Emission line spectrum of an x-ray heated accretion disk in LMXB

1994 ◽  
Author(s):  
Yuan-Kuen Ko ◽  
Timothy R. Kallman
Keyword(s):  
Emission Line ◽  
Accretion Disk ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

scholarly journals The May 1985 Superoutburst of OY Carinae: II. Phase-Resolved IUE Spectroscopy and Exosat Observations

1987 ◽  
Vol 93 ◽  
pp. 371-376 ◽  
Author(s):  
B.J.M. Hassall ◽  
T. Naylor ◽  
G.T. Bath ◽  
P.A. Charles ◽  
G. Sonneborn ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Dwarf Nova ◽  
Uv Emission ◽  
Emission Line Spectrum ◽  
Coronal Region

AbstractWe present ultraviolet and X-ray observations of the eclipsing SU UMa dwarf nova OY Car early in the decline from a superoutburst. From the UV emission line spectrum and lack of X-ray eclipse, we deduce the presence of an extended coronal region.

scholarly journals Structure and Emission Line Spectrum of an X-ray Heated Accretion Disk in AGN

1994 ◽  
Vol 159 ◽  
pp. 484-484
Author(s):  
Yuan-Kuen Ko ◽  
Timothy R. Kallman
Keyword(s):  
Emission Line ◽  
Active Galactic Nuclei ◽  
Accretion Disk ◽  
Line Emission ◽  
Galactic Nuclei ◽  
X Ray ◽  
Disk Size ◽  
Emission Line Spectrum ◽  
Self Gravity ◽  
A Site

We investigate the structure of an X-ray heated accretion disk in active galactic nuclei. It is found that X-ray heating can prevent the disk to be disrupted by its self-gravity under sufficient X-ray heating. The disk size can be two orders of magnitute larger than that limited by self-gravity of the disk without X-ray heating. An accretion disk corona will be formed by X-ray heating and can be a site for line emission. We present such emission line spectra which range from optical to hard X-ray energies and compare with the observational data.

scholarly journals An X-ray emission-line spectrum of Nova V382 Velorum 1999

2005 ◽  
Vol 364 (3) ◽  
pp. 1015-1024 ◽  
Author(s):  
J.- U. Ness ◽  
S. Starrfield ◽  
C. Jordan ◽  
J. Krautter ◽  
J. H. M. M. Schmitt
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

scholarly journals X‐Ray–Irradiated Protoplanetary Disk Atmospheres. I. Predicted Emission‐Line Spectrum and Photoevaporation

2008 ◽  
Vol 688 (1) ◽  
pp. 398-407 ◽  
Author(s):  
Barbara Ercolano ◽  
Jeremy J. Drake ◽  
John C. Raymond ◽  
Cathie C. Clarke
Keyword(s):  
Emission Line ◽  
Protoplanetary Disk ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

[ITAL]Chandra[/ITAL] Detection of a Close X-Ray Companion and Rich Emission-Line Spectrum in the Wolf-Rayet Binary γ Velorum

2001 ◽  
Vol 558 (2) ◽  
pp. L113-L116 ◽  
Author(s):  
Stephen L. Skinner ◽  
Manuel Güdel ◽  
Werner Schmutz ◽  
Ian R. Stevens
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

Observation of the Solar Flare X-Ray Emission-Line Spectrum of Iron from 1.3 to 20 Å

1967 ◽  
Vol 149 ◽  
pp. L79 ◽  
Author(s):  
W. M. Neupert ◽  
W. Gates ◽  
M. Swartz ◽  
R. Young
Keyword(s):  
Solar Flare ◽  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

X-Ray Emission Line Spectrum of a Coronal Active Region

Nature ◽  
1967 ◽  
Vol 214 (5083) ◽  
pp. 41-42 ◽  
Author(s):  
K. EVANS ◽  
K. A. POUNDS ◽  
J. L. CULHANE
Keyword(s):  
Active Region ◽  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

scholarly journals The Ionization of Novae Ejecta

1990 ◽  
Vol 122 ◽  
pp. 215-227
Author(s):  
R.E. Williams
Keyword(s):  
Emission Line ◽  
White Dwarf ◽  
Line Spectrum ◽  
Ionized Gas ◽  
Grain Formation ◽  
Emission Line Spectrum ◽  
Pass Through

AbstractNovae ejecta pass through four distinct phases of evolution of the emission-line spectrum, caused by different ionization characteristics of the shell. These include a neutral (I), an auroral (II), a coronal (III), and a nebular (IV) phase. Photoionization from the contracting photosphere of the hot white dwarf is the source of the ionization, including the highly ionized coronal phase. Changing emission line ratios in certain novae that develop dust are caused by condensation of grains from the gas, and can be used to determine the composition of the dust. In V1370 Aql, substantial silicate grain formation appears to have taken place, probably within the ionized gas.

scholarly journals The unusual emission line spectrum of I Zw 1

2004 ◽  
Vol 2004 (IAUS222) ◽  
pp. 271-274
Author(s):  
Monique Joly ◽  
M.-P. Véron-Cetty ◽  
P. Véron
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
Emission Line Spectrum
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