SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS

We describe the X-ray emission as observed by Suzaku from five symbiotic stars that we selected for deep Suzaku observations after their initial detection with ROSAT, ASCA, and Swift. We find that the X-ray spectra of all five sources can be adequately fit with absorbed optically thin thermal plasma...

Descripción completa

Guardado en:
Detalles Bibliográficos
Publicado: 2016
Materias:
binaries: symbiotic
X-rays: individual (CD-28 3719, EG And, Hen 3-461, Hen 3-1591, 4 Dra)
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v824_n1_p_Nunez
http://hdl.handle.net/20.500.12110/paper_0004637X_v824_n1_p_Nunez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v824_n1_p_Nunez
record_format dspace
spelling paper:paper_0004637X_v824_n1_p_Nunez2023-06-08T14:29:17Z SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS binaries: symbiotic X-rays: individual (CD-28 3719, EG And, Hen 3-461, Hen 3-1591, 4 Dra) We describe the X-ray emission as observed by Suzaku from five symbiotic stars that we selected for deep Suzaku observations after their initial detection with ROSAT, ASCA, and Swift. We find that the X-ray spectra of all five sources can be adequately fit with absorbed optically thin thermal plasma models, with either single- or multi-temperature plasmas. These models are compatible with the X-ray emission originating in the boundary layer between an accretion disk and a white dwarf. The high plasma temperatures of kT > 3 keV for all five targets were greater than expected for colliding winds. Based on these high temperatures as well as previous measurements of UV variability and UV luminosity and the large amplitude of X-ray flickering in 4 Dra, we conclude that all five sources are accretion-powered through predominantly optically thick boundary layers. Our X-ray data allow us to observe a small optically thin portion of the emission from these boundary layers. Given the time between previous observations and these observations, we find that the intrinsic X-ray flux and the intervening absorbing column can vary by factors of three or more on a timescale of years. However, the location of the absorber and the relationship between changes in accretion rate and absorption are still elusive. © 2016. The American Astronomical Society. All rights reserved.. 2016 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v824_n1_p_Nunez http://hdl.handle.net/20.500.12110/paper_0004637X_v824_n1_p_Nunez
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic binaries: symbiotic
X-rays: individual (CD-28 3719, EG And, Hen 3-461, Hen 3-1591, 4 Dra)
spellingShingle binaries: symbiotic
X-rays: individual (CD-28 3719, EG And, Hen 3-461, Hen 3-1591, 4 Dra)
SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS
topic_facet binaries: symbiotic
X-rays: individual (CD-28 3719, EG And, Hen 3-461, Hen 3-1591, 4 Dra)
description We describe the X-ray emission as observed by Suzaku from five symbiotic stars that we selected for deep Suzaku observations after their initial detection with ROSAT, ASCA, and Swift. We find that the X-ray spectra of all five sources can be adequately fit with absorbed optically thin thermal plasma models, with either single- or multi-temperature plasmas. These models are compatible with the X-ray emission originating in the boundary layer between an accretion disk and a white dwarf. The high plasma temperatures of kT > 3 keV for all five targets were greater than expected for colliding winds. Based on these high temperatures as well as previous measurements of UV variability and UV luminosity and the large amplitude of X-ray flickering in 4 Dra, we conclude that all five sources are accretion-powered through predominantly optically thick boundary layers. Our X-ray data allow us to observe a small optically thin portion of the emission from these boundary layers. Given the time between previous observations and these observations, we find that the intrinsic X-ray flux and the intervening absorbing column can vary by factors of three or more on a timescale of years. However, the location of the absorber and the relationship between changes in accretion rate and absorption are still elusive. © 2016. The American Astronomical Society. All rights reserved..
title SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS
title_short SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS
title_full SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS
title_fullStr SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS
title_full_unstemmed SYMBIOTIC STARS in X-RAYS. III. SUZAKU OBSERVATIONS
title_sort symbiotic stars in x-rays. iii. suzaku observations
publishDate 2016
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v824_n1_p_Nunez
http://hdl.handle.net/20.500.12110/paper_0004637X_v824_n1_p_Nunez
_version_ 1768543972705173504

Ejemplares similares