is suspectedto be an accreting main sequence star rather than a white dwarf.},
  author       = {Eriksson, Mattias and Veenhuizen, H. and Wahlgren, Glenn and Johansson, Sveneric},
  editor       = {Allen, Christine and Scarfe, Colin},
  isbn         = {970-32-0607-7},
  keyword      = {binaries: symbiotic,Atomic Processes},
  language     = {eng},
  pages        = {132--136},
  publisher    = {ARRAY(0x685e968)},
  series       = {The Environment and Evolution of Double and Multiple Stars, Proceedings of IAU Colloquium 191 (Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias )},
  title        = {Fe II fluorescence in symbiotic stars},
  volume       = {21},
  year         = {2004},
}